the signal with an effective resolution better than IFOV size. Only the
central part (40 pixels) of each line will be transmitted to Earth, to cope
with data volume limitations.

  3. 3.

Observations of auroras (‘MAJIS_JUP_AURORAL_SCAN’) will usually consist of a
set of four cubes over the northern polar region (north of $50^{\circ}$N),
acquired in proximity of each pericenter passage when sub-spacecraft longitude
is closer to 190∘W, to ensure better visibility of the northern polar oval.
Southern polar oval is more symmetric around the pole and will be better
observed with during the high inclination phase. Cubes during each perijove
will be taken with gaps of approximately 40 minutes, to monitor the rapid
variability of auroral structures.

Although the types of observations mentioned above will represent most of the
entries in MAJIS Jupiter dataset, they will be nonetheless complemented by
other types, to be performed more rarely during the mission. This latter group
includes: a global complete mosaic at full spectral coverage (to be acquired
just once during the mission, given the massive data volume output), limb
observations while in eclipse, stellar occultations and ‘tracking’
observations (repeated observations of the same area at the relatively short
period of several minutes).

Figure 19: (Top) Expected coverage of Jupiter’s disk by MAJIS on 2032-Sep-24,
near perijove #12. Different colours present the coverage of four cubes
acquired at time intervals of 1h10m. (Bottom) Expected coverage of Jupiter’s
auroras by MAJIS on 2032-Sep-25, a few hours after perijove #12. Different
colours present the coverage of four cubes acquired at time intervals of 46m.

Figure 20: Example fields-of-view of MAJIS for different observing modes. Each
panel presents an individual cube from the set of several that are acquired in
close temporal sequence: (top left) A cube from a MAJIS_JUP_DISK_SCAN set;
acquisition starts on 2032-Sep-24 at 19:29 UTC, corresponding to the red cube
of Fig. 19 (top). (top right) A cube from a MAJIS_JUP_AURORA_SCAN set;
acquisition starts on 2032-Sep-25 at 06:51 UTC, corresponding to the red cube
of Fig. 19 (bottom). (bottom left) A cube from a MAJIS_JUP_LIMB_SCAN set;
acquisition starts on 2032-Sep-25 at 15:24 UTC. (bottom right) Detail of the
same MAJIS_JUP_LIMB_SCAN cube.

###  4.3 SWI

####  4.3.1 SWI Description

The Sub-millimetre Wave Instrument (SWI, Hartogh et al., in prep.) is a
passively cooled radio telescope with a 29-cm primary mirror that will be
sensitive to radiation produced in Jupiter’s atmosphere from its upper
troposphere to its lower thermosphere. It will be an ideal instrument to
constrain the chemistry and dynamics of Jupiter’s stratosphere.

SWI can be tuned to observe in parallel two spectral windows located in two
spectral bands, 530-625 GHz (479-565 $\mu$m) and 1067-1275 GHz (235-281
$\mu$m), with one spatial pixel, and a suite of high resolution spectrometers
(up to 107 resolving power) and continuum channels. These two windows in the
sub-millimetre open the possibility to target key neutral and ion species
(CH4, H2O, HCN, CO, CS, CH3C2H, etc.) as well as their isotopologues relevant
for Jupiter chemistry (see Figure 21). The main limitation of the instrument
concerns spatial resolution with a 1 mrad beam at best (i.e. 1000 km from
about 15 RJ) which will not enable limb scanning. Despite more limited spatial
resolution compared to other remote sensing instruments aboard JUICE, SWI will
nonetheless get vertically-resolved information on temperature and composition
from observations of the pressure broadened lineshapes. The high sensitivity
ensured by the low receiver temperatures coupled with the highest resolution
spectrometers, i.e. the Chirp Transform Spectrometers (CTS), which will have 1
GHz bandwidth and 10000 channels of 100 kHz, will result in very high S/N
observations of the lineshapes of H2O and CH4 ($\sim 50$ at 600 GHz, and $\sim
20$ at 1200 GHz with 200 kHz resolution) in 5 minutes of integration.
Observing in the two bands in parallel with the high spectral resolution of
the CTS and the high sensitivity of the receivers will enable the simultaneous
and independent retrieval of the vertical profiles of temperature (with CH4
lines around 1256 GHz), abundance of the species observed in the 600 GHz band,
and wind speeds (from the combination of the two lineshapes), from the upper
troposphere to the upper stratosphere. SWI will thus improve over previous
sub-millimetre observatories like IRAM-30m, ISO, Odin and Herschel for the
characterization of the chemistry and general circulation of Jupiter’s
stratosphere (Moreno et al., 2003; Lellouch et al., 2002; Cavalié et al.,
2008, 2012, 2013; Benmahi et al., 2020).

Figure 21: Jupiter limb spectra in the 600 GHz (top) and 1200 GHz (bottom)
bands probed by SWI, with the main observable molecular lines. Spectra are
computed at the limb for a tangential height of 200 km above the 1-bar level
and are convolved by the instrument beam and to a spectral resolution of 1
MHz.

Unlike other instruments, SWI will take advantage of its own pointing
mechanism that will enable scanning up to $\pm$72∘ along-track and $\pm$4.3∘
cross-track away from the attitude of the JUICE spacecraft. This pointing
capability has $\sim$30′′ and $\sim$9′′ steps along-track and cross-track,
respectively, with 30′′ accuracy. This mechanism will serve several
operational goals. SWI will be able to (i) map the whole Jovian disk from any
distance $>$15 RJ, (ii) compensate for spacecraft motions when performing
scans for other remote sensing instruments to ensure a stable pointing, and
(iii) reach any Galilean moon from the equatorial orbit on a daily basis to
monitor their emissions and constrain the source of their atmospheres (Tosi et
al., in prep.).

Figure 22: Example of using the Doppler shift of sub-millimetre spectral lines
to determine Jupiter’s stratospheric winds (using ALMA data, Cavalié et al.,
2021). The HCN rest frequency is 354.505 GHz (red line), but the observed line
is shifted both by the planetary rotation (blue line) and the strong $\sim$400
m/s westward winds in the south-polar stratosphere (purple line) surrounding
regions heated by the jovian auroras. SWI measurements will use the Doppler
shift of several lines to build up a 3D picture of stratospheric winds.

The main Jupiter science goals of SWI concern its stratospheric circulation
and chemistry. Constraining the general circulation of Jupiter’s stratosphere
(e.g. Medvedev et al. 2013; Guerlet et al. 2020b) requires measuring
temperature and winds simultaneously and continuously at all latitudes,
longitudes and altitudes. This can only be rarely achieved from the ground
(Benmahi et al., 2021), but can be measured precisely via SWI using the
Doppler shift of spectral lines away from their rest frequencies (Fig. 22).
The duration of the Jupiter tour will provide SWI with the possibility to
build a full 4-dimensional view of Jupiter’s stratospheric composition and
dynamics, from its QQO-dominated equatorial region to the auroral latitudes,
while ALMA can only provide irregularly-spaced snapshots (e.g., Cavalié et al.
2021, 2022). A focus will be put on equatorial latitudes to constrain what
maintains the QQO (Leovy et al., 1991b; Orton et al., 1991b; Li and Read,
2000; Cosentino et al., 2017b; Giles et al., 2020a; Benmahi et al., 2021), and
on the auroral regions to understand what controls its chemistry and dynamics
(Sinclair et al., 2017b, a, 2018a, 2019; Cavalié et al., 2021, 2022).
Composition maps will help to constrain the stratospheric photochemistry of
Jupiter (Moses et al., 2005b; Hue et al., 2018b) and spectral scans will be
performed in various regions to serendipitously search for new species and
isotopologues. SWI will also detect and quantify sources of exogenic species
other than SL9, like the Galilean moons, rings and torii (Hartogh et al.,
2011; Cavalié et al., 2019), interplanetary dust (Moses and Poppe, 2017), and
comet/asteroid impacts. The latter seem to occur regularly in giant planet
atmospheres (Bézard et al., 2002; Cavalié et al., 2010, 2014; Lellouch et al.,
2005; Moreno et al., 2017; Hueso et al., 2010, 2013, 2018a; Orton et al.,
2011).

####  4.3.2 SWI Operations

These goals will be achieved from the following observation products: regular
2D wind maps from 10 $\mu$bar to 400 mbar with 3∘ latitudinal resolution;
global thermal structure also from 10 $\mu$bar to 400 mbar with 3∘ latitudinal
resolution and 20∘ longitudinal resolution; vertical distribution of a variety
of species, tracing atmospheric transport from SL9-derived species
distributions; isotopic composition; and search for new species. The
observation strategy adopted by SWI mostly depends on the distance to Jupiter
(see Figure 23). When JUICE is closer than 25 RJ, limb stares and limb rasters
will be prioritised to map temperatures (from CH4), abundances and wind speeds
with the required latitudinal resolution. Observations from these distances
will be complemented by zonal scans to look for thermal waves, 2D maps and
meridional scans to measure the latitudinal distributions of high priority
species (H2O, HCN, CO). These observations will be clustered around perijoves
in the early phases of the tour and during Phase 5. At intermediate distances
(between 25 RJ and 35 RJ), SWI will measure the latitudinal distributions of
lower priority species (CS, CH3C2H, isotopologues) with 5∘ latitudinal
resolution and look for new species using limb stares, limb rasters and 2D
maps. At distances beyond 35 RJ, SWI will monitor line emissions at lower
spatial resolutions from the equatorial region to the auroras, and perform
calibration observations, using 2D maps, 5-point crosses and nadir stares.

Figure 23: Five main observations modes used by SWI for Jupiter atmospheric
investigations. Their use mainly depends on the distance to the planet, as
depicted by the color code: yellow, green and blue for modes to be used when
JUICE is at distance $d$ $<$25$R_{J}$, 25$R_{J}<d<$35$R_{J}$, and
$d>$35$R_{J}$, respectively. The along-track and cross-track mechanisms of the
instrument enable pointing independently from the spacecraft to build various
patterns (stares, crosses, scans, and maps). The 2D map mode can be set such
that meridional or zonal scans are performed. The limb stares and rasters use
a limb-finding procedure at each latitude in which the continuum is recorded
over several tens of positions from nadir to sky to reconstruct a posteriori
the pointing of the long integration for accurate rotation removal in wind
measurements.

###  4.4 JANUS

####  4.4.1 JANUS Description

The JUICE optical camera, JANUS (Jovis, Amorum ac Natorum Undique Scrutator,
Palumbo et al., in prep.) is a multi-filter camera system with a CMOS detector
and thirteen filters spanning the near-UV (340 nm) to the near-IR (1080 nm).
JANUS addresses a number of the scientific investigations in Section 2 and
Table 1. JANUS will investigate the dynamics of the weather layer by providing
high-resolution observations of the atmosphere from the cloud layer to the
upper hazes in multiple wavelengths. Repeated observations will be used to
characterise the atmospheric dynamics and circulation [JA.1] including the
role of atmospheric waves at multiple scales [JA.3]. Observations in multiple
wavelengths will be used to investigate the vertical cloud structure [JC.1]
and the coupling of different clouds with the dynamics [JC.2]. Dayside and
night-side observations of convective regions will be used to study the role
of moist convection in meteorology [JB.4]. Auroral processes imaged at night
[JA.4] will also constitute an important dataset to understand the auroral
structure and the impact of auroral processes in forming high altitude aerosol
layers in the polar regions. JANUS observations will consist in the
combination of mappings of the planet taking advantage of the planet rotation,
and high-resolution observations of different targets separated by different
time-scales.

The field-of-view of the detector covers a rectangular area over the sky of
1.29∘$\times$ 1.72∘, with the largest size of the detector oriented parallel
to Jupiter’s equator with the nominal spacecraft attitude during Jupiter
observations. The detector has 1504 $\times$ 1200 pixels with a pixel IFoV of
15 $\mu$rad that allows images with a 15 km/pix from a target distance of
$10^{6}$ km. Images with a Signal to Noise Ratio (SNR) larger than 100 are
achievable in most operational conditions foreseen during the Jupiter
investigation, with dayside integration times of 1 s or less even in the
filters sensitive to strong methane absorption bands. JANUS observations of
the nightside of the planet will be obtained with larger exposure times below
an upper operational limit of 112 s.

Table 3 provides details about the filters. Each of these filters have
spectral transmission curves that are almost rectangular-shaped. The
instrument spectral response is also determined by the optical elements and
detector spectral response, with a steep decrease at low and high range edges.
JANUS filters can be compared with filters from previous missions in Table 4.

Table 3: JANUS filters Position | Filter id. | Central wavelength / | Note
---|---|---|---
|  | Bandpass [nm] |
F1 | PAN | 650/500 | Panchromatic (clear) – monochromatic imaging
F2 | BLUE | 450/60 | Blue – aerosol colours
F3 | GREEN | 540/60 | Green, background for Na – aerosol colours
F4 | RED | 646/60 | Red, background for H$\alpha$ – aerosol colours
F5 | CMT medium | 750/20 | Continuum for medium Jovian Methane band
F6 | Na | 590/10 | Sodium D-lines in exospheres
F7 | MT strong | 889/20 | Strong Jovian Methane band
F8 | CMT strong | 940/20 | Continuum for strong Jovian Methane band
F9 | MT medium | 727/10 | Medium Jovian Methane band
F10 | Violet | 380/80 | UV slope
F11 | NIR 1 | 910/80 | Cloud structure
F12 | NIR 2 | 1015/130 | Cloud structure
F13 | H$\alpha$ | 656/10 | H$\alpha$-line for aurorae and lightning
Table 4: Comparison of JANUS filters with those on previous missions

Wavelength centres [nm] | Galileo SSI (a) | Voyager | Cassini ISS | New Horizon | Juno JunoCam (f) | JUICE JANUS
---|---|---|---|---|---|---
|  | NAC (b) | WAC (b) | NAC (c) | WAC (c) | RALPH (d) | LORRI (e) |  |
Clear | 611 (440) | 497 (360) | 470 (290) | 611 | 635 | 687 (575) | 600 (500) | - | 650 (500)
UV | - | - | - | 258 | - | - | - | - | n.a.
UV | - | - | - | 298 | - | - | - | - | n.a.
UV | - | 346 | - | 338 | - | - | - | - | n.a.
Violet | 404 | 416 | 426 | - | 420 | - | - | - | 380 (80)
Blue (2) | - | - | - | 440 | - | - | - | - | -
Blue | - | 479 | 476 | 451 | 460 | 475 | - | Bayer Pattern blue | 450 (60)
Methane | - | - | 541 | - | - | - | - | - | -
Green | 559 | 566 | 560 | 568 | 567 | - | - | Bayer Pattern green | 540 (60)
Sodium-D | - | - | 589 | - | - | - | - | - | 590 (10)
Orange | - | 591 | 605 | - | - | - | - | - | -
Methane | - | - | 618 | 619 | - | - | - | - | -
Continuum 2-lobed | - | - | - | 603, 635 | - | - | - | - | -
Red | 671 | - | - | 650 | 648 | 620 | - | Bayer Pattern red | 646 (60)
H-alpha | - | - | - | 656 | 656 | - | - | - | 656 (10)
Methane | 734 | - | - | 727 | 728 | - | - | - | 727 (10)
Continuum / NIR | 756 | - | - | 750 | 752 | - | - | - | 750 (20)
NIR (broad) | - | - | - | 752 | 742 | - | - | - | -
NIR (broad) | - | - | - | 862 | 853 | 880 | - | - | -
Methane | 887 | - | - | 889 | 890 | 885 | - | - | 889 (20)
Near Infrared | - | - | - | 930 | 918 | - | - | - | 910 (80)
Continuum | - | - | - | 938 | 939 | - | - | - | 940 (20)
Near Infrared | 986 - | - | 1002 | 1001 | - | - | - | 1015 (130) |
NIR (broad) | - | - | - | - | 1028 | - | - | - | -

Notes: Bandwith is given in parentheses for the clear filter (ISS polarization
filters and two-filter bandpasses not considered). (a) (Belton et al., 1992),
(b) (Smith et al., 1977), (c) (Porco et al., 2004), (d) (Reuter et al., 2008),
(e) (Cheng et al., 2008b), (f) (Hansen et al., 2017b).

####  4.4.2 JANUS Operations

Figure 24 shows sketches of some of the operational models of JANUS. JANUS
will provide the highest spatial resolution observations over the planet with
the capability to map the planet as it rotates and image specific features at
very high spatial resolution ($\sim$10 km/pix). To map the planet JANUS will
perform vertical scans of Jupiter (Figure 24a) in which different frames will
cover different latitudinal ranges and different longitudes will be sampled as
the planet rotates over its 10-hour rotation period. These maps will be
obtained at low and intermediate phase angles ($<$90∘) over the illuminated
side of Jupiter and will attain spatial resolutions of about 15–30 km/pix. The
different opportunities in the orbital tour to obtain full maps of the planet
separated by one Jovian rotation (10hr) will result in several determinations
of the mean zonal winds and their variability over the course of the orbital
tour. These wind fields will have a noise level of less than 1 m/s and will be
used to answer fundamental question on the energy inputs of the jets and cloud
systems and how is the interaction between the eddies and zonal winds (e.g.,
Salyk et al. 2006), and on the meridional transport on belts and zones (Duer
et al., 2021) at different moments during the mission. Higher resolution
observations of particular features will unveil the internal wind field of
vortices, cyclonic regions, and convective storms (Figure 6).

Close to the planet, JANUS will observe specific regions at spatial
resolutions down to 10 km/pix including the limbs (Figure 24b). Repeated
observations of the same regions obtained after a given amount of time will be
used to infer dynamics by examining cloud motions on time-scales of 0.5, 2.0
and 10.0 hr tracking specific features of interest like the Great Red Spot and
other regions. Specific observations of the polar regions from sub-spacecraft
latitudes of about $\pm$30∘will be obtained to investigate long-term changes
of the polar atmosphere since the Juno observations (Adriani et al., 2018b).

In addition, by using a combination of filters sensitive to color and cloud
altitude via different atmospheric absorption bands, JANUS image will
investigate the particle size and optical properties of the clouds, hazes and
aerosols, investigating the complex and poorly determined relations between
colour distribution and atmospheric dynamics in Jupiter. By observing the
limbs at high spatial resolutions over a variety of phase angles over
different latitudes JANUS will further investigate the elevated hazes at
levels close to the stratopause and higher.

Nightside observations will map the spatial distribution of lightning (Figure
24c) to complement and extend the results from previous missions (Little et
al., 1999; Dyudina et al., 2004; Baines et al., 2007; Becker et al., 2020b).
Observations of lightning at high spatial resolution will be used to
investigate lightning spot sizes to constrain the depth of the lightning
source. Dayside observations of the same areas observed on the nightside with
time differences of a few hours will also give information about the
intensity, depth and vertical transport associated to moist convective storms.
Nightside observations of the polar region (Figure 24c) will also investigate
the emissions of the aurora and its vertical structure.

Figure 24: Sketch of different JANUS frames over the planet covering different
topics. (a) Dayside observations obtaining vertical scans of the planet as it
rotates (green frames), or images of specific features obtained at high
spatial resolution with small time differences (purple frames) will be used
for dynamics. (b) Limb observations at different wavelengths will complement
observations at a variety of phase angles to determine the vertical cloud
structure and directly observe haze systems over the limb. (c) Night side
observations at high phase angles will map lightning (dark yellow) at moderate
resolution but high-resolution images of latitudes with convective activity
will also be obtained at high-resolution (red). Auroras observations will also
be possible at different spatial and temporal resolutions (blue). These
observations will be spread over different phases of the mission.

###  4.5 3GM

####  4.5.1 3GM Description

The 3GM (Gravity & Geophysics of Jupiter and Galilean Moons, Iess et al., in
prep.) is the experiment onboard the JUICE mission responsible for the radio
science. This instrument consists of two separate and independently operated
units incorporated in the Telemetry Tracking and Command subsystem of the
spacecraft: a Ka band Transponder (KaT) and an Ultra Stable Oscillator (USO).
The KaT will enable two-way range and Doppler measurements with very high
accuracy at Ka band (34.5-32.2 GHz), measuring the gravity fields of Europa,
Ganymede and Callisto (Cappuccio et al., 2022). Juno measured the gravity
field of Jupiter to high accuracy (Iess et al., 2018), enabling the
determination of the zonal wind depth (Kaspi et al., 2018). This was made
possible by Juno’s close proximity to Jupiter’s cloud tops (a few thousand
kilometres altitude). However, JUICE will orbit Jupiter with a proximity of
hundreds of thousands of kilometres, rendering Juno-like gravity measurements
of Jupiter’s deep interior impracticable. However, the USO will enable radio
occultations of Jupiter’s atmosphere by providing a highly stable frequency
reference for the transmitted signal, establishing the possibility of one-way
downlink radio occultation experiments. Together with X and Ka band
transponders, providing various communication links, the USO will be used to
perform radio science to retrieve the structure and composition of the neutral
atmosphere and ionosphere of both Jupiter and its moons.

These occultations and bistatic radar radio science experiments permit the
retrieval of vertical profiles of density, pressure, temperature and
composition in the Jovian neutral atmosphere and electron/ion densities in the
Jovian Ionosphere. The wide temporal and spatial variability of the
experiments will also enable the study of vertically-propagating waves
influencing the heating in the thermosphere, and monitor this variability with
time and latitude.

The main principle of radio occultation measurements is the transmission of an
electromagnetic signal in the radio spectrum (X and Ka band) between two
separated stations (the JUICE spacecraft and an Earth-based ground-station),
thereby passing through the atmosphere or ionosphere of a solar system object
(Jupiter or its moons). Electromagnetic signals crossing an optical medium
experience refraction, which can have two distinct effects on the signal. The
first is the increase in the phase speed of the signal as the wave propagates
in a neutral medium and the decrease in the phase speed of the signal while
propagating in an ionised medium. The second is the bending of the signal
towards regions of higher index of refraction, instead of traveling in a
straight line from transmission to reception. These effects on the signal
result in frequency shifts (Doppler shifts) with respect to a signal that
would be traveling in vacuum. This refraction is exploited and studied in
radio occultation experiments in order to retrieve the atmospheric properties
of planetary atmospheres in the form of profiles varying with depth and
latitude (e.g., Lindal et al. 1981, Schinder et al. 2015).

The orbit of JUICE will enable the widespread distribution of these vertical
profiles, guaranteeing good spatial coverage. The vertical temperature
profiles will be improved by the instrumental accuracy of the USO that will
allow a resolution of about 0.1 K over 1 km. The vertical resolution of
occultations is also characterised by the Fresnel scale, some 6 km in the
stratosphere, and a few hundred meters in the troposphere (due to refractive
defocusing), from the distance of Ganymede. In addition, the attenuation of
the signal can be used to deduce the absorptivity of ammonia, since radio
occultations (at X band) are expected to be able to probe down to
approximately the cloud level at the $\sim$700 mbar level, whereupon NH3
absorption fully attenuates the signal.

####  4.5.2 3GM Operations

All predicted JUICE radio occultation opportunities of Jupiter are portrayed
for the period of July 2032 to January 2036, separated into the different
phases of the mission (Figure 25). The latest scenario of an April 2023 launch
campaign (Crema 5.0b23) allows for around 80 radio occultations of the gas
giant. The orbit of JUICE allows for not only a large number of radio
occultations over the timeframe of the mission, but also for a broad
latitudinal coverage. This will enable a better three-dimensional mapping of
the upper atmosphere of Jupiter than has been previously possible. Figure 25
shows the wide distribution of the radio occultation possibilities over Jovian
latitude (upper) and longitude (lower). Jupiter’s northern hemisphere has
significantly more coverage due to the timing of the JUICE mission, providing
the chance for occultations at approximately the same latitude twice.
Equatorial latitudes will only be observable with occultations during Phase 4
(the inclined phase). Since the southern hemisphere has fewer opportunities,
and all during Phase 3 (the Europa flybys), the portrayed radio occultations
are important to include in the science activity plan. Note that future
changes in the tour of JUICE can affect the frequency and possibilities of the
radio occultation experiments, especially in the southern hemisphere.

Figure 25: JUICE radio occultation opportunities of Jupiter based on Crema
5.0b23, for both latitudinal coverage (top) and longitudinal coverage (bottom)
for Phases 3 through 6 of the mission. Note the large numbers of occultations
while JUICE is in orbit around Ganymede during Phase 6.

The USO on board of JUICE provides a highly stable frequency reference for the
transmitted signal in X and Ka bands, leading to the possibility for one-way
radio occultation analysis. In one-way mode, the pointing of the spacecraft
will be adjusted continuously to the direction that allows the signal
transmitted by the spacecraft to be bent in a way that it will be traveling
toward the receiving station after traversing Jupiter’s atmosphere. The
analysis of radio occultations of oblate planetary objects is performed in a
different way than for spherically symmetrical ones, due to the fact that the
signal in the oblate case refracts three-dimensionally. The ray-tracing method
used for the analysis of Jupiter follows Schinder et al. (2015). This method
uses a numerical integration of the equations (Eikonal Equations) describing
subsequent optical rays across a barotropic layered atmosphere.

A few radio occultation experiments of Jupiter have been performed in the
past, and can provide benchmarks and constrain more finely the composition of
the atmosphere. A series of radio occultations experiments of Jupiter were
performed by the Voyager 1 and 2 missions (Lindal et al., 1981; Gupta et al.,
2022), with a similar configuration to the JUICE mission. Both Voyager
spacecrafts carried a USO on board, which was used to provide a very stable
frequency reference for the pure tones in the S and X frequency bands, so that
the analysis could be performed in one-way mode.

The analysis of $\sim 20$ upcoming radio occultations by the Juno spacecraft
during its extended mission (2023-2025), covering both northern and southern
hemispheres, will provide the most recent data for comparison to the JUICE
radio science. Juno occultations will be performed in two-way mode since no
USO is present on board Juno. In a two-way mode, the highly stable frequency
reference is not on the spacecraft but at a transmitting station on the Earth.

###  4.6 RPWI

####  4.6.1 RPWI Description

The JUICE Radio & Plasma Wave Investigation (RPWI) instrument package and
science objectives are described in detail in Wahlund et al. (in prep.). Here
we briefly focus on the parts relevant for the Jupiter science goals. The RPWI
instrument package will measure the electric- and magnetic-field vectors, as
well as thermal plasma properties in a wide frequency range and with high
temporal/spatial resolution. The electric field is measured from DC up to 1.4
MHz by a set of four Langmuir probes. A search coil magnetometer will measure
the magnetic field in the frequency range 0.1-20 kHz, complementing the higher
frequency wave components of the J-MAG measurements. Onboard analysis of these
measurements, combined with the RPWI electric components, will be used to
obtain the polarization and propagation properties of electromagnetic waves in
this frequency range.

Broadband measurements of all these wave field components will be especially
useful for analysis of electromagnetic signals emitted from electric
discharges in the Jovian atmosphere and waves in different propagation modes
linked to Jovian aurora. The near DC electric field measurements, together
with the J-MAG magnetic field measurements, will enable us to continuously
give values of the $\bm{E}\times\bm{B}$ convection (i.e., wherever JUICE is
traversing in the Jovian system). These convection electric fields are mapped,
along magnetic field flux tubes, down to Jupiter’s atmosphere and ionosphere,
there giving rise to electrodynamic momentum and energy exchange primarily
within the Jovian thermosphere and ionosphere. Along these flux tubes energy
and momentum is also transported by Alfvén wave activity, readily monitored by
RPWI determining their Poynting flux and dispersive properties. This is
especially important on magnetic footprints corresponding to the Jovian
auroral regions and the flux tubes connecting to the larger icy moons
(Callisto, Ganymede, and Europa). Jovian radio waves are monitored by a
special antenna system operating from 80 kHz to 45 MHz. In addition, the RPWI
sensors monitor thermal plasma and $\mu$m-sized dust properties wherever they
operate.

More specifically, the RPWI will contribute to Jupiter science goals in the
following ways:

  * •

Map the thermal plasma and the electrodynamic (convection) interaction
processes along Jovian magnetic footprint fluxtubes corresponding to the icy
moons and the Jovian auroral regions.

  * •

Characterise Alfvén waves, whistler mode waves, plasma waves in the Jovian
magnetosphere of importance for the energy and momentum flux down to the
Jovian ionosphere/thermosphere.

  * •

Characterise radio and whistler wave emissions from lightning at Jupiter.

  * •

Determination of the general dynamic state of the Jovian magnetosphere through
monitoring of the Jovian radio emission activity.

####  4.6.2 RPWI Operations

The RPWI sensors will nominally be continuously operating together with J-MAG.
The convection electric field (and $\bm{E}\times\bm{B}$), thermal plasma
properties, and Jovian plasma and radio wave activity will therefore always be
available, with limited impact on the remote sensing plan during the perijove
windows in Section 3. Certain periods will require ‘burst-mode data‘ to enable
detailed studies near the large icy moons or magnetosphere boundaries, e.g.,
characterizing the icy moons ionospheres or icy thickness, the icy moons
interaction with the Jovian magnetosphere, the energy and momentum processes
related to the magnetospheric footprints to Jupiter, etc. Multidimensional
electromagnetic signals from electrical discharges in the Jovian atmosphere
will be also captured during the dedicated burst mode periods. The RPWI
operations will implement a so-called selective downlink where the RPWI
instrument almost always does burst mode measurements, while the telemetry
allocation determines how much data RPWI can download at a specific time
during a period of a few weeks.

###  4.7 PRIDE

The Planetary Radio Interferometry and Doppler Experiment (PRIDE-JUICE,
Gurvits et al., in prep.) experiment will conduct radio occultation
observations, alongside 3GM, using radio telescopes from the European VLBI
network (EVN), and other radio telescopes around the world, as receivers in a
one-way mode using the X- and, optionally, Ka- bands. The experimental setup
is shown in Gurvits et al. (in prep.), whereby the PRIDE telescopes would
perform shadow tracking of the spacecraft during the occultation (e.g.,
Bocanegra-Bahamón et al. 2019). The radio signal would be recorded as it gets
refracted by Jupiter’s ionosphere and atmosphere in a wideband open-loop
configuration, which allows capturing its high dynamic range. PRIDE has access
through the EVN (and other networks) to tens of radio telescopes in Europe,
Asia, the Americas, South Africa and Australia, including large antennas such
as the 65-m Tianma (China), 64-m Sardinia (Italy) and 100-m Effelsberg
(Germany). The use of many antennas, and of large antennas in particular in
radio occultation measurements, especially for those geometries with limited
SNR (Bocanegra-Bahamón et al., 2018)), would improve the quality of the
atmospheric data retrieved and allow sounding deeper in the atmosphere than
with antennas of smaller collecting area.

These observations probe the upper troposphere down to the top-most condensate
clouds, with the X-band probing deepest (to approximately 700 mbar, Gurvits et
al., in prep.), because the effects of refractive defocussing are larger for
the Ka band. Both the X and Ka bands are needed to disentangle the
contributions of NH3 and PH3 absorption to the signal, but these are both
independent from the derivation of atmospheric temperature. The absorptivity
is derived from the change in amplitude of the signal, whereas the temperature
is derived from the refraction caused by the atmosphere, which is measured by
the excess Doppler (change in instantaneous frequency) of the observed signal.
Retrievals of NH3 and PH3 abundances from absorptivity, alongside measurements
from MAJIS and UVS, could lead to an improved characterisation of NH3
condensation physics and PH3 photochemical destruction processes in Jupiter’s
atmosphere.

##  5 Synergistic Science at Jupiter

The previous sections described the JUICE scientific objectives (Section 2),
the requirements on the Jupiter tour and its segmentation (Section 3), and the
capabilities of the payload for Jupiter science (Section 4). In this Section
we provide a subset of examples of how the different instruments might work
together synergistically to explore equatorial dynamics, moist convection and
lightning, stratospheric chemistry, auroral activity, and vertical wave
structures, e.g. by taking advantage from the complementary vertical coverage
of the various remote sensing instruments as shown in Fig. 26.

Figure 26: Synergistic observations are possible due to the overlapping
vertical sensitivity of each instrument in nadir sounding, compared to
Jupiter’s thermal structure from Voyager radio occultations (Gupta et al.,
2022), the Galileo Probe Atmospheric Structure Instrument (Seiff et al.,
1998), and an average of Cassini/CIRS temperature retrievals (Fletcher et al.,
2016). Key atmospheric regions, species, and aerosols are labelled where they
can be studied via spectroscopy. At higher altitudes, in-situ instruments
(J-MAG, RPWI, PEP) will contribute to characterise the energy and dynamics of
the thermosphere (and ionosphere).

###  5.1 Jupiter’s Equatorial Circulation and Meteorology

Jupiter’s Equatorial Zone (EZ) and neighbouring belts display a plethora of
dynamic activity: from evidence of moist convection and lightning in the
belts, to waves, variable winds, large vortices, and a Hadley-like circulation
pattern generating extreme contrasts in volatiles (e.g., NH3 de Pater et al.,
2016; Li et al., 2017), temperatures and disequilibrium species (e.g.,
Fletcher et al., 2009) between the EZ, NEB and SEB. The sole in situ
measurement of a giant planet comes from Galileo Probe observations in a
region between the NEB and EZ (Atkinson et al., 1998; Wong et al., 2004), and
it remains unclear how representative these measurements were of the planetary
bulk. Tropospheric dynamics provide the spectrum of waves responsible for
Jupiter’s equatorial stratospheric oscillation (Leovy et al., 1991a), which
subsequently influences the temperatures, winds and composition of the
stratosphere. All of these processes vary over timescales from hours to
months, but systematic multi-wavelength studies have proven challenging.

JUICE observations are designed to address the need for atmospheric
monitoring, both from the perijove windows to the monitoring opportunities
throughout Phases 2, 3 and 5. MAJIS spectral maps of reflected sunlight and
thermal emission to map aerosols and gaseous composition will be interspersed
with JANUS dayside cloud tracking for tropospheric winds and dynamics, UVS
scans for aerosols and stratospheric composition, SWI zonal scans to determine
the stratospheric temperature structure, and SWI limb observations to derive
the vertical winds associated with the QQO. UVS, MAJIS and SWI (via the 572
GHz line) all have sensitivity to Jovian NH3, enabling reconstruction of the
gaseous distribution above the condensation clouds to study its temporal
variability. Radio occultations during Phase 4 will provide the vertical
$T(p)$ and NH3 absorption for comparison with remote sensing measurements, and
RPWI will be able to search for evidence of lightning activity (see below).

###  5.2 Moist Convection and Lightning

As described in Section 2.1.3, mapping of lightning activity provides a
powerful probe of Jupiter’s meteorology within the water-cloud regions. UVS
may detect transient luminous events (Giles et al., 2020b) that could be
associated with lightning; JANUS will use nightside imaging to search for
optical flashes (and dayside imaging to find their storm counterparts) using a
similar approach to Galileo (Gierasch et al., 2000) and Juno (Becker et al.,
2020a). MAJIS observations of evolving storm plumes could constrain their
changing optical depth from bright fresh plumes to darker ovals, following
similar techniques for Cassini at Saturn (Sromovsky et al., 2018). Lightning
whistler measurements will also be performed by the RPWI search coil
magnetometer and the Langmuir probes used as electric antennas. Based on the
received signals in a range from 10 Hz to 20 kHz the LF (low frequency)
receiver will produce snapshots a few seconds long, producing spectra of high
temporal resolution from which the whistler dispersion can be measured.
Measurement of sferics or Jovian dispersed pulses from lightning by RPWI might
also be possible using the three RWI antennas and its corresponding HF (high
frequency) receiver in the frequency range above 80 kHz, where each sweep will
take a few seconds. Such a receiver mode at high frequencies would work for
the detection of Saturn lightning, but previous attempts to use similar
frequency-sweeping receivers on a spacecraft at Jupiter have so far failed to
detect any Jovian sferics. Similarly, the RPWI LP receiver can use the
Langmuir probes in the electric field mode from DC to 1.5 MHz to produce
electric field spectra with low time resolution. Taken together, these
techniques will build a statistical picture of lightning phenomena on Jupiter,
relating lightning detection to discrete regions of features.

###  5.3 Stratospheric Chemistry

As described in Section 2.3.2, the vertical and meridional distributions of
Jupiter’s stratospheric hydrocarbons remain poorly understood. The high
latitude distributions of C2 species was first observed during the Cassini
flyby, with C2H2 and C2H6 showing opposite behaviours as a function of
latitude (Nixon et al., 2007a). Longitudinally resolved observations of the
auroral regions unveiled an even more complex situation, with a high degree of
variability in all three dimensions for the main C2 species (Sinclair et al.,
2018a) and for more complex hydrocarbons (Sinclair et al., 2019). Some binary
or multi star systems have both UV bright and near-infrared bright stars
collocated on the sky. Leveraging this group of unique targets, UVS and MAJIS
will be able to perform simultaneous occultation observations. These
synchronous observations will provide a high fidelity measurement of the
thermal and chemical structure structure from the lower thermosphere to the
troposphere. JANUS would contribute with contextual astrometry observations.
All these observations would be complemented by SWI limb observations of the
stratospheric thermal structure from CH4 observations at 1256 GHz and the
vertical profile of CH3C2H. These combined observations of the temperature and
hydrocarbon distributions would help to constrain photochemical and transport
models of Jupiter’s stratosphere (Moses et al., 2005b; Hue et al., 2018b),
alongside SWI measurements of the spatial distributions of long-lived H2O, CO,
HCN and CS deposited by the SL9 comet impact in 1994 and diffusing with
latitude and depth ever since (Moreno et al., 2003; Griffith et al., 2004;
Lellouch et al., 2002, 2006; Cavalié et al., 2013, 2022).

###  5.4 Auroral Morphology, Chemistry and Dynamics

Multi-wavelength simultaneous monitoring of the auroral emissions from the UV
to the submillimeter will enable better understanding the variability,
energetics, and dynamics of the auroras. UVS will perform regular meridional
scans of the auroras to monitor the morphology of the auroras. The produced
brightness and color ratio maps will make use of CH4, C2H6 and C2H2
distributions retrieved from UV stellar occultation experiments (see Fig. 16)
to capture the flux and energy of the precipitating auroral particles, giving
a measure of the auroral energy deposited into the polar region. MAJIS maps of
H${}_{3}^{+}$ emission give insight into the cooling due to radiation to space
of some of the auroral heating via H${}_{3}^{+}$ emissions (Gérard et al.,
2023). Thermospheric temperatures and H${}_{3}^{+}$ densities can be inferred
from the H${}_{3}^{+}$ emissions, while the upper stratospheric and lower
thermospheric temperatures can be captured by SWI observations of CH4 and HCN
lines, revealing how auroral processes contribute to heating and cooling of
the neutral atmosphere. JANUS observations of visible-light emissions will
provide context for the auroral morphology and vertical structure of the
auroral curtain (Vasavada et al., 1999). RPWI will detect electromagnetic
waves of various modes linked to auroral phenomena in a broad frequency range,
such as Alfvén waves, whistler mode waves, and free space mode radio waves.
Multicomponent measurements of fluctuating electric and magnetic fields will
be used to characterise the wave polarization and propagation properties,
including their Poynting flux.

Compositional contrasts between the auroral ovals and their surroundings will
be studied with UVS, MAJIS and SWI, and SWI will provide upper stratospheric
wind measurements to assess whether auroral winds measured from the ionosphere
(Rego et al., 1999; Stallard et al., 2001, 2003; Johnson et al., 2017) down to
the stratosphere (Cavalié et al., 2021) play an active role in favouring
auroral chemistry interior of the main ovals by confining photochemical
products in a region rich in energetic magnetospheric electrons. UVS and SWI
will also look in the moon auroral footprints for exogenic species possibly
transported from the Io (and Europa) torus to Jupiter’s atmosphere. For
instance, UVS is sensitive to SO2 and SWI can look for SO and SO2 lines. These
measurements, in combination with MAJIS H${}_{3}^{+}$ emission detection from
the moon footprints, will also try to solve the puzzling structure of the near
footprint tail (Mura et al., 2018).

###  5.5 Occultations and Waves

The spatial distribution of radio occultation opportunities was described in
Section 4.5 and shown in Figure 25. These will probe both the electron density
of the ionosphere and the temperature structure of the neutral atmosphere with
a high vertical resolution, at a variety of latitudes and local times. Once
the occultation is complete and JUICE has rotated back to Jupiter, remote
sensing instruments will be able to provide contextual measurements for the
same locations: for example, MAJIS observations of aerosols and NH3, SWI
measurements of temperatures and winds; and JANUS and UVS observations of any
layering observed in the aerosol field on the Jovian limb. Independently of
the radio occultations, stellar occultations observed by UVS, MAJIS and JANUS
will be coordinated to ensure multi-spectral context for any vertical
variability. This would allow vertically-propagating waves observed during the
radio/stellar occultations to be tied to thermal, aerosol, and chemical
layering observed on the planetary limb, and its variability with time.

##  6 JUICE Science in Context

###  6.1 Complementary Earth-Based Observations

JUICE will be orbiting the Jupiter system for the first half of the 2030s,
exploring the atmosphere and auroras from vantage points that can only be
achieved from an orbiting spacecraft. It will be joined by NASA’s Europa
Clipper mission, dedicated to the exploration of Europa but carrying exciting
additional capabilities for Jupiter science. However, just as with numerous
previous planetary missions (including Cassini and Juno), Earth-based
observatories, both professional and amateur, will be able to provide
significant spatial, temporal, and spectral support for these missions. In
terms of spatial context, imaging and spectroscopy from ground- and space-
based telescopes provide global, moderate-resolution views of Jupiter to
supplement the close-in high-resolution views of the spacecraft, aiding in
registration of observations and providing broader context (e.g., by
characterising environmental conditions across a broad belt or zone to support
JUICE observations of an embedded thunderstorm).

Given limitations on system resources (e.g., data volume), competition between
scientific disciplines, and the finite duration of the Jupiter tour, Earth-
based monitoring can also provide temporal context. As storms, vortices, and
the planetary bands evolve and shift over timescales ranging from days to
years, ground-based records can be used to track meteorological features.
Lucky-imaging techniques employed by amateur astronomers (Mousis et al., 2014)
produce high-quality Jupiter imaging on a near nightly basis. By stacking only
the sharpest frames, observers can reduce the blurring effects of atmospheric
seeing to create excellent images, which are then shared with the community
via repositories such as the Planetary Virtual Observatory (PVOL, Hueso et
al., 2018b) and the Association of Lunar and Planetary Observers (ALPO-
Japan222http://alpo-j.sakura.ne.jp/indexE.htm). Discrete storm features are
tracked from night to night to reconstruct zonal winds, wave patterns, and
drift of active domains. During Juno’s prime mission, such drift charts proved
essential for targeting JunoCam visible-light images. Asteroid and cometary
impacts caught by amateur imaging (Hueso et al., 2010, 2013, 2018a) can also
provide opportunities for JUICE to observe impact-driven alterations of
atmospheric composition and temperature. With advances expected in amateur
capabilities in the coming decade, and machine-learning approaches to tracking
atmospheric features, such long-term atmospheric monitoring will help to
connect the Jovian phenomena of the 2030s to the record of observations
spanning back decades (Rogers, 1995). Furthermore, ground-based infrared
(e.g., 3-4 $\mu$m H${}_{3}^{+}$) observations and space-based UV (e.g., HST,
if still operational in the 2030s) observations can track the fluctuating
auroral emissions over short timescales to complement the JUICE observations.

But perhaps the most important contribution from Earth-based observations is
access to wider wavelength ranges to provide spectral context, at potentially
higher spectral resolutions, than is possible from the JUICE spacecraft. For
example, JUICE does not have instrumentation spanning Jupiter X-ray emission
(e.g., Dunn et al., 2017; Yao et al., 2021), so cannot access the hard X-ray
bremsstrahlung emission, pulsed/flared soft X-ray emissions, and the dim
flickering aurora observed by the likes of Chandra and XMM Newton. These
facilities (or their successors) should be able to observe Jupiter in tandem
with JUICE to connect the X-ray emission to the remote sensing discussed in
Section 4. There is also a significant infrared gap in JUICE’s capabilities,
between the long-wave cutoff of MAJIS at 5.5 $\mu$m, and the 250 $\mu$m
channel of SWI. This spans the mid- and far-infrared spectrum previously
studied by Cassini/CIRS (Flasar et al., 2004), which provides a means of
mapping tropospheric and stratospheric temperatures via a host of absorption
and emission features, respectively. The MIRI instrument on JWST, which is
expected to be operating well into the 2030s, provides spectroscopic mapping
in the 5-11 $\mu$m range without saturation, but the fields of view are too
small (3-7” in size) to view the entirety of Jupiter without complex
mosaicking (Norwood et al., 2016). Thus the only imaging capabilities for the
mid- and far-infrared are likely to come from ground-based telescopes with 3-
and 8-m diameter primary mirrors, which will hopefully still be available to
the planetary community in the 2030s (at the time of writing, only a small
number of ageing mid-infrared instruments are still operational).

At even longer wavelengths, JUICE observations could be supported in the
millimetre, centimetre, and metre ranges by facilities like ALMA (Cavalié et
al., 2021), the next-generation Very Large Array (ngVLA, de Pater et al.,
2018), and the Square Kilometre Array (SKA, Butler et al., 2004). In the
continuum bands, these facilities are sensitive to temperatures, ammonia, and
possibly PH3 at depths below the cloud-forming region described in Section 2.
Joint campaigns between JUICE and these ground-based observatories could help
connect Jupiter’s dynamic weather layer to what is happening at great depth.
At decimeter to decameter wavelengths, Jupiter is one of the most prominent
celestial radio sources. LOFAR has revealed the first low frequency resolved
images of the radiation belts of Jupiter (Girard et al., 2016); the long
wavelength range makes the observations sensitive to the lower energy end of
the Jovian radiation belt electrons. Io-induced and non-Io decametric emission
have also been observed (Turner et al., 2019). LOFAR’s unprecedented long
baselines and spectra-temporal resolution also provide the opportunity to
image the dynamics of charge bunches causing Jovian decametric emission and
test physical models of the associated plasma instabilities (Zarka, 2004).
Jupiter is also likely to become an object of studies with prospective
spaceborne radio telescopes at wavelengths longer than 20-m at the hitherto
unreachable (to ground-based radio telescopes) ultra-low frequency part of the
electromagnetic spectrum (Bentum et al., 2020).

JUICE operations in the 2030s will be in an era of major new facilities for
astronomy. The European Extremely Large Telescope (ELT), a 39-m diameter
observatory based in the Atacama desert, will provide high-resolution
observations in the visible, near-infrared, and mid-infrared out to
approximately 14 $\mu$m. The primary science targets for the first-light
instruments require small fields of view, creating a substantial mosaicking
challenge for the large disc of Jupiter (but excellent for mapping the
Galilean satellites), but could nevertheless observe atmospheric phenomena at
the same time as JUICE. The Vera C. Rubin Observatory, previously known as the
Large Synoptic Survey Telescope (LSST), will begin operating in the 2020s,
increasing the catalogue of small objects throughout the solar system. Within
that extensive new survey, potential objects on collision courses with the
Jovian system could be identified early, and then JUICE observations adjusted
to investigate the aftermath. The JUICE tour will therefore retain some
flexibility in planning, to take advantage of potentially unique and
unforeseen opportunities during the mission, as highlighted in Section 3.

###  6.2 JUICE and Exoplanets

Finally, the JUICE mission will be operating in an era when our exploration of
extrasolar planets moves from a phase of detection into an era of
spectroscopic characterisation, via techniques such as transit spectroscopy
and direct imaging. The discovery of the first hot Jupiter exoplanet (Mayor
and Queloz, 1995) fundamentally modified our vision of the Solar System
planets. Firstly, planetary formation models have been challenged by the
discovery of the Jupiter-mass planets closer to their star than Mercury, with
the introduction of migration processes as a natural step following planet
formation (Morbidelli, 2020). Secondly, the mass distribution of the
$\sim$5000 exoplanets discovered to date exhibits a very different pattern
than that in the Solar System, with a peak in the mass range of 5–10 Earth
masses, corresponding to the “intermediate planets”, mini-Neptunes or super-
Earths, which are not found in our Solar System.

JUICE’s exploration in the 2030s will allow us to compare Jupiter’s
atmospheric phenomena and composition with the wider collection of extrasolar
giants, as the closest member of a class of astrophysical object. The wider
context and temperature range offered by exoplanet spectroscopic surveys could
reveal whether Jupiter is a more or less typical giant planet in composition
and structure, or a more rare and special product of our Solar System.
Similarly, the growing census of exo-planetary system architectures may also
lead to broader understanding of how Jupiter’s formation and migration shaped
the structure of our own Solar System. The climate, meteorology, energetics
and variability of Jupiter explored by JUICE will serve as the archetype for
hydrogen-dominated giant planets and Brown Dwarfs.

ESA’s ARIEL mission, to be launched in 2029 (Tinetti et al., 2018), is
expected to be contemporaneous to JUICE. ARIEL is devoted to a statistical
study of the composition of $\sim$1000 exoplanets from warm super-Earths to
hot Jupiters. Interaction between the science teams of these two missions
could therefore improve the science return of both, by addressing
astrophysical questions about planetary origins and environments in a much
broader context.

##  7 Summary

The exploration of Jupiter as an archetype for giant planets, both in our
Solar system and beyond, has been one of the two primary scientific objectives
of ESA’s JUICE mission since its original inception. Since that time, NASA’s
Juno mission has revealed a wealth of new insights into the interior,
atmosphere, and magnetosphere of the gas giant, prompting us to revisit the
JUICE scientific requirements in this article. Section 2 reviewed the current
status of Jupiter exploration, from the dynamic weather layer with its belts,
zones, vortices, and convective storms; to the chemistry and circulation of
the middle atmosphere; the global composition as a window onto planetary
origins; and the energetics and circulation of the ionosphere, thermosphere,
and auroras. JUICE will explore how these different layers are interconnected
and coupled, both to the circulations of the deep interior, and to the
processes at work in Jupiter’s magnetosphere. These themes are used to justify
the JUICE Jupiter science requirements in Table 1.

Section 3 then described how the 3.5-year Jupiter tour, with its equatorial
and inclined phases bringing JUICE within 700,000 km of Jupiter at the closest
perijoves, provides the observational opportunities needed to achieve the
science goals. JUICE’s long-term monitoring of atmospheric and auroral
phenomena, its global perspective from a variety of phase angles (dayside to
nightside), and its near-equatorial vantage point all complement Juno’s close-
in regional views of Jupiter from its highly-inclined orbit, its 40-to-50-day
separation of perijoves, and its near-terminator ($90^{\circ}$ phase angle)
viewing geometry. The high-inclination phase enables excellent spatial and
temporal coverage of Jupiter’s polar atmosphere and auroras, some 5-10 years
after the Juno mission.

Section 4 then described the subset of instruments that are needed to achieve
closure with respect to the JUICE science requirements: namely the remote
sensing instruments (JANUS, MAJIS, UVS and SWI), radio occultations (3GM) and
radio and plasma wave measurements (RPWI). These instruments offer flexible
opportunities and modes, working within the spacecraft resource envelope of
power and data volume, and can operate both independently and synergistically
(Section 5 to explore phenomena across a broad spectral range. UVS covers the
50-204 nm range of the far-UV (similar to the 68-210 nm range of Juno/UVS);
JANUS provides multi-wavelength imaging from 340 to 1080 nm (complementing the
R, G, B and CH4 bands on Juno/JunoCam); and MAJIS provides visible and near-
infrared spectroscopy from 0.49 to 5.56 $\mu$m (extending the 2.0-5.0 $\mu$m
coverage of Juno/JIRAM). SWI provides a unique capability to access the
temperatures, winds, and composition high in Jupiter’s stratosphere, using
sub-millimetre spectroscopy in two channels, 530-625 GHz (479-565 $\mu$m) and
1080-1275 GHz (235-277 $\mu$m). JUICE does not have capabilities in the mid-
infrared (5.5-30 $\mu$m), nor in the microwave ($>1$ cm, like Juno/MWR) or
X-ray. JUICE observations will therefore be supported by ground- and space-
based observatories (including JWST) wherever possible (Section 6). Finally,
3GM radio occultations will provide electron and neutral temperature profiles
at a range of latitudes, longitudes, and local times, complementing those
being acquired by Juno during its extended mission.

JUICE launched in April 2023, and the scientific questions will no doubt
evolve as JUICE cruises towards Jupiter in the 2020s, informed by discoveries
made by Juno, by ground- and space-based observatories, by theoretical
modelling, by laboratory investigations, and by the ongoing characterisation
of giant exoplanets. Most importantly, Jupiter has the ability to surprise us,
with unforeseen connections, unexpected events, and new puzzles. The JUICE
spacecraft, scientific payload, and orbital tour have been designed to
maximise our capability to explore the unexpected, and to provide our best
four-dimensional characterisation of this archetypal giant planet.

###### Acknowledgements.

We wish to express our gratitude to the teams of scientists, engineers, and
mission planners that have made JUICE a reality, far beyond those scientists
listed here as co-authors. Without them, the scientific potential expressed in
this article would remain unrealised. L.N. Fletcher is a JUICE
Interdisciplinary Scientist supported by a European Research Council
Consolidator Grant (under the European Union’s Horizon 2020 research and
innovation programme, grant agreement No 723890) at the University of
Leicester. T. Cavalié acknowledges support from CNES and the Programme
National de Planétologie (PNP) of CNRS/INSU. Fletcher and Cavalié have jointly
chaired the ‘JUICE Jupiter Working Group’ since 2015. D. Grassi, P. Palumbo,
G. Piccioni, F. Altieri and A. Mura were supported by Italian Space Agency
“Accordo ASI-INAF n. 2018-25-HH.0, Attività scientifiche per JUICE fase C/D”.
The Italian contribution to MAJIS has been coordinated and funded by the
Italian Space Agency (contract 2021-18-I.0), and supported by the ASI-INAF
agreement number 2023-6-HH.0. R. Hueso and A. Sánchez-Lavega were supported by
grant PID2019-109467GB-I00 funded by MCIN/AEI/10.13039/501100011033/ and
Grupos Gobierno Vasco IT- 1742-22. L. M. Lara was supported by project
PGC2018-099425-B-I00 (MCI/AEI/FEDER, UE). Y. Kaspi, E. Galanti and M. Smirnova
were supported by the Israeli Space Agency. T. K. Greathouse, P. M. Molyneux,
G.R. Gladstone and K. D. Retherford acknowledge NASA funding supporting the
UVS team for ESA’s JUICE mission. M. Galand was supported by the UK Space
Agency [grant number ST/W001071/1]. The JUICE/RPWI efforts are supported by
the Swedish National Space Agency (SNSA). I. Kolmasova and O. Santolik were
supported from the Czech contribution to the ESA PRODEX programme and from the
MŠMT grant LUAUS23152. P. G. J. Irwin acknowledges the support of the UK
Science and Technology Facilities Council (ST/S000461/1). A. Coustenis was
supported by the Centre National d’Études Spatiales (CNES) in France. G. H.
Jones acknowledges the support of the UK Science and Technology Facilities
Council, as well as to the International Space Science Institute, ISSI, Bern,
for support as a Visiting Scientist. We wish to express our gratitude to two
anonymous referees, and to T. M. Bocanegra-Bahamón, for their help in
improving this manuscript.

## Conflict of Interest Statement

The authors declare that they have no competing financial or non-financial
interests to declare that are relevant to the content of this article.

## References

  * Achilleos et al. (1998) N. Achilleos, S. Miller, J. Tennyson, A.D. Aylward, I. Mueller-Wodarg, D. Rees, JIM: A time-dependent, three-dimensional model of Jupiter’s thermosphere and ionosphere. Journal of Geophysical Research 103(E9), 20089–20112 (1998). doi:10.1029/98JE00947
  * Achterberg et al. (2006) R.K. Achterberg, B.J. Conrath, P.J. Gierasch, Cassini CIRS retrievals of Ammonia in Jupiter’s Upper Troposphere. Icarus 182, 169–180 (2006). doi:10.1016/j.icarus.2005.12.020
  * Adriani et al. (2017) A. Adriani, A. Mura, M.L. Moriconi, B.M. Dinelli, F. Fabiano, F. Altieri, G. Sindoni, S.J. Bolton, J.E.P. Connerney, S.K. Atreya, F. Bagenal, J.-C.M.C. Gérard, G. Filacchione, F. Tosi, A. Migliorini, D. Grassi, G. Piccioni, R. Noschese, A. Cicchetti, G.R. Gladstone, C. Hansen, W.S. Kurth, S.M. Levin, B.H. Mauk, D.J. McComas, A. Olivieri, D. Turrini, S. Stefani, M. Amoroso, Preliminary JIRAM results from Juno polar observations: 2. Analysis of the Jupiter southern H3+ emissions and comparison with the north aurora. Geophys. Res. Lett. 44(10), 4633–4640 (2017). doi:10.1002/2017GL072905
  * Adriani et al. (2018a) A. Adriani, M.L. Moriconi, F. Altieri, G. Sindoni, D. Grassi, L.N. Fletcher, H. Melin, A. Mura, A.P. Ingersoll, S.K. Atreya, F. Tosi, A. Cicchetti, R. Noschese, J.I. Lunine, G.S. Orton, C. Plainaki, R. Sordini, A. Olivieri, S. Bolton, J.E.P. Connerney, S. Levin, Characterization of mesoscale waves in Jupiter’s NEB by Jupiter InfraRed Auroral Mapper onboard Juno. in preparation (2018a)
  * Adriani et al. (2018b) A. Adriani, A. Mura, G. Orton, C. Hansen, F. Altieri, M.L. Moriconi, J. Rogers, G. Eichstädt, T. Momary, A.P. Ingersoll, G. Filacchione, G. Sindoni, F. Tabataba-Vakili, B.M. Dinelli, F. Fabiano, S.J. Bolton, J.E.P. Connerney, S.K. Atreya, J.I. Lunine, F. Tosi, A. Migliorini, D. Grassi, G. Piccioni, R. Noschese, A. Cicchetti, C. Plainaki, A. Olivieri, M.E. O’Neill, D. Turrini, S. Stefani, R. Sordini, M. Amoroso, Clusters of cyclones encircling Jupiter’s poles. Nature 555(7695), 216–219 (2018b). doi:10.1038/nature25491
  * Allegrini et al. (2020) F. Allegrini, B. Mauk, G. Clark, G.R. Gladstone, V. Hue, W.S. Kurth, F. Bagenal, S. Bolton, B. Bonfond, J.E.P. Connerney, R.W. Ebert, T. Greathouse, M. Imai, S. Levin, P. Louarn, D.J. McComas, J. Saur, J.R. Szalay, P.W. Valek, R.J. Wilson, Energy Flux and Characteristic Energy of Electrons Over Jupiter’s Main Auroral Emission. Journal of Geophysical Research (Space Physics) 125(4), 27693 (2020). doi:10.1029/2019JA027693
  * Allison (1990) M. Allison, Planetary waves in Jupiter’s equatorial atmosphere. Icarus 83, 282–307 (1990). doi:10.1016/0019-1035(90)90069-L
  * Anderson et al. (2022) C.M. Anderson, N. Biver, G.L. Bjoraker, T. Cavalié, G. Chin, M.A. DiSanti, P. Hartogh, A. Tielens, C.K. Walker, Solar System Science with the Orbiting Astronomical Satellite Investigating Stellar Systems (OASIS) Observatory. Space Sci. Rev. 218(5), 43 (2022). doi:10.1007/s11214-022-00911-5
  * Anguiano-Arteaga et al. (2021) A. Anguiano-Arteaga, S. Pérez-Hoyos, A. Sánchez-Lavega, J.F. Sanz-Requena, P.G.J. Irwin, Vertical Distribution of Aerosols and Hazes Over Jupiter’s Great Red Spot and Its Surroundings in 2016 From HST/WFC3 Imaging. Journal of Geophysical Research (Planets) 126(11), 06996 (2021). doi:10.1029/2021JE006996
  * Antuñano et al. (2018) A. Antuñano, L.N. Fletcher, G.S. Orton, H. Melin, J.H. Rogers, J. Harrington, P.T. Donnelly, N. Rowe-Gurney, J.S.D. Blake, Infrared Characterization of Jupiter’s Equatorial Disturbance Cycle. Geophys. Res. Lett. 45, 10 (2018). doi:10.1029/2018GL080382
  * Antuñano et al. (2019) A. Antuñano, L.N. Fletcher, G.S. Orton, H. Melin, S. Milan, J. Rogers, T. Greathouse, J. Harrington, P.T. Donnelly, R. Giles, Jupiter’s Atmospheric Variability from Long-term Ground-based Observations at 5 $\mu$m. Astronomical Journal 158(3), 130 (2019). doi:10.3847/1538-3881/ab2cd6
  * Antuñano et al. (2021) A. Antuñano, R.G. Cosentino, L.N. Fletcher, A.A. Simon, T.K. Greathouse, G.S. Orton, Fluctuations in Jupiter’s equatorial stratospheric oscillation. Nature Astronomy 5, 71–77 (2021). doi:10.1038/s41550-020-1165-5
  * Arregi et al. (2006) J. Arregi, J.F. Rojas, A. Sánchez-Lavega, A. Morgado, Phase dispersion relation of the 5-micron hot spot wave from a long-term study of Jupiter in the visible. Journal of Geophysical Research (Planets) 111, 9010 (2006). doi:10.1029/2005JE002653
  * Arregi et al. (2009) J. Arregi, J.F. Rojas, R. Hueso, A. Sánchez-Lavega, Gravity waves in Jupiter’s equatorial clouds observed by the Galileo orbiter. Icarus 202, 358–360 (2009). doi:10.1016/j.icarus.2009.03.028
  * Atkinson et al. (1998) D.H. Atkinson, J.B. Pollack, A. Seiff, The Galileo probe Doppler wind experiment: Measurement of the deep zonal winds on Jupiter. J. Geophys. Res. 103, 22911–22928 (1998). doi:10.1029/98JE00060
  * Atreya et al. (1999) S.K. Atreya, M.H. Wong, T.C. Owen, P.R. Mahaffy, H.B. Niemann, I. de Pater, P. Drossart, T. Encrenaz, A comparison of the atmospheres of Jupiter and Saturn: deep atmospheric composition, cloud structure, vertical mixing, and origin. Plan. & Space Sci. 47, 1243–1262 (1999)
  * Atreya et al. (2003) S.K. Atreya, P.R. Mahaffy, H.B. Niemann, M.H. Wong, T.C. Owen, Composition and origin of the atmosphere of Jupiter-an update, and implications for the extrasolar giant planets. Plan. & Space Sci. 51, 105–112 (2003). doi:10.1016/S0032-0633(02)00144-7
  * Baines et al. (2007) K.H. Baines, A.A. Simon-Miller, G.S. Orton, H.A. Weaver, A. Lunsford, T.W. Momary, J. Spencer, A.F. Cheng, D.C. Reuter, D.E. Jennings, G.R. Gladstone, J. Moore, S.A. Stern, L.A. Young, H. Throop, P. Yanamandra-Fisher, B.M. Fisher, J. Hora, M.E. Ressler, Polar Lightning and Decadal-Scale Cloud Variability on Jupiter. Science 318, 226–228 (2007). doi:10.1126/science.1147912
  * Baines et al. (2019) K.H. Baines, L.A. Sromovsky, R.W. Carlson, T.W. Momary, P.M. Fry, The visual spectrum of Jupiter’s Great Red Spot accurately modeled with aerosols produced by photolyzed ammonia reacting with acetylene. Icarus 330, 217–229 (2019). doi:10.1016/j.icarus.2019.04.008
  * Baines et al. (2002) K.H. Baines, R.W. Carlson, L.W. Kamp, Fresh Ammonia Ice Clouds in Jupiter I. Spectroscopic Identification, Spatial Distribution, and Dynamical Implications. Icarus 159(1), 74–94 (2002)
  * Barcilon and Gierasch (1970) A. Barcilon, P. Gierasch, A Moist, Hadley Cell Model for Jupiter’s Cloud Bands. Journal of Atmospheric Sciences 27, 550–560 (1970). doi:10.1175/1520-0469(1970)027¡0550:AMHCMF¿2.0.CO;2
  * Barrado-Izagirre et al. (2008a) N. Barrado-Izagirre, A. Sánchez-Lavega, S. Pérez-Hoyos, R. Hueso, Jupiter’s polar clouds and waves from Cassini and HST images: 1993 2006\. Icarus 194, 173–185 (2008a). doi:10.1016/j.icarus.2007.08.025
  * Barrado-Izagirre et al. (2008b) N. Barrado-Izagirre, A. Sánchez-Lavega, S. Pérez-Hoyos, R. Hueso, Jupiter’s polar clouds and waves from Cassini and HST images: 1993 2006\. Icarus 194(1), 173–185 (2008b). doi:10.1016/j.icarus.2007.08.025
  * Becker et al. (2020a) H.N. Becker, J.W. Alexander, S.K. Atreya, S.J. Bolton, M.J. Brennan, S.T. Brown, A. Guillaume, T. Guillot, A.P. Ingersoll, S.M. Levin, J.I. Lunine, Y.S. Aglyamov, P.G. Steffes, Small lightning flashes from shallow electrical storms on Jupiter. Nature 584(7819), 55–58 (2020a). doi:10.1038/s41586-020-2532-1
  * Becker et al. (2020b) H.N. Becker, J.W. Alexander, S.K. Atreya, S.J. Bolton, M.J. Brennan, S.T. Brown, A. Guillaume, T. Guillot, A.P. Ingersoll, S.M. Levin, J.I. Lunine, Y.S. Aglyamov, P.G. Steffes, Small lightning flashes from shallow electrical storms on Jupiter. Nature 584(7819), 55–58 (2020b). doi:10.1038/s41586-020-2532-1
  * Belton et al. (1992) M.J.S. Belton, K.P. Klaasen, M.C. Clary, J.L. Anderson, C.D. Anger, M.H. Carr, C.R. Chapman, M.E. Davies, R. Greeley, D. Anderson, L.K. Bolef, T.E. Townsend, R. Greenberg, I. Head James W., G. Neukum, C.B. Pilcher, J. Veverka, P.J. Gierasch, F.P. Fanale, A.P. Ingersoll, H. Masursky, D. Morrison, J.B. Pollack, The Galileo Solid-State Imaging experiment. Space Sci. Rev. 60(1-4), 413–455 (1992). doi:10.1007/BF00216864
  * Benmahi et al. (2020) B. Benmahi, T. Cavalié, M. Dobrijevic, N. Biver, K. Bermudez-Diaz, A. Sandqvist, E. Lellouch, R. Moreno, T. Fouchet, V. Hue, P. Hartogh, F. Billebaud, A. Lecacheux, Å. Hjalmarson, U. Frisk, M. Olberg, Odin Team, Monitoring of the evolution of H2O vapor in the stratosphere of Jupiter over an 18-yr period with the Odin space telescope. Astron. Astrophys. 641, 140 (2020). doi:10.1051/0004-6361/202038188
  * Benmahi et al. (2021) B. Benmahi, T. Cavalié, T.K. Greathouse, V. Hue, R. Giles, S. Guerlet, A. Spiga, R. Cosentino, Mapping the zonal winds of Jupiter’s stratospheric equatorial oscillation. Astron. Astrophys. 652, 125 (2021). doi:10.1051/0004-6361/202141523
  * Benmahi et al. (2022) B. Benmahi, T. Cavalié, T. Fouchet, R. Moreno, E. Lellouch, D. Bardet, S. Guerlet, V. Hue, A. Spiga, First absolute wind measurements in Saturn’s stratosphere from ALMA observations. Astron. Astrophys. 666, 117 (2022). doi:10.1051/0004-6361/202244200
  * Bentum et al. (2020) M.J. Bentum, M.K. Verma, R.T. Rajan, A.J. Boonstra, C.J.M. Verhoeven, E.K.A. Gill, A.J. van der Veen, H. Falcke, M.K. Wolt, B. Monna, S. Engelen, J. Rotteveel, L.I. Gurvits, A roadmap towards a space-based radio telescope for ultra-low frequency radio astronomy. Advances in Space Research 65(2), 856–867 (2020). doi:10.1016/j.asr.2019.09.007
  * Bézard et al. (2002) B. Bézard, E. Lellouch, D. Strobel, J.-P. Maillard, P. Drossart, Carbon Monoxide on Jupiter: Evidence for Both Internal and External Sources. Icarus 159, 95–111 (2002). doi:10.1006/icar.2002.6917
  * Bhattacharyya et al. (2018) D. Bhattacharyya, J.T. Clarke, J. Montgomery, B. Bonfond, J.-C. Gérard, D. Grodent, Evidence for Auroral Emissions From Callisto’s Footprint in HST UV Images. Journal of Geophysical Research (Space Physics) 123(1), 364–373 (2018). doi:10.1002/2017JA024791
  * Bjoraker et al. (2018) G.L. Bjoraker, M.H. Wong, I. de Pater, T. Hewagama, M. Ádámkovics, G.S. Orton, The Gas Composition and Deep Cloud Structure of Jupiter’s Great Red Spot. Astron. J. 156(3), 101 (2018). doi:10.3847/1538-3881/aad186
  * Blanc and Greeley (2010) M. Blanc, R. Greeley, Science of the Joint ESA-NASA Europa Jupiter System Mission (EJSM), in EGU General Assembly Conference Abstracts. EGU General Assembly Conference Abstracts, 2010, p. 13347
  * Blanc et al. (2009) M. Blanc, Y. Alibert, N. André, S. Atreya, R. Beebe, W. Benz, S.J. Bolton, A. Coradini, A. Coustenis, V. Dehant, M. Dougherty, P. Drossart, M. Fujimoto, O. Grasset, L. Gurvits, P. Hartogh, H. Hussmann, Y. Kasaba, M. Kivelson, K. Khurana, N. Krupp, P. Louarn, J. Lunine, M. McGrath, D. Mimoun, O. Mousis, J. Oberst, T. Okada, R. Pappalardo, O. Prieto-Ballesteros, D. Prieur, P. Regnier, M. Roos-Serote, S. Sasaki, G. Schubert, C. Sotin, T. Spilker, Y. Takahashi, T. Takashima, F. Tosi, D. Turrini, T. van Hoolst, L. Zelenyi, LAPLACE: A mission to Europa and the Jupiter System for ESA’s Cosmic Vision Programme. Experimental Astronomy 23(3), 849–892 (2009). doi:10.1007/s10686-008-9127-4
  * Bocanegra-Bahamón et al. (2018) T.M. Bocanegra-Bahamón, G. Molera Calvés, L.I. Gurvits, D.A. Duev, S.V. Pogrebenko, G. Cimò, D. Dirkx, P. Rosenblatt, Planetary Radio Interferometry and Doppler Experiment (PRIDE) technique: A test case of the Mars Express Phobos Flyby. II. Doppler tracking: Formulation of observed and computed values, and noise budget. Astron. Astrophys. 609, 59 (2018). doi:10.1051/0004-6361/201731524
  * Bocanegra-Bahamón et al. (2019) T.M. Bocanegra-Bahamón, G. Molera Calvés, L.I. Gurvits, G. Cimò, D. Dirkx, D.A. Duev, S.V. Pogrebenko, P. Rosenblatt, S. Limaye, L. Cui, P. Li, T. Kondo, M. Sekido, A.G. Mikhailov, M.A. Kharinov, A.V. Ipatov, W. Wang, W. Zheng, M. Ma, J.E.J. Lovell, J.N. McCallum, Venus Express radio occultation observed by PRIDE. Astron. Astrophys. 624, 59 (2019). doi:10.1051/0004-6361/201833160
  * Bolton et al. (2017) S.J. Bolton, A. Adriani, V. Adumitroaie, M. Allison, J. Anderson, S. Atreya, J. Bloxham, S. Brown, J.E.P. Connerney, E. DeJong, W. Folkner, D. Gautier, D. Grassi, S. Gulkis, T. Guillot, C. Hansen, W.B. Hubbard, L. Iess, A. Ingersoll, M. Janssen, J. Jorgensen, Y. Kaspi, S.M. Levin, C. Li, J. Lunine, Y. Miguel, A. Mura, G. Orton, T. Owen, M. Ravine, E. Smith, P. Steffes, E. Stone, D. Stevenson, R. Thorne, J. Waite, D. Durante, R.W. Ebert, T.K. Greathouse, V. Hue, M. Parisi, J.R. Szalay, R. Wilson, Jupiter’s interior and deep atmosphere: The initial pole-to-pole passes with the Juno spacecraft. Science 356, 821–825 (2017). doi:10.1126/science.aal2108
  * Bolton et al. (2021) S.J. Bolton, S.M. Levin, T. Guillot, C. Li, Y. Kaspi, G. Orton, M.H. Wong, F. Oyafuso, M. Allison, J. Arballo, S. Atreya, H.N. Becker, J. Bloxham, S.T. Brown, L.N. Fletcher, E. Galanti, S. Gulkis, M. Janssen, A. Ingersoll, J.L. Lunine, S. Misra, P. Steffes, D. Stevenson, J.H. Waite, R.K. Yadav, Z. Zhang, Microwave observations reveal the deep extent and structure of Jupiter’s atmospheric vortices. Science 374(6570), 968–972 (2021). doi:10.1126/science.abf1015
  * Bonfond et al. (2017) B. Bonfond, G.R. Gladstone, D. Grodent, T.K. Greathouse, M.H. Versteeg, V. Hue, M.W. Davis, M.F. Vogt, J.-C. Gérard, A. Radioti, S. Bolton, S.M. Levin, J.E.P. Connerney, B.H. Mauk, P. Valek, A. Adriani, W.S. Kurth, Morphology of the UV aurorae Jupiter during Juno’s first perijove observations. Geophys. Res. Lett. 44(10), 4463–4471 (2017). doi:10.1002/2017GL073114
  * Bonfond et al. (2021a) B. Bonfond, Z.H. Yao, G.R. Gladstone, D. Grodent, J.-C. Gérard, J. Matar, B. Palmaerts, T.K. Greathouse, V. Hue, M.H. Versteeg, J.A. Kammer, R.S. Giles, C. Tao, M.F. Vogt, A. Mura, A. Adriani, B.H. Mauk, W.S. Kurth, S.J. Bolton, Are Dawn Storms Jupiter’s Auroral Substorms? AGU Advances 2(1), 00275 (2021a). doi:10.1029/2020AV000275
  * Bonfond et al. (2021b) B. Bonfond, Z.H. Yao, G.R. Gladstone, D. Grodent, J.-C. Gérard, J. Matar, B. Palmaerts, T.K. Greathouse, V. Hue, M.H. Versteeg, J.A. Kammer, R.S. Giles, C. Tao, M.F. Vogt, A. Mura, A. Adriani, B.H. Mauk, W.S. Kurth, S.J. Bolton, Are Dawn Storms Jupiter’s Auroral Substorms? AGU Advances 2(1), 00275 (2021b). doi:10.1029/2020AV000275
  * Borucki and Williams (1986) W.J. Borucki, M.A. Williams, Lightning in the Jovian water cloud. J. Geophys. Res. 91, 9893–9903 (1986). doi:10.1029/JD091iD09p09893
  * Borucki et al. (1996) W.J. Borucki, C.P. McKay, D. Jebens, H.S. Lakkaraju, C.T. Vanajakshi, Spectral Irradiance Measurements of Simulated Lightning in Planetary Atmospheres. Icarus 123(2), 336–344 (1996). doi:10.1006/icar.1996.0162
  * Boutonnet et al. (in prep.) Boutonnet et al., JUICE Trajectory Design. Space Science Reviews (in prep.)
  * Braude et al. (2020) A.S. Braude, P.G.J. Irwin, G.S. Orton, L.N. Fletcher, Colour and tropospheric cloud structure of Jupiter from MUSE/VLT: Retrieving a universal chromophore. Icarus 338, 113589 (2020). doi:10.1016/j.icarus.2019.113589
  * Brown et al. (2018) S. Brown, M. Janssen, V. Adumitroaie, S. Atreya, S. Bolton, S. Gulkis, A. Ingersoll, S. Levin, C. Li, L. Li, J. Lunine, S. Misra, G. Orton, P. Steffes, F. Tabataba-Vakili, I. Kolmašová, M. Imai, O. Santolík, W. Kurth, G. Hospodarsky, D. Gurnett, J. Connerney, Prevalent lightning sferics at 600 megahertz near Jupiter’s poles. Nature 558, 87–90 (2018). doi:10.1038/s41586-018-0156-5
  * Butler et al. (2004) B.J. Butler, D.B. Campbell, I. de Pater, D.E. Gary, Solar system science with SKA. New Astron. Rev. 48(11-12), 1511–1535 (2004). doi:10.1016/j.newar.2004.09.031
  * Cao and Stevenson (2017) H. Cao, D.J. Stevenson, Zonal flow magnetic field interaction in the semi-conducting region of giant planets. Icarus 296, 59–72 (2017). doi:10.1016/j.icarus.2017.05.015
  * Cappuccio et al. (2022) P. Cappuccio, M. Di Benedetto, D. Durante, L. Iess, Callisto and Europa Gravity Measurements from JUICE 3GM Experiment Simulation. Plan. Sci. J. 3(8), 199 (2022). doi:10.3847/PSJ/ac83c4
  * Cavalié et al. (2023) T. Cavalié, J. Lunine, O. Mousis, A subsolar oxygen abundance or a raditaive region revealed by thermochemical modeling. Nat. Astron. accepted (2023). doi:10.1038/s41550-023-01928-8
  * Cavalié et al. (2008) T. Cavalié, F. Billebaud, N. Biver, M. Dobrijevic, E. Lellouch, J. Brillet, A. Lecacheux, Å. Hjalmarson, A. Sandqvist, U. Frisk, M. Olberg, E.A. Bergin, The Odin Team, Observation of water vapor in the stratosphere of Jupiter with the Odin space telescope. Planet. Space Sci. 56, 1573–1584 (2008). doi:10.1016/j.pss.2008.04.013
  * Cavalié et al. (2010) T. Cavalié, P. Hartogh, F. Billebaud, M. Dobrijevic, T. Fouchet, E. Lellouch, T. Encrenaz, J. Brillet, G.H. Moriarty-Schieven, A cometary origin for CO in the stratosphere of Saturn? Astron. Astrophys. 510, 88 (2010)
  * Cavalié et al. (2012) T. Cavalié, N. Biver, P. Hartogh, M. Dobrijevic, F. Billebaud, E. Lellouch, A. Sandqvist, J. Brillet, A. Lecacheux, Å. Hjalmarson, U. Frisk, M. Olberg, Odin Team, Odin space telescope monitoring of water vapor in the stratosphere of Jupiter. Planet. Space Sci. 61, 3–14 (2012). doi:10.1016/j.pss.2011.04.001
  * Cavalié et al. (2013) T. Cavalié, H. Feuchtgruber, E. Lellouch, M. de Val-Borro, C. Jarchow, R. Moreno, P. Hartogh, G. Orton, T.K. Greathouse, F. Billebaud, M. Dobrijevic, L.M. Lara, A. González, H. Sagawa, Spatial distribution of water in the stratosphere of Jupiter from Herschel HIFI and PACS observations. Astron. Astrophys. 553, 21 (2013). doi:10.1051/0004-6361/201220797
  * Cavalié et al. (2014) T. Cavalié, R. Moreno, E. Lellouch, P. Hartogh, O. Venot, G.S. Orton, C. Jarchow, T. Encrenaz, F. Selsis, F. Hersant, L.N. Fletcher, The first submillimeter observation of CO in the stratosphere of Uranus. Astron. Astrophys. 562, 33 (2014). doi:10.1051/0004-6361/201322297
  * Cavalié et al. (2019) T. Cavalié, V. Hue, P. Hartogh, R. Moreno, E. Lellouch, H. Feuchtgruber, C. Jarchow, T. Cassidy, L.N. Fletcher, F. Billebaud, M. Dobrijevic, L. Rezac, G.S. Orton, M. Rengel, T. Fouchet, S. Guerlet, Herschel map of Saturn’s stratospheric water, delivered by the plumes of Enceladus. Astron. Astrophys. 630, 87 (2019). doi:10.1051/0004-6361/201935954
  * Cavalié et al. (2021) T. Cavalié, B. Benmahi, V. Hue, R. Moreno, E. Lellouch, T. Fouchet, P. Hartogh, L. Rezac, T.K. Greathouse, G.R. Gladstone, J.A. Sinclair, M. Dobrijevic, F. Billebaud, C. Jarchow, First direct measurement of auroral and equatorial jets in the stratosphere of Jupiter. Astron. Astrophys 647, 8 (2021). doi:10.1051/0004-6361/202140330
  * Cavalié et al. (2022) T. Cavalié, L. Rezac, R. Moreno, E. Lellouch, T. Fouchet, B. Benmahi, T.K. Greathouse, J.A. Sinclair, V. Hue, P. Hartogh, M. Dobrijevic, N. Carrasco, Z. Perrin, Evidence for auroral influence on Jupiter’s stratospheric composition revealed by ALMA. Nat. Astron. submitted (2022)
  * Cheng et al. (2008a) A.F. Cheng, A.A. Simon-Miller, H.A. Weaver, K.H. Baines, G.S. Orton, P.A. Yanamandra-Fisher, O. Mousis, E. Pantin, L. Vanzi, L.N. Fletcher, J.R. Spencer, S.A. Stern, J.T. Clarke, M.J. Mutchler, K.S. Noll, Changing Characteristics of Jupiter’s Little Red Spot. Astronomical Journal 135, 2446–2452 (2008a). doi:10.1088/0004-6256/135/6/2446
  * Cheng et al. (2008b) A.F. Cheng, H.A. Weaver, S.J. Conard, M.F. Morgan, O. Barnouin-Jha, J.D. Boldt, K.A. Cooper, E.H. Darlington, M.P. Grey, J.R. Hayes, K.E. Kosakowski, T. Magee, E. Rossano, D. Sampath, C. Schlemm, H.W. Taylor, Long-Range Reconnaissance Imager on New Horizons. Space Sci. Rev. 140(1-4), 189–215 (2008b). doi:10.1007/s11214-007-9271-6
  * Choi et al. (2013) D.S. Choi, A.P. Showman, A.R. Vasavada, A.A. Simon-Miller, Meteorology of Jupiter’s equatorial hot spots and plumes from Cassini. Icarus 223, 832–843 (2013). doi:10.1016/j.icarus.2013.02.001
  * Christensen et al. (2020) U.R. Christensen, J. Wicht, W. Dietrich, Mechanisms for Limiting the Depth of Zonal Winds in the Gas Giant Planets. Astrophys. J. 890(1), 61 (2020). doi:10.3847/1538-4357/ab698c
  * Clarke et al. (2004) J.T. Clarke, D. Grodent, S.W.H. Cowley, E.J. Bunce, P. Zarka, J.E.P. Connerney, T. Satoh, In Jupiter. The Planet, Satellites and Magnetosphere, in Jupiter’s Aurora, 2004, pp. 79–104
  * Clarke et al. (2009) J.T. Clarke, J. Nichols, J.-C. Gérard, D. Grodent, K.C. Hansen, W. Kurth, G.R. Gladstone, J. Duval, S. Wannawichian, E. Bunce, S.W.H. Cowley, F. Crary, M. Dougherty, L. Lamy, D. Mitchell, W. Pryor, K. Retherford, T. Stallard, B. Zieger, P. Zarka, B. Cecconi, Response of Jupiter’s and Saturn’s auroral activity to the solar wind. Journal of Geophysical Research (Space Physics) 114(A5), 05210 (2009). doi:10.1029/2008JA013694
  * Connerney (1986) J.E.P. Connerney, Magnetic connection for Saturn’s rings and atmosphere. Geophys. Res. Lett. 13(8), 773–776 (1986). doi:10.1029/GL013i008p00773
  * Conrath and Pirraglia (1983) B.J. Conrath, J.A. Pirraglia, Thermal structure of Saturn from Voyager infrared measurements - Implications for atmospheric dynamics. Icarus 53, 286–292 (1983). doi:10.1016/0019-1035(83)90148-3
  * Cosentino et al. (2017a) R.G. Cosentino, B. Butler, R.J. Sault, R. Morales-Juberías, A.A. Simon, I. de Pater, Atmospheric waves and dynamics beneath Jupiter’s clouds from radio wavelength observations. Icarus, in press (2017a). doi:http://dx.doi.org/10.1016/j.icarus.2017.01.006
  * Cosentino et al. (2017b) R.G. Cosentino, R. Morales-Juberías, T. Greathouse, G. Orton, P. Johnson, L.N. Fletcher, A. Simon, New Observations and Modeling of Jupiter’s Quasi-Quadrennial Oscillation. J. Geophys. Res. 122(12), 2719–2744 (2017b). doi:10.1002/2017JE005342
  * Cowley and Bunce (2001) S.W.H. Cowley, E.J. Bunce, Origin of the main auroral oval in Jupiter’s coupled magnetosphere-ionosphere system. Plan. & Space Sci. 49(10-11), 1067–1088 (2001). doi:10.1016/S0032-0633(00)00167-7
  * Dahl et al. (2021) E.K. Dahl, N.J. Chanover, G.S. Orton, K.H. Baines, J.A. Sinclair, D.G. Voelz, E.A. Wijerathna, P.D. Strycker, P.G.J. Irwin, Vertical Structure and Color of Jovian Latitudinal Cloud Bands during the Juno Era. Plan. Sci. J. 2(1), 16 (2021). doi:10.3847/PSJ/abd400
  * Davis et al. (2020) M.W. Davis, G.R. Gladstone, R.S. Giles, T.K. Greathouse, P.M. Molyneux, U. Raut, K.D. Retherford, S. Baldor, M.H. Versteeg, M. Freeman, K. Persson, S.C. Persyn, Ground calibration results of the JUICE ultraviolet spectrograph, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series. Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, vol. 11444, 2020, p. 1144404. doi:10.1117/12.2562986
  * de Pater et al. (2016) I. de Pater, R.J. Sault, B. Butler, D. DeBoer, M.H. Wong, Peering through Jupiter’s clouds with radio spectral imaging. Science 352, 1198–1201 (2016). doi:10.1126/science.aaf2210
  * de Pater et al. (2018) I. de Pater, B. Butler, R.J. Sault, A. Moullet, C. Moeckel, J. Tollefson, K. de Kleer, M. Gurwell, S. Milam, Potential for Solar System Science with the ngVLA. Science with a Next Generation Very Large Array 517, 49 (2018)
  * de Pater et al. (2019a) I. de Pater, R.J. Sault, C. Moeckel, A. Moullet, M.H. Wong, C. Goullaud, D. DeBoer, B.J. Butler, G. Bjoraker, M. Ádámkovics, R. Cosentino, P.T. Donnelly, L.N. Fletcher, Y. Kasaba, G.S. Orton, J.H. Rogers, J.A. Sinclair, E. Villard, First ALMA Millimeter-wavelength Maps of Jupiter, with a Multiwavelength Study of Convection. Astronomical Journal 158(4), 139 (2019a). doi:10.3847/1538-3881/ab3643
  * de Pater et al. (2019b) I. de Pater, R.J. Sault, M.H. Wong, L.N. Fletcher, D. DeBoer, B. Butler, Jupiter’s ammonia distribution derived from VLA maps at 3-37 GHz. Icarus 322, 168–191 (2019b). doi:10.1016/j.icarus.2018.11.024
  * Denk et al. (in prep.) Denk et al., Io and the Minor Moons from JUICE. Space Science Reviews (in prep.)
  * Dinelli et al. (2017) B.M. Dinelli, F. Fabiano, A. Adriani, F. Altieri, M.L. Moriconi, A. Mura, G. Sindoni, G. Filacchione, F. Tosi, A. Migliorini, D. Grassi, G. Piccioni, R. Noschese, A. Cicchetti, S.J. Bolton, J.E.P. Connerney, S.K. Atreya, F. Bagenal, G.R. Gladstone, C.J. Hansen, W.S. Kurth, S.M. Levin, B.H. Mauk, D.J. McComas, J.-C. Gèrard, D. Turrini, S. Stefani, M. Amoroso, A. Olivieri, Preliminary JIRAM results from Juno polar observations: 1. Methodology and analysis applied to the Jovian northern polar region. Geophys. Res. Lett. 44(10), 4625–4632 (2017). doi:10.1002/2017GL072929
  * Drossart et al. (1989) P. Drossart, J.-P. Maillard, J. Caldwell, S.J. Kim, J.K.G. Watson, W.A. Majewski, J. Tennyson, S. Miller, S.K. Atreya, J.T. Clarke, J.H. Waite, R. Wagener, Detection of H3+ on Jupiter. Nature 340(6234), 539–541 (1989). doi:10.1038/340539a0
  * Duer et al. (2021) K. Duer, N. Gavriel, E. Galanti, Y. Kaspi, L.N. Fletcher, T. Guillot, S.J. Bolton, S.M. Levin, S.K. Atreya, D. Grassi, A.P. Ingersoll, C. Li, L. Li, J.I. Lunine, G.S. Orton, F.A. Oyafuso, J.H. Waite, Evidence for Multiple Ferrel-Like Cells on Jupiter. Geophys. Res. Lett. 48(23), 95651 (2021). doi:10.1029/2021GL095651
  * Dunn et al. (2017) W.R. Dunn, G. Branduardi-Raymont, L.C. Ray, C.M. Jackman, R.P. Kraft, R.F. Elsner, I.J. Rae, Z. Yao, M.F. Vogt, G.H. Jones, G.R. Gladstone, G.S. Orton, J.A. Sinclair, P.G. Ford, G.A. Graham, R. Caro-Carretero, A.J. Coates, The independent pulsations of Jupiter’s northern and southern X-ray auroras. Nature Astronomy 1, 758–764 (2017). doi:10.1038/s41550-017-0262-6
  * Dyudina et al. (2004) U.A. Dyudina, A.D. Del Genio, A.P. Ingersoll, C.C. Porco, R.A. West, A.R. Vasavada, J.M. Barbara, Lightning on Jupiter observed in the Hα line by the Cassini imaging science subsystem. Icarus 172(1), 24–36 (2004). doi:10.1016/j.icarus.2004.07.014
  * Dyudina et al. (2013) U.A. Dyudina, A.P. Ingersoll, S.P. Ewald, C.C. Porco, G. Fischer, Y. Yair, Saturn’s visible lightning, its radio emissions, and the structure of the 2009-2011 lightning storms. Icarus 226, 1020–1037 (2013). doi:10.1016/j.icarus.2013.07.013
  * Ebert et al. (2017) R.W. Ebert, F. Allegrini, F. Bagenal, S.J. Bolton, J.E.P. Connerney, G. Clark, G.A. DiBraccio, D.J. Gershman, W.S. Kurth, S. Levin, P. Louarn, B.H. Mauk, D.J. McComas, M. Reno, J.R. Szalay, M.F. Thomsen, P. Valek, S. Weidner, R.J. Wilson, Accelerated flows at Jupiter’s magnetopause: Evidence for magnetic reconnection along the dawn flank. Geophys. Res. Lett. 44(10), 4401–4409 (2017). doi:10.1002/2016GL072187
  * Edgington et al. (1998) S.G. Edgington, S.K. Atreya, L.M. Trafton, J.J. Caldwell, R.F. Beebe, A.A. Simon, R.A. West, C. Barnet, On the Latitude Variation of Ammonia, Acetylene, and Phosphine Altitude Profiles on Jupiter from HST Faint Object Spectrograph Observations. Icarus 133, 192–209 (1998). doi:10.1006/icar.1998.5925
  * Edgington et al. (1999) S.G. Edgington, S.K. Atreya, L.M. Trafton, J.J. Caldwell, R.F. Beebe, A.A. Simon, R.A. West, Ammonia and Eddy Mixing Variations in the Upper Troposphere of Jupiter from HST Faint Object Spectrograph Observations. Icarus 142, 342–356 (1999). doi:10.1006/icar.1999.6228
  * Encrenaz (2003) T. Encrenaz, ISO observations of the giant planets and Titan: what have we learnt? Planet. Space Sci. 51(2), 89–103 (2003). doi:10.1016/S0032-0633(02)00145-9
  * Feuchtgruber et al. (1997) H. Feuchtgruber, E. Lellouch, T. de Graauw, B. Bezard, T. Encrenaz, M. Griffin, External supply of oxygen to the atmospheres of giant planets. Nature 389, 159–162 (1997)
  * Flasar et al. (2004) F.M. Flasar, V.G. Kunde, R.K. Achterberg, B.J. Conrath, A.A. Simon-Miller, C.A. Nixon, P.J. Gierasch, P.N. Romani, B. Bézard, P. Irwin, G.L. Bjoraker, J.C. Brasunas, D.E. Jennings, J.C. Pearl, M.D. Smith, G.S. Orton, L.J. Spilker, R. Carlson, S.B. Calcutt, P.L. Read, F.W. Taylor, P. Parrish, A. Barucci, R. Courtin, A. Coustenis, D. Gautier, E. Lellouch, A. Marten, R. Prangé, Y. Biraud, T. Fouchet, C. Ferrari, T.C. Owen, M.M. Abbas, R.E. Samuelson, F. Raulin, P. Ade, C.J. Césarsky, K.U. Grossman, A. Coradini, An intense stratospheric jet on Jupiter. Nature 427, 132–135 (2004)
  * Fletcher (2017) L.N. Fletcher, Cycles of activity in the Jovian atmosphere. Geophys. Res. Lett. 44, 4725–4729 (2017). doi:10.1002/2017GL073806
  * Fletcher et al. (2009) L.N. Fletcher, G.S. Orton, N.A. Teanby, P.G.J. Irwin, Phosphine on Jupiter and Saturn from Cassini/CIRS. Icarus 202, 543–564 (2009). doi:10.1016/j.icarus.2009.03.023
  * Fletcher et al. (2010) L.N. Fletcher, G.S. Orton, O. Mousis, P. Yanamandra-Fisher, P.D. Parrish, P.G.J. Irwin, B.M. Fisher, L. Vanzi, T. Fujiyoshi, T. Fuse, A.A. Simon-Miller, E. Edkins, T.L. Hayward, J. De Buizer, Thermal structure and composition of Jupiter’s Great Red Spot from high-resolution thermal imaging. Icarus 208, 306–328 (2010). doi:10.1016/j.icarus.2010.01.005
  * Fletcher et al. (2011) L.N. Fletcher, K.H. Baines, T.W. Momary, A.P. Showman, P.G.J. Irwin, G.S. Orton, M. Roos-Serote, C. Merlet, Saturn’s tropospheric composition and clouds from Cassini/VIMS 4.6-5.1 $\mu$m nightside spectroscopy. Icarus 214, 510–533 (2011). doi:10.1016/j.icarus.2011.06.006
  * Fletcher et al. (2016) L.N. Fletcher, T.K. Greathouse, G.S. Orton, J.A. Sinclair, R.S. Giles, P.G.J. Irwin, T. Encrenaz, Mid-infrared mapping of Jupiter’s temperatures, aerosol opacity and chemical distributions with IRTF/TEXES. Icarus 278, 128–161 (2016). doi:10.1016/j.icarus.2016.06.008
  * Fletcher et al. (2017a) L.N. Fletcher, G.S. Orton, J.A. Sinclair, P. Donnelly, H. Melin, J.H. Rogers, T.K. Greathouse, Y. Kasaba, T. Fujiyoshi, T.M. Sato, J. Fernandes, P.G.J. Irwin, R.S. Giles, A.A. Simon, M.H. Wong, M. Vedovato, Jupiter’s North Equatorial Belt expansion and thermal wave activity ahead of Juno’s arrival. Geophys. Res. Lett. 44, 7140–7148 (2017a). doi:10.1002/2017GL073383
  * Fletcher et al. (2017b) L.N. Fletcher, I. de Pater, W.T. Reach, M. Wong, G.S. Orton, P.G.J. Irwin, R.D. Gehrz, Jupiter’s para-H2 distribution from SOFIA/FORCAST and Voyager/IRIS 17-37 $\mu$m spectroscopy. Icarus 286, 223–240 (2017b). doi:10.1016/j.icarus.2016.10.002
  * Fletcher et al. (2017c) L.N. Fletcher, G.S. Orton, J.H. Rogers, R.S. Giles, A.V. Payne, P.G.J. Irwin, M. Vedovato, Moist convection and the 2010-2011 revival of Jupiter’s South Equatorial Belt. Icarus 286, 94–117 (2017c). doi:10.1016/j.icarus.2017.01.001
  * Fletcher et al. (2018) L.N. Fletcher, H. Melin, A. Adriani, A.A. Simon, A. Sanchez-Lavega, P.T. Donnelly, A. Antuñano, G.S. Orton, R. Hueso, M.L. Moriconi, F. Altieri, G. Sindoni, Jupiter’s Mesoscale Waves Observed at 5 $\mu$m by Ground-Based Observations and Juno JIRAM. ApJ, submitted (2018)
  * Fletcher et al. (2021) L.N. Fletcher, F.A. Oyafuso, M. Allison, A. Ingersoll, L. Li, Y. Kaspi, E. Galanti, M.H. Wong, G.S. Orton, K. Duer, Z. Zhang, C. Li, T. Guillot, S.M. Levin, S. Bolton, Jupiter’s Temperate Belt/Zone Contrasts Revealed at Depth by Juno Microwave Observations. Journal of Geophysical Research (Planets) 126(10), 06858 (2021). doi:10.1029/2021JE006858
  * Fletcher et al. (2020) L.N. Fletcher, Y. Kaspi, T. Guillot, A.P. Showman, How Well Do We Understand the Belt/Zone Circulation of Giant Planet Atmospheres? Space Science Reviews 216(2), 30 (2020). doi:10.1007/s11214-019-0631-9
  * Friedson (1999) A.J. Friedson, New Observations and Modelling of a QBO-Like Oscillation in Jupiter’s Stratosphere. Icarus 137, 34–55 (1999). doi:10.1006/icar.1998.6038
  * Friedson et al. (2002a) A.J. Friedson, A.-S. Wong, Y.L. Yung, Models for polar haze formation in Jupiter’s stratosphere. Icarus 158, 389–400 (2002a)
  * Friedson et al. (2002b) A.J. Friedson, A.-S. Wong, Y.L. Yung, Models for Polar Haze Formation in Jupiter’s Stratosphere. Icarus 158(2), 389–400 (2002b). doi:10.1006/icar.2002.6885
  * García-Melendo and Sánchez-Lavega (2001) E. García-Melendo, A. Sánchez-Lavega, A Study of the Stability of Jovian Zonal Winds from HST Images: 1995-2000. Icarus 152, 316–330 (2001). doi:10.1006/icar.2001.6646
  * Gavriel and Kaspi (2021) N. Gavriel, Y. Kaspi, The number and location of Jupiter’s circumpolar cyclones explained by vorticity dynamics. Nature Geoscience 14(8), 559–563 (2021). doi:10.1038/s41561-021-00781-6
  * Gérard et al. (2018) J.-C. Gérard, A. Mura, B. Bonfond, G.R. Gladstone, A. Adriani, V. Hue, B.M. Dinelli, T.K. Greathouse, D. Grodent, F. Altieri, M.L. Moriconi, A. Radioti, J.E.P. Connerney, S.J. Bolton, S.M. Levin, Concurrent ultraviolet and infrared observations of the north Jovian aurora during Juno’s first perijove. Icarus 312, 145–156 (2018). doi:10.1016/j.icarus.2018.04.020
  * Gérard et al. (2023) J.-C. Gérard, L. Gkouvelis, B. Bonfond, G.R. Gladstone, A. Mura, A. Adriani, D. Grodent, V. Hue, T.K. Greathouse, H3+ cooling in the jovian aurora: Juno remote sensing observations and modeling. Icarus 389, 115261 (2023). doi:10.1016/j.icarus.2022.115261
  * Gierasch et al. (1986) P.J. Gierasch, J.A. Magalhaes, B.J. Conrath, Zonal mean properties of Jupiter’s upper troposphere from Voyager infrared observations. Icarus 67, 456–483 (1986). doi:10.1016/0019-1035(86)90125-9
  * Gierasch et al. (2000) P.J. Gierasch, A.P. Ingersoll, D. Banfield, S.P. Ewald, P. Helfenstein, A. Simon-Miller, A. Vasavada, H.H. Breneman, D.A. Senske, Galileo Imaging Team, Observation of moist convection in Jupiter’s atmosphere. Nature 403, 628–630 (2000). doi:10.1038/35001017
  * Giles et al. (2017) R.S. Giles, L.N. Fletcher, P.G.J. Irwin, Latitudinal variability in Jupiter’s tropospheric disequilibrium species: GeH4, AsH3 and PH3. Icarus 289, 254–269 (2017). doi:10.1016/j.icarus.2016.10.023
  * Giles et al. (2020a) R.S. Giles, T.K. Greathouse, R.G. Cosentino, G.S. Orton, J.H. Lacy, Vertically-resolved observations of Jupiter’s quasi-quadrennial oscillation from 2012 to 2019. Icarus 350, 113905 (2020a). doi:10.1016/j.icarus.2020.113905
  * Giles et al. (2020b) R.S. Giles, T.K. Greathouse, B. Bonfond, G.R. Gladstone, J.A. Kammer, V. Hue, D.C. Grodent, J.-C. Gérard, M.H. Versteeg, M.H. Wong, S.J. Bolton, J.E.P. Connerney, S.M. Levin, Possible Transient Luminous Events Observed in Jupiter’s Upper Atmosphere. Journal of Geophysical Research (Planets) 125(11), 06659 (2020b). doi:10.1029/2020JE006659
  * Giles et al. (2021a) R.S. Giles, T.K. Greathouse, J.A. Kammer, G.R. Gladstone, B. Bonfond, V. Hue, D.C. Grodent, J.-C. Gérard, M.H. Versteeg, S.J. Bolton, J.E.P. Connerney, S.M. Levin, Detection of a Bolide in Jupiter’s Atmosphere With Juno UVS. Geophys. Res. Lett. 48(5), 91797 (2021a). doi:10.1029/2020GL091797
  * Giles et al. (2021b) R.S. Giles, T.K. Greathouse, V. Hue, G.R. Gladstone, H. Melin, L.N. Fletcher, P.G.J. Irwin, J.A. Kammer, M.H. Versteeg, B. Bonfond, D.C. Grodent, S.J. Bolton, S.M. Levin, Meridional Variations of C2H2 in Jupiter’s Stratosphere From Juno UVS Observations. Journal of Geophysical Research (Planets) 126(8), 06928 (2021b). doi:10.1029/2021JE006928
  * Giles et al. (2023) R.S. Giles, V. Hue, T.K. Greathouse, G.R. Gladstone, J.A. Kammer, M.H. Versteeg, B. Bonfond, D.C. Grodent, J.-C. Gérard, J.A. Sinclair, S.J. Bolton, S.M. Levin, Enhanced C2H2 Absorption Within Jupiter’s Southern Auroral Oval From Juno UVS Observations. Journal of Geophysical Research (Planets) 128(2), 2022–007610 (2023). doi:10.1029/2022JE007610
  * Girard et al. (2016) J.N. Girard, P. Zarka, C. Tasse, S. Hess, I. de Pater, D. Santos-Costa, Q. Nenon, A. Sicard, S. Bourdarie, J. Anderson, A. Asgekar, M.E. Bell, I. van Bemmel, M.J. Bentum, G. Bernardi, P. Best, A. Bonafede, F. Breitling, R.P. Breton, J.W. Broderick, W.N. Brouw, M. Brüggen, B. Ciardi, S. Corbel, A. Corstanje, F. de Gasperin, E. de Geus, A. Deller, S. Duscha, J. Eislöffel, H. Falcke, W. Frieswijk, M.A. Garrett, J. Grießmeier, A.W. Gunst, J.W.T. Hessels, M. Hoeft, J. Hörandel, M. Iacobelli, E. Juette, V.I. Kondratiev, M. Kuniyoshi, G. Kuper, J. van Leeuwen, M. Loose, P. Maat, G. Mann, S. Markoff, R. McFadden, D. McKay-Bukowski, J. Moldon, H. Munk, A. Nelles, M.J. Norden, E. Orru, H. Paas, M. Pandey-Pommier, R. Pizzo, A.G. Polatidis, W. Reich, H. Röttgering, A. Rowlinson, D. Schwarz, O. Smirnov, M. Steinmetz, J. Swinbank, M. Tagger, S. Thoudam, M.C. Toribio, R. Vermeulen, C. Vocks, R.J. van Weeren, R.A.M.J. Wijers, O. Wucknitz, Imaging Jupiter’s radiation belts down to 127 MHz with LOFAR. Astron. Astrophys. 587, 3 (2016). doi:10.1051/0004-6361/201527518
  * Gladstone and Yung (1983) G.R. Gladstone, Y.L. Yung, An analysis of the reflection spectrum of Jupiter from 1500 A to 1740 A. Astrophys. J. 266, 415–424 (1983). doi:10.1086/160789
  * Gladstone et al. (in prep.) Gladstone et al., The UVS Instrument for JUICE. Space Science Reviews (in prep.)
  * Grasset et al. (2013) O. Grasset, M.K. Dougherty, A. Coustenis, E.J. Bunce, C. Erd, D. Titov, M. Blanc, A. Coates, P. Drossart, L.N. Fletcher, H. Hussmann, R. Jaumann, N. Krupp, J.-P. Lebreton, O. Prieto-Ballesteros, P. Tortora, F. Tosi, T. Van Hoolst, JUpiter ICy moons Explorer (JUICE): An ESA mission to orbit Ganymede and to characterise the Jupiter system. Planet. Space Sci. 78, 1–21 (2013). doi:10.1016/j.pss.2012.12.002
  * Grassi et al. (2010) D. Grassi, A. Adriani, M.L. Moriconi, N.I. Ignatiev, E. D’Aversa, F. Colosimo, A. Negrão, L. Brower, B.M. Dinelli, A. Coradini, G. Piccioni, Jupiter’s hot spots: Quantitative assessment of the retrieval capabilities of future IR spectro-imagers. Plan. & Space Sci. 58(10), 1265–1278 (2010). doi:10.1016/j.pss.2010.05.003
  * Grassi et al. (2017) D. Grassi, A. Adriani, A. Mura, B.M. Dinelli, G. Sindoni, D. Turrini, G. Filacchione, A. Migliorini, M.L. Moriconi, F. Tosi, R. Noschese, A. Cicchetti, F. Altieri, F. Fabiano, G. Piccioni, S. Stefani, S. Atreya, J. Lunine, G. Orton, A. Ingersoll, S. Bolton, S. Levin, J. Connerney, A. Olivieri, M. Amoroso, Preliminary results on the composition of Jupiter’s troposphere in hot spot regions from the JIRAM/Juno instrument. Geophys. Res. Lett. 44, 4615–4624 (2017). doi:10.1002/2017GL072841
  * Grassi et al. (2020) D. Grassi, A. Adriani, A. Mura, S.K. Atreya, L.N. Fletcher, J.I. Lunine, G.S. Orton, S. Bolton, C. Plainaki, G. Sindoni, F. Altieri, A. Cicchetti, B.M. Dinelli, G. Filacchione, A. Migliorini, M.L. Moriconi, R. Noschese, A. Olivieri, G. Piccioni, R. Sordini, S. Stefani, F. Tosi, D. Turrini, On the Spatial Distribution of Minor Species in Jupiter’s Troposphere as Inferred From Juno JIRAM Data. Journal of Geophysical Research (Planets) 125(4), 06206 (2020). doi:10.1029/2019JE006206
  * Grassi et al. (2021) D. Grassi, A. Mura, G. Sindoni, A. Adriani, S.K. Atreya, G. Filacchione, L.N. Fletcher, J.I. Lunine, M.L. Moriconi, R. Noschese, G.S. Orton, C. Plainaki, R. Sordini, F. Tosi, D. Turrini, A. Olivieri, G. Eichstädt, C.J. Hansen, H. Melin, F. Altieri, A. Cicchetti, B.M. Dinelli, A. Migliorini, G. Piccioni, S. Stefani, S.J. Bolton, On the clouds and ammonia in Jupiter’s upper troposphere from Juno JIRAM reflectivity observations. Mon. Not. R. Astron. Soc. 503(4), 4892–4907 (2021). doi:10.1093/mnras/stab740
  * Greathouse et al. (2010) T. Greathouse, J. Moses, L. Fletcher, G. Orton, S. Guerlet, Seasonal Temperature Variations in Saturn’s Stratosphere: Radiative Seasonal Model vs. Observations., in EGU General Assembly Conference Abstracts. EGU General Assembly Conference Abstracts, vol. 12, 2010, p. 4806
  * Greathouse et al. (2021) T. Greathouse, R. Gladstone, M. Versteeg, V. Hue, J. Kammer, R. Giles, M. Davis, S. Bolton, S. Levin, J. Connerney, J.-C. Gérard, D. Grodent, B. Bonfond, E. Bunce, M.F. Vogt, Local Time Dependence of Jupiter’s Polar Auroral Emissions Observed by Juno UVS. Journal of Geophysical Research (Planets) 126(12), 06954 (2021). doi:10.1029/2021JE006954
  * Griffith et al. (2004) C.A. Griffith, B. Bézard, T. Greathouse, E. Lellouch, J. Lacy, D. Kelly, M.J. Richter, Meridional transport of HCN from SL9 impacts on Jupiter. Icarus 170, 58–69 (2004). doi:10.1016/j.icarus.2004.02.006
  * Grodent et al. (2003) D. Grodent, J.T. Clarke, J.H. Waite, S.W.H. Cowley, J.-C. GéRard, J. Kim, Jupiter’s polar auroral emissions. Journal of Geophysical Research (Space Physics) 108(A10), 1366 (2003). doi:10.1029/2003JA010017
  * Grodent (2015) D. Grodent, A Brief Review of Ultraviolet Auroral Emissions on Giant Planets. Space Science Reviews 187(1-4), 23–50 (2015). doi:10.1007/s11214-014-0052-8
  * Grodent et al. (2008) D. Grodent, B. Bonfond, J.-C. GéRard, A. Radioti, J. Gustin, J.T. Clarke, J. Nichols, J.E.P. Connerney, Auroral evidence of a localized magnetic anomaly in Jupiter’s northern hemisphere. Journal of Geophysical Research (Space Physics) 113(A9), 09201 (2008). doi:10.1029/2008JA013185
  * Guerlet et al. (2020a) S. Guerlet, A. Spiga, H. Delattre, T. Fouchet, Radiative-equilibrium model of Jupiter’s atmosphere and application to estimating stratospheric circulations. Icarus 351, 113935 (2020a). doi:10.1016/j.icarus.2020.113935
  * Guerlet et al. (2020b) S. Guerlet, A. Spiga, H. Delattre, T. Fouchet, Radiative-equilibrium model of Jupiter’s atmosphere and application to estimating stratospheric circulations. Icarus 351, 113935 (2020b). doi:10.1016/j.icarus.2020.113935
  * Guillot (1995) T. Guillot, Condensation of Methane, Ammonia, and Water and the Inhibition of Convection in Giant Planets. Science 269, 1697–1699 (1995). doi:10.1126/science.7569896
  * Guillot et al. (2018) T. Guillot, Y. Miguel, B. Militzer, W.B. Hubbard, Y. Kaspi, E. Galanti, H. Cao, R. Helled, S.M. Wahl, L. Iess, W.M. Folkner, D.J. Stevenson, J.I. Lunine, D.R. Reese, A. Biekman, M. Parisi, D. Durante, J.E.P. Connerney, S.M. Levin, S.J. Bolton, A suppression of differential rotation in Jupiter’s deep interior. Nature 555, 227–230 (2018). doi:10.1038/nature25775
  * Guillot et al. (2004) T. Guillot, D.J. Stevenson, W.B. Hubbard, D. Saumon, The Interior of Jupiter, ed. by F. Bagenal, T.E. Dowling, W.B. McKinnon, vol. 1 (Jupiter. The Planet, Satellites and Magnetosphere, 2004), pp. 35–57
  * Guillot et al. (2020a) T. Guillot, D.J. Stevenson, S.K. Atreya, S.J. Bolton, H.N. Becker, Storms and the Depletion of Ammonia in Jupiter: I. Microphysics of “Mushballs”. Journal of Geophysical Research (Planets) 125(8), 06403 (2020a). doi:10.1029/2020JE006403
  * Guillot et al. (2020b) T. Guillot, C. Li, S.J. Bolton, S.T. Brown, A.P. Ingersoll, M.A. Janssen, S.M. Levin, J.I. Lunine, G.S. Orton, P.G. Steffes, D.J. Stevenson, Storms and the Depletion of Ammonia in Jupiter: II. Explaining the Juno Observations. Journal of Geophysical Research (Planets) 125(8), 06404 (2020b). doi:10.1029/2020JE006404
  * Gupta et al. (2022) P. Gupta, S.K. Atreya, P.G. Steffes, L.N. Fletcher, T. Guillot, M.D. Allison, S.J. Bolton, R. Helled, S. Levin, C. Li, J.I. Lunine, Y. Miguel, G.S. Orton, J. Hunter Waite, P. Withers, Jupiter’s Temperature Structure: A Reassessment of the Voyager Radio Occultation Measurements. Plan. Sci. J. 3(7), 159 (2022). doi:10.3847/PSJ/ac6956
  * Gurnett et al. (1979) D.A. Gurnett, R.R. Shaw, R.R. Anderson, W.S. Kurth, F.L. Scarf, Whistlers observed by Voyager 1: Detection of lightning on Jupiter. Geophys. Res. Lett. 6(6), 511–514 (1979). doi:10.1029/GL006i006p00511
  * Gurvits et al. (in prep.) Gurvits et al., The PRIDE experiment for JUICE. Space Science Reviews (in prep.)
  * Hammel et al. (2010) H.B. Hammel, M.H. Wong, J.T. Clarke, I. de Pater, L.N. Fletcher, R. Hueso, K. Noll, G.S. Orton, S. Pérez-Hoyos, A. Sánchez-Lavega, A.A. Simon-Miller, P.A. Yanamandra-Fisher, Jupiter after the 2009 Impact: Hubble Space Telescope Imaging of the Impact-generated Debris and its Temporal Evolution. ApJ 715(2), 150–154 (2010)
  * Hansen et al. (2017a) C.J. Hansen, M.A. Caplinger, A. Ingersoll, M.A. Ravine, E. Jensen, S. Bolton, G. Orton, Junocam: Juno’s Outreach Camera. Space Science Reviews 213(1-4), 475–506 (2017a). doi:10.1007/s11214-014-0079-x
  * Hansen et al. (2017b) C.J. Hansen, M.A. Caplinger, A. Ingersoll, M.A. Ravine, E. Jensen, S. Bolton, G. Orton, Junocam: Juno’s Outreach Camera. Space Sci. Rev. 213(1-4), 475–506 (2017b). doi:10.1007/s11214-014-0079-x
  * Harrington et al. (2004) J. Harrington, I. de Pater, S.H. Brecht, D. Deming, V. Meadows, K. Zahnle, P.D. Nicholson, Lessons from Shoemaker-Levy 9 about Jupiter and planetary impacts (Cambridge Planetary Science. Cambridge Univ. Press, New York, ???, 2004), pp. 159–184. Chap. 8
  * Hartogh et al. (2011) P. Hartogh, E. Lellouch, R. Moreno, D. Bockelée-Morvan, N. Biver, T. Cassidy, M. Rengel, C. Jarchow, T. Cavalié, J. Crovisier, F.P. Helmich, M. Kidger, Direct detection of the Enceladus water torus with Herschel. Astron. Astrophys. 532, 2 (2011). doi:10.1051/0004-6361/201117377
  * Hartogh et al. (in prep.) Hartogh et al., The SWI Instrument for JUICE. Space Science Reviews (in prep.)
  * Holton (2004) J.R. Holton, An Introduction to Dynamic Meteorology (Academic press, ???, 2004). ISBN 0123540151
  * Hue et al. (2018a) V. Hue, F. Hersant, T. Cavalié, M. Dobrijevic, J.A. Sinclair, Photochemistry, mixing and transport in Jupiter’s stratosphere constrained by Cassini. Icarus 307, 106–123 (2018a). doi:10.1016/j.icarus.2018.02.018
  * Hue et al. (2018b) V. Hue, F. Hersant, T. Cavalié, M. Dobrijevic, J.A. Sinclair, Photochemistry, mixing and transport in Jupiter’s stratosphere constrained by Cassini. Icarus 307, 106–123 (2018b). doi:10.1016/j.icarus.2018.02.018
  * Hueso et al. (2002) R. Hueso, A. Sánchez-Lavega, T. Guillot, A model for large-scale convective storms in Jupiter. Journal of Geophysical Research (Planets) 107, 5–1 (2002). doi:10.1029/2001JE001839
  * Hueso et al. (2010) R. Hueso, A. Wesley, C. Go, S. Pérez-Hoyos, M.H. Wong, L.N. Fletcher, A. Sánchez-Lavega, M.B.E. Boslough, I. de Pater, G.S. Orton, A.A. Simon-Miller, S.G. Djorgovski, M.L. Edwards, H.B. Hammel, J.T. Clarke, K.S. Noll, P.A. Yanamandra-Fisher, First Earth-based Detection of a Superbolide on Jupiter. Astrophys. J. Lett. 721(2), 129–133 (2010). doi:10.1088/2041-8205/721/2/L129
  * Hueso et al. (2013) R. Hueso, S. Pérez-Hoyos, A. Sánchez-Lavega, A. Wesley, G. Hall, C. Go, M. Tachikawa, K. Aoki, M. Ichimaru, J.W.T. Pond, D.G. Korycansky, C. Palotai, G. Chappell, N. Rebeli, J. Harrington, M. Delcroix, M. Wong, I. de Pater, L.N. Fletcher, H. Hammel, G.S. Orton, I. Tabe, J. Watanabe, J.C. Moreno, Impact flux on Jupiter: From superbolides to large-scale collisions. Astron. Astrophys. 560, 55 (2013). doi:10.1051/0004-6361/201322216
  * Hueso et al. (2017) R. Hueso, A. Sánchez-Lavega, P. Iñurrigarro, J.F. Rojas, S. Pérez-Hoyos, I. Mendikoa, J.M. Gómez-Forrellad, C. Go, D. Peach, F. Colas, M. Vedovato, Jupiter cloud morphology and zonal winds from ground-based observations before and during Juno’s first perijove. Geophys. Res. Lett. 44, 4669–4678 (2017). doi:10.1002/2017GL073444
  * Hueso et al. (2018a) R. Hueso, M. Delcroix, A. Sánchez-Lavega, S. Pedranghelu, G. Kernbauer, J. McKeon, A. Fleckstein, A. Wesley, J.M. Gómez-Forrellad, J.F. Rojas, J. Juaristi, Small impacts on the giant planet Jupiter. Astron. Astrophys. 617, 68 (2018a). doi:10.1051/0004-6361/201832689
  * Hueso et al. (2018b) R. Hueso, J. Juaristi, J. Legarreta, A. Sánchez-Lavega, J.F. Rojas, S. Erard, B. Cecconi, P. Le Sidaner, The Planetary Virtual Observatory and Laboratory (PVOL) and its integration into the Virtual European Solar and Planetary Access (VESPA). Plan. & Space Sci. 150, 22–35 (2018b). doi:10.1016/j.pss.2017.03.014
  * Hueso et al. (2022) R. Hueso, P. Iñurrigarro, A. Sánchez-Lavega, C.R. Foster, J.H. Rogers, G.S. Orton, C. Hansen, G. Eichstädt, I. Ordonez-Etxeberria, J.F. Rojas, S.R. Brueshaber, J.F. Sanz-Requena, S. Pérez-Hoyos, M.H. Wong, T.W. Momary, B. Jónsson, A. Antuñano, K.H. Baines, E.K. Dahl, S. Mizumoto, C. Go, A. Anguiano-Arteaga, Convective storms in closed cyclones in Jupiter’s South Temperate Belt: (I) observations. Icarus 380, 114994 (2022). doi:10.1016/j.icarus.2022.114994
  * Iess et al. (2018) L. Iess, W.M. Folkner, D. Durante, M. Parisi, Y. Kaspi, E. Galanti, T. Guillot, W.B. Hubbard, D.J. Stevenson, J.D. Anderson, D.R. Buccino, L.G. Casajus, A. Milani, R. Park, P. Racioppa, D. Serra, P. Tortora, M. Zannoni, H. Cao, R. Helled, J.I. Lunine, Y. Miguel, B. Militzer, S. Wahl, J.E.P. Connerney, S.M. Levin, S.J. Bolton, Measurement of Jupiter’s asymmetric gravity field. Nature 555(7695), 220–222 (2018). doi:10.1038/nature25776
  * Iess et al. (in prep.) Iess et al., The 3GM Instrument for JUICE. Space Science Reviews (in prep.)
  * Imai et al. (2019) M. Imai, I. Kolmašová, W.S. Kurth, O. Santolík, G.B. Hospodarsky, D.A. Gurnett, S.T. Brown, S.J. Bolton, J.E.P. Connerney, S.M. Levin, Evidence for low density holes in Jupiter’s ionosphere. Nature Communications 10, 2751 (2019). doi:10.1038/s41467-019-10708-w
  * Ingersoll et al. (2000) A.P. Ingersoll, G.P. J., B. D., A.R. Vasavada, Galileo Imaging Team, Moist convection as an energy source for the large-scale motions in Jupiter’s atmosphere. Nature 403, 630–632 (2000). doi:10.1038/35001021
  * Ingersoll et al. (2004) A.P. Ingersoll, T.E. Dowling, P.J. Gierasch, G.S. Orton, P.L. Read, A. Sánchez-Lavega, A.P. Showman, A.A. Simon-Miller, A.R. Vasavada, Dynamics of Jupiter’s atmosphere, ed. by F. Bagenal, T.E. Dowling, W.B. McKinnon (Jupiter. The Planet, Satellites and Magnetosphere, 2004), pp. 105–128
  * Ingersoll et al. (2017) A.P. Ingersoll, V. Adumitroaie, M.D. Allison, S. Atreya, A.A. Bellotti, S.J. Bolton, S.T. Brown, S. Gulkis, M.A. Janssen, S.M. Levin, C. Li, L. Li, J.I. Lunine, G.S. Orton, F.A. Oyafuso, P.G. Steffes, Implications of the ammonia distribution on Jupiter from 1 to 100 bars as measured by the Juno microwave radiometer. Geophys. Res. Lett. 44, 7676–7685 (2017). doi:10.1002/2017GL074277
  * Irwin et al. (1998) P.G.J. Irwin, A.L. Weir, S.E. Smith, F.W. Taylor, A.L. Lambert, S.B. Calcutt, P.J. Cameron-Smith, R.W. Carlson, K. Baines, G.S. Orton, P. Drossart, T. Encrenaz, M. Roos-Serote, Cloud structure and atmospheric composition of Jupiter retrieved from Galileo near-infrared mapping spectrometer real-time spectra. J. Geophys. Res. 103(12), 23001–23022 (1998). doi:10.1029/98JE00948
  * Johnson et al. (2017) R.E. Johnson, T.S. Stallard, H. Melin, J.D. Nichols, S.W.H. Cowley, Jupiter’s polar ionospheric flows: High resolution mapping of spectral intensity and line-of-sight velocity of H${}_{3}^{+}$ ions. J. Geophys. Res. 122(7), 7599–7618 (2017). doi:10.1002/2017JA024176
  * Karkoschka (1994) E. Karkoschka, Spectrophotometry of the Jovian Planets and Titan at 300- to 1000-nm Wavelength: The Methane Spectrum. Icarus 111(1), 174–192 (1994). doi:10.1006/icar.1994.1139
  * Kaspi et al. (2018) Y. Kaspi, E. Galanti, W.B. Hubbard, D.J. Stevenson, S.J. Bolton, L. Iess, T. Guillot, J. Bloxham, J.E.P. Connerney, H. Cao, D. Durante, W.M. Folkner, R. Helled, A.P. Ingersoll, S.M. Levin, J.I. Lunine, Y. Miguel, B. Militzer, M. Parisi, S.M. Wahl, Jupiter’s atmospheric jet streams extend thousands of kilometres deep. Nature 555, 223–226 (2018). doi:10.1038/nature25793
  * Kaspi et al. (2020) Y. Kaspi, E. Galanti, A.P. Showman, D.J. Stevenson, T. Guillot, L. Iess, S.J. Bolton, Comparison of the Deep Atmospheric Dynamics of Jupiter and Saturn in Light of the Juno and Cassini Gravity Measurements. Space Sci. Rev. 216(5), 84 (2020). doi:10.1007/s11214-020-00705-7
  * Kaye and Strobel (1984) J.A. Kaye, D.F. Strobel, Phosphine photochemistry in the atmosphere of Saturn. Icarus 59, 314–335 (1984). doi:10.1016/0019-1035(84)90105-2
  * Kolmašová et al. (2018) I. Kolmašová, M. Imai, O. Santolík, W.S. Kurth, G.B. Hospodarsky, D.A. Gurnett, J.E.P. Connerney, S.J. Bolton, Discovery of rapid whistlers close to Jupiter implying lightning rates similar to those on Earth. Nature Astronomy 2, 544–548 (2018). doi:10.1038/s41550-018-0442-z
  * Koskinen et al. (2015) T.T. Koskinen, B.R. Sandel, R.V. Yelle, D.F. Strobel, I.C.F. Müller-Wodarg, J.T. Erwin, Saturn’s variable thermosphere from Cassini/UVIS occultations. Icarus 260, 174–189 (2015). doi:10.1016/j.icarus.2015.07.008
  * Kurth et al. (1985) W.S. Kurth, B.D. Strayer, D.A. Gurnett, F.L. Scarf, A summary of whistlers observed by Voyager 1 at Jupiter. Icarus 61(3), 497–507 (1985). doi:10.1016/0019-1035(85)90138-1
  * Kurth et al. (2018) W.S. Kurth, B.H. Mauk, S.S. Elliott, D.A. Gurnett, G.B. Hospodarsky, O. Santolik, J.E.P. Connerney, P. Valek, F. Allegrini, G.R. Gladstone, S.J. Bolton, S.M. Levin, Whistler Mode Waves Associated With Broadband Auroral Electron Precipitation at Jupiter. Geophys. Res. Lett. 45(18), 9372–9379 (2018). doi:10.1029/2018GL078566
  * Laraia et al. (2013) A.L. Laraia, A.P. Ingersoll, M.A. Janssen, S. Gulkis, F. Oyafuso, M. Allison, Analysis of Saturn’s thermal emission at 2.2-cm wavelength: Spatial distribution of ammonia vapor. Icarus 226, 641–654 (2013). doi:10.1016/j.icarus.2013.06.017
  * Leconte et al. (2017) J. Leconte, F. Selsis, F. Hersant, T. Guillot, Condensation-inhibited convection in hydrogen-rich atmospheres . Stability against double-diffusive processes and thermal profiles for Jupiter, Saturn, Uranus, and Neptune. Astron. Astrophys. 598, 98 (2017). doi:10.1051/0004-6361/201629140
  * Lellouch et al. (2005) E. Lellouch, R. Moreno, G. Paubert, A dual origin for Neptune’s carbon monoxide? Astron. Astrophys. 430, 37–40 (2005). doi:10.1051/0004-6361:200400127
  * Lellouch et al. (1995a) E. Lellouch, G. Paubert, R. Moreno, M.C. Festou, B. Bézard, D. Bockelée-Morvan, P. Colom, J. Crovisier, T. Encrenaz, D. Gautier, A. Marten, D. Despois, D.F. Strobel, A. Sievers, Chemical and thermal response of Jupiter’s atmosphere following the impact of comet Shoemaker-Levy 9. Nature 373, 592–595 (1995a). doi:10.1038/373592a0
  * Lellouch et al. (1995b) E. Lellouch, G. Paubert, R. Moreno, M.C. Festou, B. Bezard, D. Bockelee-Morvan, P. Colom, J. Crovisier, T. Encrenaz, D. Gautier, A. Marten, D. Despois, D.F. Strobel, A. Sievers, The collision of Comet P/Shoemaker-Levy 9 with Jupiter: Detection and monitoring of CO, CS and OCS. Highlights of Astronomy 10, 648 (1995b)
  * Lellouch et al. (2001a) E. Lellouch, B. Bézard, T. Fouchet, H. Feuchtgruber, T. Encrenaz, T. de Graauw, The deuterium abundance in Jupiter and Saturn from ISO-SWS observations. Astron. Astrophys. 370, 610–622 (2001a). doi:10.1051/0004-6361:20010259
  * Lellouch et al. (2001b) E. Lellouch, B. Bézard, T. Fouchet, H. Feuchtgruber, T. Encrenaz, T. de Graauw, The deuterium abundance in Jupiter and Saturn from ISO-SWS observations. Astron. Astrophys. 370, 610–622 (2001b). doi:10.1051/0004-6361:20010259
  * Lellouch et al. (2002) E. Lellouch, B. Bézard, J.I. Moses, G.R. Davis, P. Drossart, H. Feuchtgruber, E.A. Bergin, R. Moreno, T. Encrenaz, The Origin of Water Vapor and Carbon Dioxide in Jupiter’s Stratosphere. Icarus 159, 112–131 (2002). doi:10.1006/icar.2002.6929
  * Lellouch et al. (2006) E. Lellouch, B. Bézard, D.F. Strobel, G.L. Bjoraker, F.M. Flasar, P.N. Romani, On the HCN and CO 2 abundance and distribution in Jupiter’s stratosphere. Icarus 184(2), 478–497 (2006). doi:10.1016/j.icarus.2006.05.018
  * Lemasquerier et al. (2020) D. Lemasquerier, G. Facchini, B. Favier, M. Le Bars, Remote determination of the shape of Jupiter’s vortices from laboratory experiments. Nature Physics 16(6), 695–700 (2020). doi:10.1038/s41567-020-0833-9
  * Leovy et al. (1991a) C.B. Leovy, A.J. Friedson, G.S. Orton, The quasiquadrennial oscillation of Jupiter’s equatorial stratosphere. Nature 354, 380–382 (1991a). doi:10.1038/354380a0
  * Leovy et al. (1991b) C.B. Leovy, A.J. Friedson, G.S. Orton, The quasiquadrennial oscillation of Jupiter’s equatorial stratosphere. Nature 354(6352), 380–382 (1991b). doi:10.1038/354380a0
  * Levine et al. (1977) J.S. Levine, D.R. Kraemer, W.R. Kuhn, Solar Radiation Incident on Mars and the Outer Planets: Latitudinal, Seasonal, and Atmospheric Effects. Icarus 31(1), 136–145 (1977). doi:10.1016/0019-1035(77)90076-8
  * Li and Ingersoll (2015) C. Li, A.P. Ingersoll, Moist convection in hydrogen atmospheres and the frequency of Saturn’s giant storms. Nature Geoscience 8, 398–403 (2015). doi:10.1038/ngeo2405
  * Li et al. (2017) C. Li, A. Ingersoll, M. Janssen, S. Levin, S. Bolton, V. Adumitroaie, M. Allison, J. Arballo, A. Bellotti, S. Brown, S. Ewald, L. Jewell, S. Misra, G. Orton, F. Oyafuso, P. Steffes, R. Williamson, The distribution of ammonia on Jupiter from a preliminary inversion of Juno microwave radiometer data. Geophys. Res. Lett. 44, 5317–5325 (2017). doi:10.1002/2017GL073159
  * Li et al. (2018) C. Li, T. Le, X. Zhang, Y.L. Yung, A high-performance atmospheric radiation package: With applications to the radiative energy budgets of giant planets. J. Quant. Spectrosc. Radiat. Transfer 217, 353–362 (2018). doi:10.1016/j.jqsrt.2018.06.002
  * Li et al. (2020) C. Li, A. Ingersoll, S. Bolton, S. Levin, M. Janssen, S. Atreya, J. Lunine, P. Steffes, S. Brown, T. Guillot, M. Allison, J. Arballo, A. Bellotti, V. Adumitroaie, S. Gulkis, A. Hodges, L. Li, S. Misra, G. Orton, F. Oyafuso, D. Santos-Costa, H. Waite, Z. Zhang, The water abundance in Jupiter’s equatorial zone. Nature Astronomy 4, 609–616 (2020). doi:10.1038/s41550-020-1009-3
  * Li et al. (2013) L. Li, R.K. Achterberg, B.J. Conrath, P.J. Gierasch, M.A. Smith, A.A. Simon-Miller, C.A. Nixon, G.S. Orton, F.M. Flasar, X. Jiang, K.H. Baines, R. Morales-Juberías, A.P. Ingersoll, A.R. Vasavada, A.D. Del Genio, R.A. West, S.P. Ewald, Strong Temporal Variation Over One Saturnian Year: From Voyager to Cassini. Scientific Reports 3 (2013). doi:10.1038/srep02410
  * Li and Read (2000) X. Li, P.L. Read, A mechanistic model of the quasi-quadrennial oscillation in Jupiter’s stratosphere. Planet. Space Sci. 48(7-8), 637–669 (2000). doi:10.1016/S0032-0633(00)00033-7
  * Lindal et al. (1981) G.F. Lindal, G.E. Wood, G.S. Levy, J.D. Anderson, D.N. Sweetnam, H.B. Hotz, B.J. Buckles, D.P. Holmes, P.E. Doms, V.R. Eshleman, G.L. Tyler, T.A. Croft, The atmosphere of Jupiter: an analysis of the Voyager radio occulation measurements. Journal of Geophysical Research 86(A10), 8721–8727 (1981). doi:10.1029/JA086iA10p08721
  * Little et al. (1999) B. Little, C.D. Anger, A.P. Ingersoll, A.R. Vasavada, D.A. Senske, H.H. Breneman, W.J. Borucki, The Galileo SSI Team, Galileo Images of Lightning on Jupiter. Icarus 142, 306–323 (1999). doi:10.1006/icar.1999.6195
  * Lunine et al. (2004) J.I. Lunine, A. Coradini, D. Gautier, T.C. Owen, G. Wuchterl, The origin of Jupiter, ed. by Bagenal, F., Dowling, T. E., & McKinnon, W. B. 2004, pp. 19–34
  * Mahaffy et al. (2000) P.R. Mahaffy, H.B. Niemann, A. Alpert, S.K. Atreya, J. Demick, T.M. Donahue, D.N. Harpold, T.C. Owen, Noble gas abundance and isotope ratios in the atmosphere of Jupiter from the Galileo Probe Mass Spectrometer. J. Geophys. Res. 105, 15061–15072 (2000). doi:10.1029/1999JE001224
  * Masters et al. (in prep.) Masters et al., Magnetosphere and plasma science with the Jupiter Icy Moons Explorer. Space Science Reviews (in prep.)
  * Matcheva et al. (2001) K.I. Matcheva, D.F. Strobel, F.M. Flasar, Interaction of Gravity Waves with Ionospheric Plasma: Implications for Jupiter’s Ionosphere. Icarus 152(2), 347–365 (2001). doi:10.1006/icar.2001.6631
  * Mauk et al. (2020) B.H. Mauk, G. Clark, G.R. Gladstone, S. Kotsiaros, A. Adriani, F. Allegrini, F. Bagenal, S.J. Bolton, B. Bonfond, J.E.P. Connerney, R.W. Ebert, D.K. Haggerty, P. Kollmann, W.S. Kurth, S.M. Levin, C.P. Paranicas, A.M. Rymer, Energetic Particles and Acceleration Regions Over Jupiter’s Polar Cap and Main Aurora: A Broad Overview. Journal of Geophysical Research (Space Physics) 125(3), 27699 (2020). doi:10.1029/2019JA027699
  * Mayor and Queloz (1995) M. Mayor, D. Queloz, A Jupiter-mass companion to a solar-type star. Nature 378(6555), 355–359 (1995). doi:10.1038/378355a0
  * Medvedev et al. (2013) A.S. Medvedev, J. Sethunadh, P. Hartogh, From cold to warm gas giants: A three-dimensional atmospheric general circulation modeling. Icarus 225(1), 228–235 (2013). doi:10.1016/j.icarus.2013.03.028
  * Meftah et al. (2018) M. Meftah, L. Damé, D. Bolsée, A. Hauchecorne, N. Pereira, D. Sluse, G. Cessateur, A. Irbah, J. Bureau, M. Weber, K. Bramstedt, T. Hilbig, R. Thiéblemont, M. Marchand, F. Lefèvre, A. Sarkissian, S. Bekki, SOLAR-ISS: A new reference spectrum based on SOLAR/SOLSPEC observations. Astron. Astrophys. 611, 1 (2018). doi:10.1051/0004-6361/201731316
  * Melin et al. (2018) H. Melin, L.N. Fletcher, P.T. Donnelly, T.K. Greathouse, J.H. Lacy, G.S. Orton, R.S. Giles, J.A. Sinclair, P.G.J. Irwin, Assessing the long-term variability of acetylene and ethane in the stratosphere of Jupiter. Icarus 305, 301–313 (2018). doi:10.1016/j.icarus.2017.12.041
  * Melin et al. (2020) H. Melin, L.N. Fletcher, P.G.J. Irwin, S.G. Edgington, Jupiter in the Ultraviolet: Acetylene and Ethane Abundances in the Stratosphere of Jupiter from Cassini Observations between 0.15 and 0.19 $\mu$m. Astron. J. 159(6), 291 (2020). doi:10.3847/1538-3881/ab91a6
  * Moirano et al. (2021) A. Moirano, A. Mura, A. Adriani, V. Dols, B. Bonfond, J.H. Waite, V. Hue, J.R. Szalay, A.H. Sulaiman, B.M. Dinelli, F. Tosi, F. Altieri, A. Cicchetti, G. Filacchione, D. Grassi, A. Migliorini, M.L. Moriconi, R. Noschese, G. Piccioni, R. Sordini, D. Turrini, C. Plainaki, G. Sindoni, S. Massetti, R.L. Lysak, S.L. Ivanovski, S.J. Bolton, Morphology of the Auroral Tail of Io, Europa, and Ganymede From JIRAM L-Band Imager. Journal of Geophysical Research (Space Physics) 126(9), 29450 (2021). doi:10.1029/2021JA029450
  * Morbidelli (2020) A. Morbidelli, Planet formation by pebble accretion in ringed disks. Astron. Astrophys. 638, 1 (2020). doi:10.1051/0004-6361/202037983
  * Moreno et al. (2003) R. Moreno, A. Marten, H.E. Matthews, Y. Biraud, Long-term evolution of CO, CS and HCN in Jupiter after the impacts of comet Shoemaker-Levy 9. Planet. Space Sci. 51, 591–611 (2003)
  * Moreno et al. (2017) R. Moreno, E. Lellouch, T. Cavalié, A. Moullet, Detection of CS in Neptune’s atmosphere from ALMA observations. Astron. Astrophys. 608, 5 (2017). doi:10.1051/0004-6361/201731472
  * Moriconi et al. (2017) M.L. Moriconi, A. Adriani, B.M. Dinelli, F. Fabiano, F. Altieri, F. Tosi, G. Filacchione, A. Migliorini, J.C. Gérard, A. Mura, D. Grassi, G. Sindoni, G. Piccioni, R. Noschese, A. Cicchetti, S.J. Bolton, J.E.P. Connerney, S.K. Atreya, F. Bagenal, G.R. Gladstone, C. Hansen, W.S. Kurth, S.M. Levin, B.H. Mauk, D.J. McComas, D. Turrini, S. Stefani, A. Olivieri, M. Amoroso, Preliminary JIRAM results from Juno polar observations: 3. Evidence of diffuse methane presence in the Jupiter auroral regions. Geophys. Res. Lett. 44(10), 4641–4648 (2017). doi:10.1002/2017GL073592
  * Moses and Poppe (2017) J.I. Moses, A.R. Poppe, Dust ablation on the giant planets: Consequences for stratospheric photochemistry. Icarus 297, 33–58 (2017). doi:10.1016/j.icarus.2017.06.002
  * Moses et al. (2005a) J.I. Moses, T. Fouchet, B. Bézard, G.R. Gladstone, E. Lellouch, H. Feuchtgruber, Photochemistry and diffusion in Jupiter’s stratosphere: Constraints from ISO observations and comparisons with other giant planets. Journal of Geophysical Research (Planets) 110, 08001 (2005a). doi:10.1029/2005JE002411
  * Moses et al. (2005b) J.I. Moses, T. Fouchet, B. Bézard, G.R. Gladstone, E. Lellouch, H. Feuchtgruber, Photochemistry and diffusion in Jupiter’s stratosphere: Constraints from ISO observations and comparisons with other giant planets. Journal of Geophysical Research (Planets) 110, 08001 (2005b). doi:10.1029/2005JE002411
  * Moses and Poppe (2017) J.I. Moses, A.R. Poppe, Dust ablation on the giant planets: Consequences for stratospheric photochemistry. Icarus 297, 33–58 (2017). doi:10.1016/j.icarus.2017.06.002
  * Mousis et al. (2014) O. Mousis, R. Hueso, J.-P. Beaulieu, S. Bouley, B. Carry, F. Colas, A. Klotz, C. Pellier, J.-M. Petit, P. Rousselot, M. Ali-Dib, W. Beisker, M. Birlan, C. Buil, A. Delsanti, E. Frappa, H.B. Hammel, A.C. Levasseur-Regourd, G.S. Orton, A. Sánchez-Lavega, A. Santerne, P. Tanga, J. Vaubaillon, B. Zanda, D. Baratoux, T. Böhm, V. Boudon, A. Bouquet, L. Buzzi, J.-L. Dauvergne, A. Decock, M. Delcroix, P. Drossart, N. Esseiva, G. Fischer, L.N. Fletcher, S. Foglia, J.M. Gómez-Forrellad, J. Guarro-Fló, D. Herald, E. Jehin, F. Kugel, J.-P. Lebreton, J. Lecacheux, A. Leroy, L. Maquet, G. Masi, A. Maury, F. Meyer, S. Pérez-Hoyos, A.S. Rajpurohit, C. Rinner, J.H. Rogers, F. Roques, R.W. Schmude, B. Sicardy, B. Tregon, M. Vanhuysse, A. Wesley, T. Widemann, Instrumental methods for professional and amateur collaborations in planetary astronomy. Experimental Astronomy 38, 91–191 (2014). doi:10.1007/s10686-014-9379-0
  * Mura et al. (2017a) A. Mura, A. Adriani, F. Altieri, J.E.P. Connerney, S.J. Bolton, M.L. Moriconi, J.-C. Gérard, W.S. Kurth, B.M. Dinelli, F. Fabiano, F. Tosi, S.K. Atreya, F. Bagenal, G.R. Gladstone, C. Hansen, S.M. Levin, B.H. Mauk, D.J. McComas, G. Sindoni, G. Filacchione, A. Migliorini, D. Grassi, G. Piccioni, R. Noschese, A. Cicchetti, D. Turrini, S. Stefani, M. Amoroso, A. Olivieri, Infrared observations of Jovian aurora from Juno’s first orbits: Main oval and satellite footprints. Geophys. Res. Lett. 44(11), 5308–5316 (2017a). doi:10.1002/2017GL072954
  * Mura et al. (2017b) A. Mura, A. Adriani, F. Altieri, J.E.P. Connerney, S.J. Bolton, M.L. Moriconi, J.-C. Gérard, W.S. Kurth, B.M. Dinelli, F. Fabiano, F. Tosi, S.K. Atreya, F. Bagenal, G.R. Gladstone, C. Hansen, S.M. Levin, B.H. Mauk, D.J. McComas, G. Sindoni, G. Filacchione, A. Migliorini, D. Grassi, G. Piccioni, R. Noschese, A. Cicchetti, D. Turrini, S. Stefani, M. Amoroso, A. Olivieri, Infrared observations of Jovian aurora from Juno’s first orbits: Main oval and satellite footprints. Geophysical Research Letters 44(11), 5308–5316 (2017b). doi:10.1002/2017GL072954
  * Mura et al. (2018) A. Mura, A. Adriani, J.E.P. Connerney, S. Bolton, F. Altieri, F. Bagenal, B. Bonfond, B.M. Dinelli, J.-C. Gérard, T. Greathouse, D. Grodent, S. Levin, B. Mauk, M.L. Moriconi, J. Saur, J.H. Waite, M. Amoroso, A. Cicchetti, F. Fabiano, G. Filacchione, D. Grassi, A. Migliorini, R. Noschese, A. Olivieri, G. Piccioni, C. Plainaki, G. Sindoni, R. Sordini, F. Tosi, D. Turrini, Juno observations of spot structures and a split tail in Io-induced aurorae on Jupiter. Science 361(6404), 774–777 (2018). doi:10.1126/science.aat1450