# Near-Earth Asteroids of Cometary Origin Associated with the Virginid Complex

G.I. Kokhirova<EMAIL_ADDRESS>A.I. Zhonmuhammadi  U.H. Khamroev  T.J.
Jopek  Institute of Astrophysics of the National Academy of Sciences of
Tajikistan, Ayni 299/5, Dushanbe, 734063, Tajikistan  Astronomical Observatory
Institute, Faculty of Physics, A. M. University, Poznan, Poland

###### Abstract

The Virginid meteoroid streams produce a series of meteor showers active
annually during February-May. A certain parent comet is not found but a
related association of some showers with near-Earth asteroids was previously
established and a cometary origin of these asteroids was suggested. We
performed a new search for NEAs belonging to the Virginid asteroid-meteoroid
complex. On the base of calculation of orbital evolution of a sample of NEAs
and determination of theoretical features of related showers a search for
observable active showers close to theoretically predicted ones was carried
out. As a result, the predicted showers of 29 NEAs were identified with the
showers of the Virginid complex. Revealed association points to a cometary
nature of NEAs that are moving within the stream and may be considered as
extinct fragments of a larger comet-progenitor of the Virginid asteroid-
meteoroid complex.

###### keywords:

meteoroid stream, meteor showers , near-Earth asteroids , extinct comets ,
asteroid-meteoroid complexes

††journal: Planetary and Space Science

##  1 Introduction

Besides of major planets a lot of smaller bodies are moving in the Solar
System. This population consists of comets, asteroids, and meteoroids. Comets
and asteroids are the parents of meteoroids. A huge number of meteoroids
generated by a one parent body form a meteoroid stream. The stream’s
meteoroids are moving in the interplanetary space by similar orbits close to
the orbit of the parent. It is accepted that the activity of comets or their
destruction are responsible for a formation of meteoroid streams. Forming of
the stable long-lived meteoroid stream can be provided by a periodic normal
gas- and dust producing activity of comet which is observing during passage of
the perihelion (Whipple, 1950, 1951; Bredihin, 1954). Moreover, a stream might
be generated as a result of the catastrophic decay of comet due to an impact
or other processes (Gronkowski, 2007; Wesolowski et al., 2020). However, a
break-up of a comet or an asteroid cannot lead to a formation of meteoroid
stream, at least, the long-lived stream, since in this case the ejection of
dust and debris will be once that is not sufficient for a formation of a
stable stream.

A concept of the formation of meteoroid streams as a result of the cometary
activity, as well as the circumstances of their evolution and structure are
described in a lot of papers (see e.g. Whipple, 1950, 1951; Hughes, 1986;
Babadzhanov, Obrubov, 1992; Williams, 1993; Babadzhanov et al., 2008a, 2015a).
When the Earth crosses the meteoroid stream orbits, the meteor showers are
occurring. As was shown by Babadzhanov, Obrubov (1992) one stream might
produce from four till eight meteor showers observable on the Earth. The
quadruple intersections are the most spread event for meteoroid streams. For
instance, the Taurid meteoroid stream consists of four meteor showers. At the
pre-perihelion crossing with the Earth’s orbit they are the Northern and
Southern Taurids (17/NTA and 2/STA according to the official nomenclature
given in the IAU MDC, see Jopek, Jenniskens (2011); Jopek, Kanuchova (2014,
2017) and after the naming rules have been modified in Jopek et al. (2023)),
which are observable on the Earth annually in September-November, as well as
the Daytime $beta$-Taurids (173/BTA) and Daytime $zeta$-Perseids (172/ZPE)
observable in June-July which are occurring at the post-perihelion crossing.
The well-known parent body of the Taurid stream is comet 2P/Encke; however, it
turned out that else more than 40 near-Earth asteroids (NEAs) relate to this
family (Asher et al., 1993a, b; Babadzhanov, 2001; Babadzhanov et al., 2008a;
Porubcan et al., 2004, 2006; Madiedo et al., 2013; Rudawska et al., 2012a, b;
Kokhirova et al., 2022). The related association of these objects was found
and the family was called as the Taurid asteroid-meteoroid complex. It was
defined that asteroids of the Taurid complex very likely are extinct cometary
nuclei or dead fragments of the larger comet-progenitor (see e.g. Asher et
al., 1993a; Porubcan et al., 2006; Babadzhanov et al., 2008a). The presence of
a certain number of extinct (dormant) cometary nuclei in the NEA population is
not in doubt; it is estimated that it may account for almost 6% of the total
number of known NEAs (Opik, 1963; Weissman et al., 1989; Jenniskens, 2008;
Babadzhanov, Kokhirova, 2009).

A cometary nucleus which was active at past and then loosed ability to
generate a coma visible at any parts of its orbit is denoted by the term
dormant or extinct comet (Weissman et al., 1989). The nuclei of such comets
have covered throughout evolution by the thick infusible mantle; as a
consequence, a normal cometary activity was ceased (Whipple, 1950, 1951; Opik,
1963). Note, extinct comet could be reactivated by the perturbing to the
smaller perihelion distance or due to collision with another body (Weissman et
al., 1989). By the ground-based observations extinct cometary nuclei outwardly
do not differ from asteroids. However, they may be distinguished by the
dynamical properties, namely, by their orbital elements. The typical comet-
like orbit of an object implies that it has a cometary origin. Finding the
connection of such an object with the meteoroid stream producing active
observable on the Earth meteor showers justifies the supposition that the
object is an extinct comet.

Several asteroid-meteoroid complexes were identified using this “meteor sign”
approach, such as the Piscid complex (Babadzhanov et al., 2008b), the
$iota$-Aquariid complex (Babadzhanov et al., 2009), the $chi$-Scorpiid complex
(possibly, the $chi$-Scorpiids relates to the $omega$-Scorpiid complex) (Cook,
1973; Babadzhanov et al., 2013), the $sigma$-Capricornid complex (Babadzhanov
et al., 2015b), etc. These complexes consist of the meteoroid streams and
objects of cometary origin identified among NEAs, which (these objects) may
supposedly be the parent bodies of these streams. However, the parent bodies
are not established for majority of known meteoroid streams. Furthermore, a
search for the parents of meteoroid streams is a key stage in a recognizing of
genetic associations between the minor bodies of the Solar system. We have
continued the investigation of their interrelations and revealing new extinct
comets among the NEAs, and present the results of a finding of related objects
in the Virginid meteoroid complex.

##  2 Meteor showers of the Virginid complex

The group of meteor showers producing by the relevant streams (sub-streams)
and having the area of radiation in the Virgo constellation forms the Virginid
complex. The period of activity of the nighttime showers begins in February,
completely covers March-April and terminates in May, while the activity of the
daytime showers falls on the period September-October. So that it is one of
the largest regions of the annual meteor activity appearing, as a rule, in 165
deg. (the nighttime showers) and 345 deg. (the daytime showers) to the West
from the Sun. The region was named as the Virginid shower by Hoffmeister
(1948) and mentioned as one of the ecliptic showers visible during a year.
Hoffmeister’s study was the first to attempt to identify the individual
streams of the Virginid region. The strongest supported shower of this complex
belongs to the $theta$-Virginids and was based on 12 individual radiant
determinations. It was most active on March 15 at the Solar longitude of 355.7
deg. from a radiation region of $RA$=192.4 deg. and $DEC$=-1.5 deg.
(Hoffmeister, 1948). Garry Kronk in his catalogue lists the following branches
of the Virginid comlpex from February to May: $eta$-Virginids, $pi$-Virginids,
$theta$-Virginigs, $alpha$-Virginids, $gamma$-Virginids and April Virginids
(Kronk, 1988). Some Virginid’s showers were mentioned in the monographs of
Lovell (1954); Jenniskens (2006) as well.

According the IAU MDC meteor showers database available at the website
https://www.ta3.sk/IAUC22DB/MDC2022/ (2023) (see Jopek, Jenniskens, 2011;
Jopek, Kanuchova, 2014, 2017; Hajdukova et al., 2023) the following
established showers of the Virginid complex are provided: $alpha$-Virginids
(21/AVB) (Southworth, Hawkins, 1963; Lindblad, 1971a, b; Jenniskens et al.,
2016), having the activity period in 12-22 April; $h$-Virginids (343/HVI)
(SonotaCo, 2009; Molau, Rendtel, 2009; Jenniskens et al., 2016; Roggemans et
al., 2020), maximum activity in 22-29 April; February $epsilon$-Virginids
(506/FEV) (Steakley, Jenniskens, 2013; Molau et al., 2013; Jenniskens et al.,
2016) with activity in 3-4 February and possible association with comets
C/1808F1 (Pons) and C/1978T3 (Bradfield); $eta$-Virginids (11/EVI) maximal
active in 18 March (Lindblad, 1971a; Jenniskens, 2006; Jenniskens et al.,
2016), the proposed parent is comet D/1766 G1 (Helfenzrieder). Besides, some
showers are given in the database which need the observational confirmation:
Northern and Southern March Virginids (123/NVI, 124/SVI) (Sekanina, 1973;
Kronk, 1988; Kascheev et al., 1967), with the activity maximum in 15-19 and
17-23 March respectively; $kappa$-Virginids (509/KVI) (Segon et al., 2013), 27
March; $mu$-Virginids (47/DLI) (Porubcan, Gavajdova, 1994), 20-29 April;
Northern and Southern $gamma$-Virginids (134/NGV and 135/SGV) (Terentjeva,
1989; Porubcan, Gavajdova, 1994), the maximum activity in 14 and 13 April
respectively, and the possible parent bodies NEAs 2002 FC and 2003 BD44,
correspondingly; etc.

Table 1 lists the average values of the more important parameters of the
Virginids complex. They were taken from the IAU MDC database, but only those
values were selected which were obtained from the averaging of the largest
number of individual radiants and orbits of the members of the given shower.
Bibliographic sources are given from the IAU MDC and denoted as Jenniskens et
al. (2016) \- J1, Roggemans et al. (2020) \- R, Sekanina (1973) \- S2, Segon
et al. (2013) \- SE, Lindblad (1971b) \- L2, Porubcan, Gavajdova (1994) \- P,
Terentjeva (1966, 1989) \- T, T1.

Table 1: Meteor showers included in the Virginids complex. The mean geocentric and heliocentric parameters were taken from the IAU MDC database (status 2023-May). $SunL$ is the Sun ecliptic longitude at the maximum shower activity, $RAg$ and $DECg$ are the geocentric radiant coordinates, $V_{g}$ is the geocentric velocity in [km/s], $q$ is the perihelion distance in [au], $e$ is the eccentricity, $\omega$ is the argument of perihelion, $\Omega$ is the longitude of the ascending node, $i$ is the inclination of the orbit, $N$ means the number of orbits used to find the mean shower parameters, in the last column the bibliographic source is given from the IAU MDC. The angular parameters are given in degrees in the reference system J2000. The four streams officially named by the IAU are highlighted by bold font. Note, the showers Northern and Southern $nu$-Virginids proposed by Terentjeva (1966, 1989) did not included into the MDC. Codes | SunL | $RA_{g}$ | $DEC_{g}$ | $V_{g}$ | $q$ | $e$ | $\omega$ | $\Omega$ | $i$ | $N$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---
21/AVB | 32.0 | 203.5 | 2.9 | 18.8 | 0.744 | 0.716 | 247.9 | 30.0 | 7.0 | 12 | J1
$\alpha$-Virds |  |  |  |  |  |  |  |  |  |  |
343/HVI | 38.4 | 203.0 | -10.7 | 18.8 | 0.740 | 0.741 | 66.0 | 219.8 | 0.4 | 34 | R
$h$-Virds |  |  |  |  |  |  |  |  |  |  |
506/FEV | 314.0 | 200.4 | 11.0 | 62.9 | 0.491 | 0.954 | 272.5 | 312.6 | 138.0 | 55 | J1
Feb.$\epsilon$-Virds |  |  |  |  |  |  |  |  |  |  |
11/EVI | 357.0 | 184.8 | 3.9 | 26.6 | 0.460 | 0.812 | 281.0 | 355.7 | 5.4 | 57 | J1
$\eta$-Virds |  |  |  |  |  |  |  |  |  |  |
123/NVI | 358.0 | 185.7 | 2.3 | 23.0 | 0.496 | (0.707) | 282.4 | 358.0 | 3.7 | 18 | S2
Northern |  |  |  |  |  |  |  |  |  |  |
March Virds |  |  |  |  |  |  |  |  |  |  |
124/SVI | 2.0 | 179.7 | -8.5 | 22.9 | 0.565 | (0.738) | 81.2 | 182.0 | 6.1 | 13 | S2
Southern |  |  |  |  |  |  |  |  |  |  |
March Virds |  |  |  |  |  |  |  |  |  |  |
509/KVI | 6 | 208 | -8 | 37.4 | 0.139 | 0.938 | 321 | 6 | 8 | 58 | SE
$\kappa$-Virds |  |  |  |  |  |  |  |  |  |  |
49/LVI | 20 | 210.7 | -10.2 | 26.8 | 0.343 | (0.870) | 295.0 | 20.2 | 2.0 | - | L2
$\lambda$-Virds |  |  |  |  |  |  |  |  |  |  |
47/DLI | 39 | 226.8 | -8.7 | 28.3 | 0.418 | (0.835) | 286.5 | 38.3 | 9.1 | 3 | P
$\mu$-Virds |  |  |  |  |  |  |  |  |  |  |
134/NGV | 24.3 | 180.6 | 17.7 | 11.7 | 0.908 | (0.596) | 221.7 | 24.3 | 5.2 | - | T1
Northern |  |  |  |  |  |  |  |  |  |  |
$\gamma$-Virds |  |  |  |  |  |  |  |  |  |  |
135/SGV | 22.7 | 183.2 | -15.5 | 13.9 | 0.867 | (0.617) | 50.0 | 212.7 | 5.0 | 5 | P
Southern |  |  |  |  |  |  |  |  |  |  |
$\gamma$-Virds |  |  |  |  |  |  |  |  |  |  |
Northern | 348.8 | 173.0 | 6.0 | 24.8 | 0.521 | 0.790 | 274.4 | 348.8 | 2.3 | - | T1
$\nu$-Virds |  |  |  |  |  |  |  |  |  |  |
Southern | 340.4 | 170.0 | 4.0 | 28.5 | 0.387 | 0.850 | 109.1 | 160.4 | 0.3 | - | T
$\nu$-Virds |  |  |  |  |  |  |  |  |  |  |

The parent comets of meteoroid streams of the Virginid complex have not been
established surely. NEA 1998 SH2 was suggested as a proper parent body of the
$alpha$-Virginids (21/AVB) stream (Jenniskens, 2006). The related association
of NEA 2004 CK39 and the Northern and Southern $nu$-Virginids (Terentjeva,
1966, 1989) as well of asteroid 2007 CA19 and the Northern and Southern
$eta$-Virginids (Sekanina, 1973, 1976; Terentjeva, 1966, 1989) was found and a
cometary nature of these asteroids was supposed on this base (Babadzhanov et
al., 2012, 2015c). In our study, we performed a search for new objects
associated with the complex, among NEAs discovered till the end of 2014, as a
result, four asteroids families were identified related to four sub-streams of
the Virginid complex. The results are presented in this paper.

##  3 Method of investigation

We adopted a concept of formation and evolution of meteoroid streams given by
Babadzhanov, Obrubov (1992). According to it, from a huge number of stream’s
meteoroids, only the bodies having the orbits with the heliocentric distances
of ascending $R_{a}$ and descending $R_{d}$ nodes close to 1 AU can intersect
the Earth’s orbit. Alongside with this, for the majority of NEAs this
condition realizes four times over one Kozai-Lidov cycle of the orbital
argument of perihelion. If an asteroid is actually a non-active comet, then in
the past it may have created a meteoroid stream. Theoretically, such a stream
may produce four meteor showers observable on the Earth - the nighttime
showers with northern and southern branches and the daytime showers also with
northern and southern branches. Having the orbital elements for which the
nodal distances $R_{a}$ or $R_{d}$ are close to 1 AU, one can calculate the
theoretical radiants of the possible meteor showers. The identification of
theoretical showers with observable showers, fireballs/meteors and other
objects most likely confirms the relationship between these showers and the
studied asteroid as well as the cometary nature of the asteroid. The orbits of
theoretical meteor showers can be obtained by calculation of the orbital
evolution of the proposed parent body – near-Earth asteroid. The orbital
evolution is calculated using various methods of numerical integration of the
motion equation for the time equal to one cycle of variation of the argument
of perihelion of the asteroid orbit. In the case of NEAs, this time interval
is usually between 5 and 12 thousand years. The methods of Everhart (1974) and
Halphen-Goryachev (Goryachev, 1937) are the most using for the orbital
evolution calculation.

##  4 The near-Earth asteroids associated with Virginids complex

Only asteroids moving on the comet-like orbits and crossing the Earth’s orbit
are subject of the investigation. The Tisserand parameter $T_{j}$ is using for
classification of orbits (Kresak, 1969, 1982; Kosai, 1992). While the value of
the Tisserand parameter satisfies the condition $T_{j}\leq$3.12, then the
orbit is classified as comet-like, when $T_{j}>$3.12 the orbit relates to
asteroidal type (Kresak, 1969; Jewitt, 2012). Applying Tisserand condition
$T_{j}\leq$3.12, 29 NEAs from JPL’s Solar System Dynamics database
(www.jpl.ssd.nasa.gov, 2023) was selected and their motion was calculated by
RADAU19 integrator (Everhart, 1974). Gravitational perturbations of major
planets Mercury-Jupiter were taken into account as well; the relevant
planetary data were taken from the JPL DE403 ephemeris (Standish et al., 1995;
www.jpl.ssd.nasa.gov, 2023).

###  4.1 Investigation of orbital evolution

As a result of calculation of orbital evolution it was found that 29 asteroids
listed in Table 2, cross the Earth’s orbit for four times during one cycle of
$\omega$ variation. It means that the sizes of $R_{a}$ and $R_{d}$ of
asteroids orbits have the values close to 1 AU four times – two cases at each
of the nodes. The variability of the length $R_{a}$ and $R_{d}$ depending on
time and argument of perihelion is illustrated in figures below. These graphs
are similar for all considered NEAs so the plots for a pair of selected
asteroids are presented. For asteroids 2010 EK44 and 2014 EQ associated with
the $alpha$-Virginid meteoroid stream it is shown in Figs. 1; for asteroids
2010 FJ81 and 2014 VC10 associated with the $eta$-Virginid meteoroid stream it
is shown in Figs. 2; for asteroids 2013 TR13 and 2013 CU82 associated with the
$nu$-Virginid meteoroid stream it is shown in Figs. 3; and for pair asteroids
2010 GO33 and 2011 VG9 associated with the $mu$-Virginid meteoroid stream it
is shown in Figs. 4.

Figure 1:  Variations of nodal distances $R_{a}$ and $R_{d}$ of the orbit of
asteroids associated with the $alpha$-Virginids meteoroid stream. Top, the NEA
2010 EK44, bottom the NEA 2014EQ. The points corresponding to the conditions
$R_{a}$ =$R_{d}$ =1 AU, i.e. intersection of the Earth’s orbit and the
asteroid orbit, are indicated by arrows.  Figure 2: Variations of nodal
distances $R_{a}$ and $R_{d}$ of the orbit of asteroids associated with the
$eta$-Virginids meteoroid stream. Top the NEA 2010 FJ81, bottom the NEA 2014
VC10. The points corresponding to the conditions $R_{a}$ =$R_{d}$ =1 AU, i.e.
intersection of the Earth’s orbit and the asteroid orbit, are indicated by
arrows.  Figure 3:  Variations of nodal distances $R_{a}$ and $R_{d}$ of the
orbit of asteroids associated with the $nu$-Virginids meteoroid stream. Top
the NEA 2013 TR13, bottom the NEA 2013 CU82. The points corresponding to the
conditions $R_{a}$ =$R_{d}$ =1 AU, i.e. intersection of the Earth’s orbit and
the asteroid orbit, are indicated by arrows.  Figure 4:  Variations of nodal
distances $R_{a}$ and $R_{d}$ of the orbit of asteroids associated with the
$mu$-Virginids meteoroid stream. Top the NEA 2010 GO33, bottom the NEA 2011
VG9. The points corresponding to the conditions $R_{a}$ =$R_{d}$ =1 AU, i.e.
intersection of the Earth’s orbit and the asteroid orbit, are indicated by
arrows.

A set of the orbital elements which corresponds to the Earth’s crossing
positions found from the calculated orbital evolution serves as the initial
data for calculation of the coordinates of theoretical geocentric radiants
(right ascension $\alpha_{g}$ and declination $\delta_{g}$), the geocentric
velocities $V_{g}$, the Solar longitudes $L_{\odot}$ and relevant dates of the
activity of theoretical showers.

###  4.2 General results

A computerized search for similar theoretically predicted and observed showers
was carried out in the published meteor/fireball catalogues: Terentjeva (1966,
1989) (T, T1), Lindblad (1971a, b) (L1, L2), Lebedinets et al. (1973) (L),
Kascheev et al. (1967) (K), Jenniskens et al. (2016) (J1), Rudawska et al.
(2015) (EDM1), Rudawska, Jenniskens (2014) (EDM2), Southworth, Hawkins (1963)
(SH), SonotaCo (2009) (SON), Sekanina (1973, 1976) (S1, S2), Gajdosh, Porubcan
(2004) (G), Cook (1973) (C), Porubcan, Gavajdova (1994) (P), etc. Up-present
orbital elements of 29 considered NEAs (Table 2) were also included into
database where we performed a search. Additionally, we performed this search
among databases of individual meteors/fireballs and known meteorites:
https://www.ta3.sk/IAUC22DB/MDC2022/ (2023) (MODC), Halliday et al. (1996)
(MORP), McCrosky et al. (1978) (PN), EN – fireballs detected by the European
fireball network, Ceplecha (1961) (C1), Spurny et al. (2003) (SP).

Under a comparison of theoretical and observable parameters we required that
the difference in radiants not exceed $\pm$10 deg. in both right ascension and
declination, the difference in geocentric velocities should be $\Delta
V_{g}\pm$5 km/s, and the periods of activity may differ no more than $\pm$15
days (see e.g. Babadzhanov et al., 2009).

A closeness of the theoretical and observable orbits was examined using the
Southworth, Hawkins (1963) $D$-function, $D_{SH}$, being a measure of the
similarity between two orbits. It is accepted to consider two orbits similar
when the condition $D_{SH}\leq$ 0.25 is fulfilled (Southworth, Hawkins, 1963).

As a result of a search it turned out that considered NEAs form four groups
associated with four sub-streams of the Virginid complex, asteroids parameters
are given in the separate sections of Table 2. In addition to the elements of
Keplerian orbits we provide the absolute magnitudes, equivalent diameters of
the NEAs as well as the number of intersections of the asteroid’s orbit with
the Earth’s orbit during one Kozai-Lidov cycle.

The diameters denoted by asterisk in Table 2 are accessible at the published
JPL SSD database. At the cases of a lack of size estimation the diameters were
calculated by the following empirical equation Harris (2002)

$d=\frac{1329}{\sqrt{p}\cdot 10^{0.2H}},$ (1)

where $p$ is the geometrical albedo of an asteroid. Very dark asteroids of
$C,P$, and $D$ types having a low albedo within 0.02-0.12 very likely might be
extinct comets (Jewitt, 1992). The diameters of asteroids were estimated using
the average value of albedo $p$=0.07.

Table 2:  The basic features of NEAs associated with the Virginid complex. In the first column the stream or NEA designations are given, the next ones contain Keplerian orbital elements (for NEAs MJD equal to 2014.12.09), $H$ is the absolute magnitude, $d$ is an equivalent diameter, $T_{j}$ is Tisserend parameter, $Ni$ is the number of intersections of the stream’s and asteroid’s orbits with the Earth’s orbit during one Kozai-Lidov cycle. All angular elements of the meteoroid streams and NEAs are given in the J2000 reference system. Object |  $a$, | $e$ |  $q$, | $i^{\circ}$ | $\omega^{\circ}$ | $\Omega^{\circ}$ | $\pi^{\circ}$ | $H$ |  $d$, | $Ni$ | $T_{j}$
---|---|---|---|---|---|---|---|---|---|---|---
| AU |  | AU |  |  |  |  |  | km |  |
21/AVB | 2.550 | 0.716 | 0.744 | 7.0 | 247.9 | 30.0 | 277.9 | - | - | 4 | 3.01
2009 HS44 | 2.572 | 0.702 | 0.766 | 2.4 | 209.3 | 73.1 | 282.4 | 26.6 | 0.02 | 4 | 3.02
2009 SM98 | 2.432 | 0.700 | 0.730 | 7.5 | 166.9 | 110.9 | 277.8 | 22.3 | 0.17 | 4 | 3.11
2010 EK44 | 2.835 | 0.772 | 0.646 | 11.2 | 180.8 | 107.6 | 288.4 | 19.8 | 0.55 | 4 | 2.76
(PHA) |  |  |  |  |  |  |  |  |  |  |
2010 FD7 | 2.584 | 0.685 | 0.813 | 6.2 | 357.5 | 269.2 | 266.8 | 22.1 | 0.08* | 4 | 3.04
2011 BE38 | 2.629 | 0.711 | 0.759 | 8.2 | 321.4 | 302.5 | 264.0 | 18.4 | 1.07 | 4 | 2.97
(PHA) |  |  |  |  |  |  |  |  |  |  |
2011 EF17 | 2.345 | 0.743 | 0.603 | 4.2 | 4.0 | 282.3 | 286.3 | 19.2 | 0.73 | 4 | 3.12
(PHA) |  |  |  |  |  |  |  |  |  |  |
2012 SW20 | 2.460 | 0.680 | 0.788 | 10.2 | 209.8 | 62.1 | 272.0 | 19.7 | 0.59 | 4 | 3.11
(PHA) |  |  |  |  |  |  |  |  |  |  |
2012 TT256 | 2.666 | 0.729 | 0.724 | 11.1 | 106.3 | 172.0 | 278.2 | 19.5 | 0.63 | 4 | 2.91
2013 TE135 | 2.361 | 0.759 | 0.569 | 6.0 | 182.4 | 102.9 | 285.4 | 19.9 | 0.52 | 4 | 3.08
(PHA) |  |  |  |  |  |  |  |  |  |  |
2014 EQ12 | 2.637 | 0.744 | 0.675 | 11.0 | 178.0 | 92.3 | 270.3 | 21.1 | 0.31 | 4 | 2.91
(PHA) |  |  |  |  |  |  |  |  |  |  |
2014 GN1 | 2.649 | 0.749 | 0.665 | 3.0 | 193.1 | 80.3 | 273.4 | 24.6 | 0.06 | 4 | 2.91
1998S H2 | 2.693 | 0.723 | 0.760 | 2.5 | 13.3 | 261.0 | 274.3 | 20.8 | 0.35 | 4 | 2.91
(PHA) |  |  |  |  |  |  |  |  |  |  |
1998 FR11 | 2.791 | 0.713 | 0.802 | 6.6 | 130.3 | 157.9 | 288.2 | 16.5 | 2.52 | 4 | 2.91
1999 UZ5 | 2.563 | 0.799 | 0.532 | 10.3 | 226.6 | 66.7 | 293.3 | 21.9 | 0.21 | 4 | 2.85
11/EVI | 2.470 | 0.812 | 0.460 | 5.4 | 281.0 | 355.7 | 276.7 | - | - | 4 | 2.91
2010 FJ81 | 3.598 | 0.684 | 1.138 | 42.5 | 97.4 | 171.7 | 269.1 | 20.5 | 0.42* | 4 | 2.34
2012 BJ134 | 2.258 | 0.833 | 0.377 | 21.2 | 144.6 | 138.2 | 282.8 | 18.2 | 1.15 | 4 | 2.99
2014 VC10 | 2.231 | 0.817 | 0.408 | 11.8 | 84.0 | 196.7 | 280.7 | 19.4 | 0.67 | 4 | 3.07
2003 FB5 | 2.512 | 0.788 | 0.532 | 5.3 | 358.4 | 288.4 | 286.8 | 23.4 | 0.10 | 4 | 2.92
1995 EK1 | 2.266 | 0.776 | 0.508 | 8.8 | 355.5 | 296.7 | 292.2 | 17.9 | 1.34 | 4 | 3.12
2007 CA19 | 2.787 | 0.827 | 0.483 | 9.6 | 174.8 | 97.6 | 272.4 | 17.6 | 0.90 | 4 | 2.80
(PHA) |  |  |  |  |  |  |  |  |  |  |
$\nu$-Virds | 2.342 | 0.822 | 0.394 | 5.8 | 289.6 | 336.6 | 271.1 | - | - | 4 | 2.99
2013 TR135 | 2.224 | 0.809 | 0.424 | 1.8 | 243.4 | 18.0 | 261.4 | 23.3 | 0.11 | 4 | 3.11
2013 CU82 | 2.493 | 0.774 | 0.562 | 10.8 | 317.8 | 303.3 | 261.0 | 21.1 | 0.31 | 4 | 2.95
2002 BK25 | 2.296 | 0.749 | 0.576 | 11.9 | 156.5 | 103.6 | 260.1 | 18.1 | 1.22 | 4 | 3.12
(PHA) |  |  |  |  |  |  |  |  |  |  |
2002 TZ59 | 2.597 | 0.842 | 0.411 | 16.5 | 7.4 | 249.7 | 257.1 | 22.9 | 0.13 | 4 | 2.79
2004 CK39 | 2.298 | 0.829 | 0.392 | 12.3 | 359.5 | 265.1 | 264.6 | 19.3 | 0.69 | 4 | 2.99
47/DLI | 2.531 | 0.835 | 0.418 | 9.1 | 286.5 | 39.3 | 325.8 | - | - | 4 | 2.81
2010 XD11 | 2.210 | 0.854 | 0.322 | 16.4 | 118.0 | 196.1 | 314.2 | 18.09 | 1.21 | 4 | 3.01
2010 GO33 | 2.409 | 0.699 | 0.724 | 19.1 | 143.6 | 153.6 | 297.2 | 19.19 | 0.31* | 4 | 3.08
2011 VG9 | 2.275 | 0.776 | 0.509 | 1.3 | 236.1 | 65.9 | 302.0 | 22.18 | 0.18 | 4 | 3.11
2003 WW26 | 2.388 | 0.798 | 0.482 | 6.3 | 57.7 | 254.6 | 312.3 | 22.21 | 0.20 | 4 | 2.99

In Table 2, the common features of 29 NEAs (including two asteroids 2007CA19
and 2004 CK39 previously established by Babadzhanov et al. (2012, 2015c)) are
the cometary nature of their orbits and close values of the longitudes of
perihelion within each group. Furthermore, 9 asteroids denoted as PHA are
classified as potentially hazardous ones (www.jpl.ssd.nasa.gov, 2023).

##  5 Identification of the theoretically predicted and observable showers

###  5.1 Asteroids associated with the $alpha$-Virginids stream

As a result of a search it was found that a set of 14 NEAS (first section of
Table 1) have close association with the meteoroid stream generating the
nighttime $alpha$-Virginids (21/AVB) shower (the Northern branch), and the
$h$-Virginids (343/HVI) and $chi$-Virginids (the Southern branch). The
parameters of the HVI (Jenniskens et al., 2016; SonotaCo, 2009) and the
$chi$-Virginids (Terentjeva, 1989) showers are also matching with the account
of the daily radiant drift $dRA$=0.11, $dDEC$=-0.27 (SonotaCo, 2009);
therefore it may be assumed that it is one shower. Besides, the related
association of NEAs: 1998 SH2, 2009 HS44, 2012 SW20, 2014 GN1, 1999 UZ5, 2009
SM98, 2014 EQ12, 2010 EK44, 2013 TE135, 1998 FR11, 2010 FD7, 2011 EF17, 1995
EK1, 2003 FB5 and 2011 BE38 with the theoretical and observable showers is
found on the base of relevant radiants and the present-date orbits of
asteroids. A proposed link of the stream with asteroid 1998 SH2 is also
confirmed.

The results of a search for asteroids 2010 EK44 and 2010 FD7 are presented in
Tables 3 and 4. For the rest asteroids of this set the outcomes are identical.
The orbital elements, radiants, Solar longitudes and activity dates of
theoretically predicted showers are given by bold font in Tables 3 and 4; the
Northern branch of nighttime shower is denoted as NNS, the Southern branch of
nighttime shower is denoted as SNS, the Northern branch of daytime shower is
denoted as NDS, and the Southern branch of daytime shower is denoted as SDS.
Catalogues and papers where active observable showers and fireballs, known
meteorites identical with the theoretical showers were found listed in Tables
3 and 4 as T1 (Terentjeva, 1989), L1, L2 (Lindblad, 1971a, b), L (Lebedinets
et al., 1973), K (Kascheev et al., 1967), J1 (Jenniskens et al., 2016), SH
(Southworth, Hawkins, 1963), SON (SonotaCo, 2009), C1 (Ceplecha, 1961), SP
(Spurny et al., 2003), MORP (Halliday et al., 1996), PN (McCrosky et al.,
1978). The present-date orbits of the asteroids are taken in
www.jpl.ssd.nasa.gov (2023) denoted in Tables 3 and 4 as JPL, their radiants
calculated in this work denoted as tw.

It turned out that features of some studied NEAs are close to features of
theoretical showers. The NEAs present-day orbital elements were given from JPL
SSD database (www.jpl.ssd.nasa.gov, 2023), their geocentric radiants,
velocities and Solar longitudes were calculated by us using the orbital
elements. A closeness of present-day orbits (and radiants) of some NEAs to
theoretical orbits (and radiants) points to a genetic relationship between
asteroid as well. As seen, the values of the $D_{SH}$ criterion confirm a
similarity of the theoretical and observable orbits. Identification of the
theoretical showers with the observable objects is approving by a closeness of
the radiant positions, velocities and activity dates. It allows concluding
that the association of the asteroids with these showers exists and,
consequently, NEAs under consideration very likely have in fact a cometary
origin. Moreover, these objects may be considered as the parent bodies of the
stream or they can be extinct fragments of a larger comet-progenitor of the
stream. Thus this meteoroid stream contains large-sized remnants of the parent
comet which presently are in dormant stage.

Table 3:  Meteor showers, fireballs and NEAs associated with NEA 2010 EK44 (J2000.0). Objects | $q$ | $e$ | $i^{\circ}$ | $\Omega^{\circ}$ | $\omega^{\circ}$ | $L_{\odot}^{\circ}$ | Date | $\alpha_{g}^{\circ}$ | $\delta_{g}^{\circ}$ | $V_{g}$ | $D$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---|---
| AU |  |  |  |  |  |  |  |  | km/s | SH |
NNS | 0.648 | 0.771 | 9.3 | 29.2 | 259.2 | 29.2 | 19Apr | 207.7 | 2.9 | 22.2 | - | tw
21/AVB | 0.724 | 0.716 | 7.0 | 30.0 | 247.9 | 30.0 | 20Apr | 203.5 | 2.9 | 18.8 | 0.17 | J1
As.8 | 0.657 | 0.700 | 11.0 | 28.0 | 260.0 | 28.0 | 18Apr | 208.0 | 6.0 | 21.2 | 0.08 | K
299 | 0.609 | 0.697 | 3.7 | 16.1 | 267.1 | 16.1 | 06Apr | 195.7 | -0.8 | 21.0 | 0.19 | MORP
300 | 0.715 | 0.680 | 2.6 | 18.0 | 252.9 | 18.0 | 07Apr | 190.2 | 0.6 | 18 .5 | 0.13 | MORP
080477 | 0.564 | 0.770 | 10.6 | 18.3 | 269.5 | 18.3 | 08Apr | 203.0 | 4.74 | 26.4 | 0.09 | EN
1998SH2 | 0.746 | 0.723 | 2.5 | 13.3 | 261.0 | 13.3 | 03Apr | 184.6 | 2.8 | 19.3 | 0.20 | JPL,tw
SNS | 0.646 | 0.772 | 10.7 | 209.2 | 79.2 | 29.2 | 19Apr | 197.3 | -23.8 | 22.4 | - | tw
343/HVI | 0.742 | 0.734 | 0.8 | 219.0 | 67.64 | 39.0 | 29Apr | 204.2 | -11.6 | 18.7 | 0.20 | SON
1999UZ5 | 0.515 | 0.799 | 10.3 | 226.6 | 66.7 | 46.6 | 07May | - | - | - | 0.16 | JPL
2009HS44 | 0.766 | 0.702 | 2.4 | 209.2 | 73.1 | 29.2 | 19Apr | 193.8 | -10.8 | 18.2 | 0.20 | JPL,tw
2012SW20 | 0.786 | 0.679 | 10.2 | 209.8 | 62.1 | 29.8 | 19Apr | 186.7 | -24.7 | 17.6 | 0.20 | JPL,tw
2014GN1 | 0.665 | 0.748 | 3.0 | 193.1 | 80.3 | 13.1 | 02Apr | 184.9 | -7.0 | 21.1 | 0.20 | JPL,tw
NDS | 0.645 | 0.772 | 10.9 | 187.8 | 100.6 | 187.8 | 01Oct | 196.9 | 9.6 | 22.5 | - | tw
2010EK44 | 0.645 | 0.772 | 11.2 | 180.8 | 107.6 | 180.8 | 23Sep | 191.8 | 12.7 | 22.0 | 0.02 | JPL,tw
2013TE135 | 0.569 | 0.759 | 6.0 | 182.4 | 102.9 | 182.4 | 25Sep | 185.5 | 6.1 | 23.0 | 0.12 | JPL,tw
2014EQ12 | 0.676 | 0.743 | 11.0 | 178.0 | 92.3 | 178.0 | 21Sep | 189.6 | 14.1 | 21.5 | 0.20 | JPL,tw
SDS | 0.651 | 0.770 | 9.6 | 7.0 | 281.4 | 187.0 | 30Sep | 185.1 | -17.3 | 22.2 | - | tw
1995EK1 | 0.508 | 0.776 | 8.8 | 355.5 | 296.7 | - | - | - | - | - | 0.19 | JPL
2010FD7 | 0.813 | 0.685 | 6.2 | 357.5 | 296.2 | 177.5 | 20Sep | 186.7 | -16.4 | 17.2 | 0.19 | JPL,tw
2011EF17 | 0.604 | 0.742 | 4.2 | 4.0 | 282.3 | 184.0 | 27Sep | 183.7 | -8.1 | 21.7 | 0.11 | JPL,tw
Table 4:  Meteor showers, fireballs, meteorites, and NEAs associated with NEA 2010 FD7 (J2000.0). Objects | $q$ | $e$ | $i^{\circ}$ | $\Omega^{\circ}$ | $\omega^{\circ}$ | $L_{\odot}^{\circ}$ | Date | $\alpha_{g}^{\circ}$ | $\delta_{g}^{\circ}$ | $V_{g}$ | $D$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---|---
| AU |  |  |  |  |  |  |  |  | km/s | SH |
NNS | 0.819 | 0.683 | 7.2 | 30.3 | 236.4 | 30.3 | 20Apr | 197.2 | 9.5 | 16.3 | - | tw
21/AVB | 0.691 | 0.732 | 4.2 | 21.7 | 240.4 | 21.7 | 11Apr | 185.4 | 9.6 | 16.8 | 0.20 | SH
21/AVB | 0.750 | 0.681 | 0.7 | 28.9 | 247.5 | 28.9 | 19Apr | 195.6 | -5.3 | 16.6 | 0.11 | L2
21/AVB | 0.809 | 0.684 | 3.1 | 31.8 | 239.7 | 31.8 | 22Apr | 195.8 | 0.4 | 16.4 | 0.10 | L1
21/AVB | 0.724 | 0.716 | 7.0 | 30.0 | 247.9 | 30.0 | 20Apr | 203.5 | 2.9 | 18.8 | 0.07 | J1
300 | 0.715 | 0.680 | 2.6 | 18.0 | 252.9 | 18.0 | 07Apr | 190.2 | 0.6 | 18.5 | 0.13 | MORP
650404 | 0.777 | 0.650 | 0.7 | 16.0 | 244.0 | 16.0 | 05Apr | 183.0 | 0.5 | 16.2 | 0.15 | PN
Pribram | 0.790 | 0.674 | 10.4 | 17.8 | 241.6 | 17.8 | 07Apr | 192.1 | 17.4 | 17.5 | 0.11 | P1
Neusch- | 0.792 | 0.670 | 11.4 | 17.5 | 241.2 | 17.5 | 06Apr | 192.3 | 19.5 | 17.5 | 0.12 | SP
wanstein |  |  |  |  |  |  |  |  |  |  |  |
1998SH2 | 0.746 | 0.723 | 2.5 | 13.3 | 261.0 | 13.3 | 03Apr | 184.6 | 2.8 | 19.3 | 0.15 | JPL,tw
SNS | 0.881 | 0.659 | 8.9 | 221.1 | 45.7 | 41.1 | 1May | 184.7 | -26.5 | 14.5 | - | tw
$\chi$-Virds | 0.718 | 0.725 | 1.4 | 202.9 | 70.7 | 22.9 | 12Apr | 190.0 | -7.0 | 19.1 | 0.12 | T1
670426 | 0.829 | 0.710 | 6.2 | 217.0 | 56.4 | 37.0 | 27Apr | 191.0 | -19.3 | 16.5 | 0.11 | PN
2009HS44 | 0.766 | 0.702 | 2.4 | 209.2 | 73.1 | 29.2 | 19Apr | 193.8 | -10.8 | 18.2 | 0.22 | JPL,tw
2012SW20 | 0.786 | 0.679 | 10.2 | 209.8 | 62.1 | 29.8 | 19Apr | 186.7 | -24.7 | 17.6 | 0.12 | JPL,tw
NDS | 0.866 | 0.665 | 9.2 | 134.4 | 132.4 | 134.4 | 07Aug | 169.6 | 28.8 | 14.8 | - | tw
1998FR11 | 0.801 | 0.713 | 6.6 | 130.3 | 157.9 | 130.3 | 02Aug | 184.3 | 20.5 | 11.4 | 0.22 | JPL,tw
SDS | 0.891 | 0.655 | 6.1 | 309.9 | 316.9 | 129.9 | 02Aug | 154.5 | -7.1 | 13.4 | - | tw
2011BE38 | 0.757 | 0.711 | 8.2 | 321.4 | 302.5 | 141.4 | 14Aug | 152.3 | -5.5 | 17.5 | 0.15 | JPL,tw

A search has also shown a close association of these asteroids with the
theoretical and observable showers, as well their mutual link. The orbit of
PHA 1998 SH2 at present is matching to the northern nighttime shower 21/AVB.
The orbits of asteroids 200 9HS44, 2012 SW20, 2014 GN1, and 1999 UZ5
correspond to the southern nighttime shower 343/HVI (and $chi$-Virginids).
Regarding the theoretical daytime showers, it was defined that the present-day
orbits of NEAs 2009 SM98, 2014 EQ12, 2010 EK44, 2013 TE135, and 1998 FR11 are
consistent with the northern branch of the daytime shower, while the orbits of
2010 FD7, 2011 EF17, 1995 EK1, 200 3FB5, and 2011 BE38 – with the southern
branch of the daytime shower. Consequently, possible incomings of asteroids
into the Earth’s atmosphere will occur at the period of activity of the
relevant shower and will have characteristics close to the features of this
shower. For instance, it is theoretically predicted that the date of presumed
impact of the potentially hazardous object 2010 EK44 will be 23 September, the
geocentric velocity will be 22 km/s, and the equatorial coordinates of the
point from which it will be directed to the Earth will be $\alpha_{g}$=191.8
deg. and $\delta_{g}$=12.7 deg.

5.1.1. A relationship with the meteorites

Notably that the orbits, radiants, velocities and the fall dates of Pribram
and Neuschwanstein meteorites are similar with the northern nighttime showers
of asteroids 2010 FD7 (Table 4), 2011 BE38, 2012 SW20, and 2014 EQ12. Pribram
meteorite fall in 7 April 1959 on the Czech territory (Ceplecha, 1961) and
Neuschwanstein meteorite dropped in 6 April 2002 in the territory of the
Germany-Austria (Spurny et al., 2003). The heliocentric orbits of the
meteorites are identical so it was supposed that the stream of meteorite
objects having the Earth’s crossing orbit was found (Spurny et al., 2003).
However, later Oberst et al. (2003) have shown that an assumption on a common
parent body of these meteorites is unlikely because of different
classification of the meteorites types. Furthermore, the different duration of
their cosmic rays radiation was established, for Pribram it is 19 million
years (Oberst et al., 2003). Since cometary meteoroid streams have
significantly less age then these meteorite objects very likely separated from
the parents more early than the stream was formed. Consequently, they very
probably belong to the one stream of objects however were produced by the
different parent bodies. Under this, they were detached from the parents more
early then usually the meteoroids of cometary streams are ejected from the
parent comets (Spurny et al., 2003).

Found association of these meteorites with the meteor showers related to
considered asteroids points to that the supposed stream of meteorites objects
matches with the alpha-Virginids meteoroid stream. Alongside with a huge
number of small meteoroids the asteroids of a cometary origin, i.e. extinct
cometary nuclei, are moving within the stream and all they were generated by
the one common parent body. Besides, the objects of an asteroidal origin of a
larger age’s presence in the stream, under this, their parents differ from
both the parent of the cometary objects of the stream and between themselves.

###  5.2  Asteroids associated with the $eta$-Virginid stream

As a result of a search for the observable showers (fireballs, meteors), and
NEAs close to theoretically predicted showers it was found that 6 NEAs listed
in the second section of Table 1 coincide with the meteoroid stream producing
the nighttime Northern and Southern $eta$-Virginids (11/EVI) (Sekanina, 1973,
1976; Terentjeva, 1966, 1989). Association of the potentially hazardous
asteroid 2007 CA19 included to this group with the Northern and Southern $eta$
-Virginids was previously found by Babadzhanov et al. (2015c). The Northern
and Southern branches of the theoretical daytime shower were identified with
29 and 22 meteors respectively from the MODC database. Coming from their mean
radiants positions and the activity dates it was proposed to design they as
Daytime October $eta$\- and $beta$-Virginids. Besides, Southern branch of the
theoretical daytime shower was identified with the observable Daytime
$psi$-Virginids shower (240/DFV) (Sekanina, 1976). These observable daytime
showers were identified with the theoretical daytime showers also of 6
asteroids of this sample.

The results of identification of theoretically predicted showers with the
observable showers, fireballs/meteors, and NEAs for asteroids 2014 VC10 and
2010 FJ81 are presented in Tables 5 and 6. For the rest asteroids of this
group the outcomes are identical. All designations in Tables 5 and 6 are the
same as in Tables 3 and 4.

Table 5: Meteor showers, fireballs/meteors, and NEAs associated with NEA 2014 VC10 (J2000.0). Objects | $q$ | $e$ | $i^{\circ}$ | $\Omega^{\circ}$ | $\omega^{\circ}$ | $L_{\odot}^{\circ}$ | Date | $\alpha_{g}^{\circ}$ | $\delta_{g}^{\circ}$ | $V_{g}$ | $D$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---|---
| AU |  |  |  |  |  |  |  |  | km/s | SH |
NNS | 0.458 | 0.795 | 3.3 | 357.9 | 282.9 | 357.9 | 18Mar | 185.1 | 1.5 | 26.2 | - | tw
11/EVI | 0.464 | 0.812 | 5.4 | 355.7 | 281.0 | 355.7 | 16Mar | 184.8 | 3.9 | 26.6 | 0.07 | J1
Virds | 0.365 | 0.914 | 3.8 | 348.5 | 286.5 | 348.5 | 09Mar | 178.1 | 4.4 | 31.0 | 0.17 | G
N.$\eta$-Virds | 0.495 | 0.707 | 3.7 | 357.3 | 282.4 | 357.3 | 18Mar | 185.1 | 2.3 | 23.0 | 0.10 | S2
N.$\eta$-Virds | 0.377 | 0.831 | 3.9 | 352.6 | 291.5 | 352.6 | 13Mar | 184.0 | 2.0 | 28.7 | 0.10 | T1
Virds | 0.349 | 0.820 | 6.0 | 356.0 | 297.0 | 356.0 | 16Mar | 188.0 | 1.0 | 27.8 | 0.20 | K
As.112 | 0.433 | 0.870 | 6.1 | 355.5 | 285.6 | 355.5 | 16Mar | 185.3 | 2.6 | 29.6 | 0.09 | L
140378 | 0.390 | 0.870 | 1.3 | 352.8 | 287.9 | 352.8 | 13Mar | 182.0 | 0.53 | 29.7 | 0.11 | EN
710319 | 0.537 | 0.710 | 5.6 | 358.0 | 276.9 | 358.0 | 18Mar | 184.0 | 5.7 | 22.6 | 0.14 | PN
680306 | 0.389 | 0.860 | 3.7 | 345.0 | 287.4 | 345.0 | 05Mar | 176.0 | 5.3 | 29.3 | 0.15 | PN
1995EK1 | 0.508 | 0.776 | 8.8 | 355.5 | 296.7 | - | - | - | - | - | 0.19 | JPL
2003FB5 | 0.533 | 0.788 | 5.3 | 358.4 | 288.4 | - | - | - | - | - | 0.12 | JPL
SNS | 0.427 | 0.809 | 5.0 | 174.4 | 106.4 | 354.4 | 15Mar | 180.1 | -5.3 | 27.2 | - | tw
S.$\eta$-Virds | 0.566 | 0.738 | 6.1 | 182.0 | 91.2 | 2.0 | 22Mar | 179.6 | -8.0 | 22.9 | 0.19 | S2
S. $\eta$-Virds | 0.499 | 0.706 | 2.6 | 171.1 | 101.8 | 351.1 | 11Mar | 176.1 | -1.6 | 22.9 | 0.17 | S3
S.$\eta$-Virds | 0.396 | 0.904 | 12.3 | 174.5 | 105.4 | 354.5 | 15Mar | 178.6 | -10.6 | 31.2 | 0.16 | T
As.2 | 0.455 | 0.82 | 6.0 | 175.0 | 100.0 | 355.0 | 15Mar | 177.0 | 5.0 | 26.7 | 0.09 | K
790303 | 0.366 | 0.865 | 0.2 | 162.8 | 111.1 | 342.8 | 3Mar | 172.9 | 3.0 | 30.0 | 0.16 | MORP
640315 | 0.417 | 0.900 | 12.3 | 175.0 | 105.4 | 355.0 | 15Mar | 179.0 | -10.6 | 31.0 | 0.18 | PN
660313 | 0.299 | 0.770 | 5.2 | 172.0 | 118.3 | 352.0 | 12Mar | 183.0 | -6.6 | 26.6 | 0.18 | PN
690318 | 0.39 | 0.840 | 2.8 | 177.0 | 109.4 | 357.0 | 17Mar | 185.0 | -5.0 | 28.7 | 0.10 | PN
2007CA19 | 0.483 | 0.827 | 9.6 | 174.8 | 97.6 | - | - | - | - | - | 0.15 | JPL
NDS | 0.430 | 0.807 | 4.8 | 206.7 | 74.0 | 206.7 | 20Oct | 199.3 | -3.1 | 27.1 | - | tw
29 meteors | 0.484 | 0.827 | 6.6 | 189.3 | 82.3 | 189.3 | 02Oct | 187.5 | 5.2 | 26.9 | 0.15 | MODC
SDS | 0.459 | 0.794 | 3.3 | 23.8 | 257.0 | 203.8 | 17Oct | 194.9 | -10.0 | 26.1 | - | tw
240/DFV | 0.525 | 0.650 | 2.6 | 22.3 | 258.1 | 202.3 | 15Oct | 193.7 | -9.6 | 21.1 | 0.16 | S3
22 meteors | 0.480 | 0.828 | 5.3 | 11.2 | 262.1 | 191.2 | 04Oct | 183.9 | -8.5 | 26.8 | 0.12 | MODC
Table 6:  Meteor showers, fireballs/meteors, and NEAs associated with NEA 2010 FJ81 (J2000.0). Objects | $q$ | $e$ | $i^{\circ}$ | $\Omega^{\circ}$ | $\omega^{\circ}$ | $L_{\odot}^{\circ}$ | Date | $\alpha_{g}^{\circ}$ | $\delta_{g}^{\circ}$ | $V_{g}$ | $D$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---|---
| AU |  |  |  |  |  |  |  |  | km/s | SH |
NNS | 0.396 | 0.810 | 4.0 | 342.1 | 290.5 | 342.1 | 2Mar | 173.9 | 6.6 | 27.6 | - | tw
11/EVI | 0.464 | 0.812 | 5.4 | 355.7 | 281.0 | 355.7 | 16Mar | 184.8 | 3.9 | 26.6 | 0.09 | J1
N.$\eta$-Virds | 0.495 | 0.707 | 3.7 | 357.0 | 282.4 | 357.0 | 17Mar | 185.1 | 2.6 | 23.0 | 0.17 | S2
N.$\eta$-Virds | 0.502 | 0.703 | 11.3 | 349.3 | 281.8 | 349.3 | 09Mar | 182.3 | 13.6 | 23.5 | 0.19 | S3
Virds | 0.365 | 0.914 | 3.8 | 348.5 | 286.5 | 348.5 | 09Mar | 178.1 | 4.4 | 31.0 | 0.11 | G
N.$\eta$-Virds | 0.377 | 0.831 | 3.9 | 352.6 | 291.5 | 352.6 | 13Mar | 184.0 | 2.0 | 28.7 | 0.16 | T1
As.68 | 0.346 | 0.820 | 5.5 | 331.6 | 296.8 | 331.6 | 20Feb | 167.6 | 10.2 | 28.9 | 0.08 | L
As.112 | 0.433 | 0.870 | 6.1 | 355.5 | 285.6 | 355.5 | 16Mar | 185.3 | 2.6 | 29.6 | 0.14 | L
680306 | 0.389 | 0.860 | 3.7 | 345.0 | 287.4 | 345.0 | 05Mar | 176.0 | 5.3 | 29.3 | 0.05 | PN
710319 | 0.537 | 0.71 | 5.6 | 358.0 | 276.9 | 358.0 | 18Mar | 184.0 | 5.7 | 22.6 | 0.17 | PN
140378 | 0.390 | 0.870 | 1.3 | 352.8 | 287.9 | 352.8 | 13Mar | 182.0 | 0.53 | 29.7 | 0.14 | EN
2003FB5 | 0.533 | 0.788 | 5.3 | 358.4 | 288.4 | - | - | - | - | - | 0.20 | JPL
SNS | 0.421 | 0.798 | 5.7 | 164.7 | 108.0 | 344.7 | 5Mar | 171.6 | -2.4 | 26.9 | - | tw
S.$\eta$-Virds | 0.566 | 0.738 | 6.1 | 181.3 | 91.2 | 1.3 | 22Mar | 179.1 | -8.2 | 22.9 | 0.16 | S2
S.$\eta$-Virds | 0.499 | 0.706 | 2.6 | 170.4 | 101.8 | 350.4 | 11Mar | 175.4 | -1.4 | 22.9 | 0.13 | S3
As.2 | 0.455 | 0.820 | 6.0 | 175.0 | 100.0 | 355.0 | 15Mar | 177.0 | 5.0 | 26.7 | 0.05 | K
S.$\eta$-Virds | 0.397 | 0.904 | 12.3 | 175.2 | 105.4 | 355.2 | 15Mar | 179.3 | -10.8 | 31.2 | 0.19 | T
790303 | 0.366 | 0.865 | 0.2 | 162.8 | 111.1 | 342.8 | 03Mar | 172.9 | 3.0 | 30.0 | 0.13 | MORP
640315 | 0.417 | 0.900 | 12.3 | 175.0 | 105.4 | 355.0 | 15Mar | 179.0 | -10.6 | 31.0 | 0.19 | PN
680225 | 0.360 | 0.820 | 15.5 | 156.0 | 113.5 | 336.0 | 24Feb | 165.0 | -7.5 | 28.9 | 0.19 | PN
690318 | 0.390 | 0.840 | 2.8 | 177.0 | 109.4 | 357.0 | 17Mar | 185.0 | -5.0 | 28.7 | 0.20 | PN
750228 | 0.415 | 0.830 | 0.4 | 159.0 | 107.1 | 339.0 | 27Feb | 168.5 | 4.6 | 28.0 | 0.13 | PN
2007CA19 | 0.483 | 0.827 | 9.6 | 174.8 | 97.6 | - | - | - | - | - | 0.10 | JPL
NDS | 0.423 | 0.796 | 5.5 | 200.2 | 72.4 | 200.2 | 13Oct | 192.9 | 0.3 | 26.9 | - | tw
29 meteors | 0.484 | 0.827 | 6.6 | 189.3 | 82.3 | 189.3 | 02Oct | 187.5 | 5.2 | 26.9 | 0.07 | MODC
SDS | 0.397 | 0.809 | 4.0 | 23.0 | 249.6 | 203.0 | 16Oct | 190.9 | -8.7 | 27.6 | - | tw
240/DFV | 0.525 | 0.650 | 2.6 | 22.3 | 258.1 | 202.4 | 15Oct | 193.7 | -9.6 | 21.1 | 0.20 | S3
22 meteors | 0.480 | 0.828 | 5.3 | 11.2 | 262.1 | 191.2 | 04Oct | 183.9 | -8.5 | 26.8 | 0.09 | MODC

As seen from Tables 5 and 6, a mutual link of asteroids is also revealed. The
present-day orbits of 2003 FB5 and 1995 EK1 correspond to the nighttime shower
Northern $eta$-Virginids while the orbit of potentially hazardous asteroid
2007 CA19 is close to the nighttime shower Southern $eta$-Virginids. Moreover,
their possible entering into the Earth’s atmosphere will be described by the
features of this showers. For instance, it is theoretically predicted that the
period of presumed impact of 2007 CA19 is around of 5 March, the geocentric
velocity is within 27-30 km/s, and the equatorial coordinates of the point
from which it will be directed to the Earth are within $\alpha_{g}$=170-180∘
and $\delta_{g}$=5- $-10^{\circ}$. Additionally, a lot of fireballs consistent
with the nighttime Northern and Southern $eta$-Virginids showers confirms it
activity.

It may be concluded that asteroids under study have a related association with
the meteoroid stream producing four active meteor showers. Found relations and
the comet-like orbits point to a cometary origin of these objects which might
be considered as the parent bodies of the stream or large-sized extinct
fragments of the comet-progenitor of the stream.

###  5.3 Asteroids associated with the $nu$-Virginid stream

Association between the stream generating the Northern and Southern
$nu$-Virginids and 5 asteroids listed in the third section of Table 2 is
found. As a result of a search the theoretical nighttime showers of the
asteroids were identified with these showers found by Terentjeva (1966, 1989).
The shower 124/SVI (EDM1, Rudawska et al. (2015)) very likely is consistent
with the Southern $nu$-Virginids shower. The results for asteroids 2013 CU82
and 2013 TR13 are given in Tables 7 and 8 where all designations are the same
as in Tables 3 and 4. For the rest asteroids of this set the outcomes are
identical. Note, the connection of asteroid 2004 CK29 with this stream was
previously revealed by Babadzhanov et al. (2012).

Table 7:  Meteor showers, fireballs, and NEAs associated with NEA 2013 CU82 (J2000.0). Objects | $q$ | $e$ | $i^{\circ}$ | $\Omega^{\circ}$ | $\omega^{\circ}$ | $L_{\odot}^{\circ}$ | Date | $\alpha_{g}^{\circ}$ | $\delta_{g}^{\circ}$ | $V_{g}$ | $D$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---|---
| AU |  |  |  |  |  |  |  |  | km/s | SH |
NNS | 0.555 | 0.777 | 9.05 | 350.2 | 270.7 | 350.2 | 10Mar | 176.8 | 16.5 | 24.3 | - | tw
N.$\nu$-Virds | 0.394 | 0.822 | 5.6 | 335.9 | 289.6 | 335.9 | 24Feb | 167.4 | 11.2 | 27.6 | 0.17 | T
N.$\nu$-Virds | 0.521 | 0.790 | 2.3 | 348.8 | 274.4 | 348.8 | 9Mar | 173.0 | 6.0 | 24.8 | 0.13 | T1
710319 | 0.537 | 0.710 | 5.6 | 358.0 | 276.9 | 358.0 | 18Mar | 184.0 | 5.7 | 22.6 | 0.20 | PN
SNS | 0.582 | 0.766 | 9.59 | 173.0 | 88.0 | 353.0 | 13Mar | 168.7 | -8.6 | 23.5 | - | tw
124/SVI | 0.576 | 0.753 | 2.8 | 170.6 | 88.5 | 350.6 | 11Mar | 169.1 | -1.0 | 22.5 | 0.12 | EDM1
680330 | 0.684 | 0.870 | 3.9 | 189.0 | 71.3 | 9.0 | 29Mar | 177.0 | -5.4 | 22.6 | 0.18 | PN
750321 | 0.710 | 0.680 | 6.7 | 180.0 | 73.9 | 0.0 | 20Mar | 168.5 | -7.7 | 18.8 | 0.19 | PN
NDS | 0.582 | 0.766 | 9.59 | 173.0 | 88.0 | 173.0 | 15Sep | 174.8 | 19.7 | 23.5 | - | tw
2002BK25 | 0.576 | 0.749 | 11.9 | 156.5 | 103.6 | 156.5 | 29Aug | 163.8 | 23.5 | 23.1 | 0.06 | JPL,tw
SDS | 0.555 | 0.777 | 9.0 | 351.8 | 269.1 | 171.8 | 14Sep | 166.9 | -6.30 | 24.2 | - | tw
2002TZ59 | 0.410 | 0.842 | 16.5 | 7.4 | 249.7 | 187.4 | 1Oct | 172.0 | -12.4 | 29.3 | 0.22 | JPL,tw
2004CK39 | 0.393 | 0.829 | 12.3 | 359.5 | 265.1 | - | - | - | - | - | 0.19 | JPL
Table 8:  Meteor showers, fireballs/meteors, and NEAs associated with NEA 2013 TR13 (J2000.0). Objects | $q$ | $e$ | $i^{\circ}$ | $\Omega^{\circ}$ | $\omega^{\circ}$ | $L_{\odot}^{\circ}$ | Date | $\alpha_{g}^{\circ}$ | $\delta_{g}^{\circ}$ | $V_{g}$ | $D$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---|---
| AU |  |  |  |  |  |  |  |  | km/s | SH |
NNS | 0.439 | 0.803 | 0.3 | 336.4 | 285.0 | 336.4 | 25Feb | 164.9 | 6.8 | 26.6 | - | tw
N.$\nu$-Virds | 0.394 | 0.822 | 5.6 | 335.9 | 289.6 | 335.9 | 24Feb | 167.4 | 11.2 | 27.6 | 0.11 | T
N.$\nu$-Virds | 0.521 | 0.79 | 2.3 | 348.8 | 274.4 | 348.8 | 09Mar | 173.0 | 6.0 | 24.8 | 0.09 | T1
As.68 | 0.346 | 0.820 | 5.5 | 331.6 | 296.8 | 331.6 | 20Feb | 167.6 | 10.2 | 28.9 | 0.16 | L
800222 | 0.498 | 0.754 | 2.8 | 332.5 | 278.9 | 332.5 | 21Feb | 160.2 | 11.9 | 24.2 | 0.16 | MORP
810210 | 0.355 | 0.822 | 4.4 | 320.9 | 294.8 | 320.9 | 09Feb | 156.3 | 13.9 | 28.6 | 0.14 | MORP
680306 | 0.389 | 0.86 | 3.7 | 345.0 | 287.4 | 345.0 | 05Mar | 176.0 | 5.3 | 29.3 | 0.19 | PN
2013CU82 | 0.563 | 0.744 | 10.8 | 317.7 | 303.2 | - | - | - | - | - | 0.20 | JPL
SNS | 0.474 | 0.787 | 2.1 | 159.7 | 101.7 | 339.7 | 28Feb | 165.3 | 3.9 | 25.6 | - | tw
S.$\nu$-Virds | 0.387 | 0.85 | 0.3 | 160.4 | 109.1 | 340.4 | 01Mar | 170.0 | 4.0 | 28.5 | 0.16 | T
As.65 | 0.427 | 0.85 | 1.6 | 150.6 | 104.3 | 330.6 | 19Feb | 158.8 | 7.3 | 28.4 | 0.12 | L
840223 | 0.515 | 0.733 | 8.4 | 153.2 | 97.6 | 333.2 | 21Feb | 155.9 | -7.0 | 23.7 | 0.19 | MORP
750228 | 0.415 | 0.83 | 0.4 | 159.0 | 107.1 | 339.0 | 27Feb | 168.5 | 4.6 | 28.0 | 0.10 | PN
NDS | 0.476 | 0.786 | 1.9 | 182.4 | 79.0 | 182.4 | 25Sep | 178.2 | 3.0 | 25.5 | - | tw
2002BK25 | 0.576 | 0.749 | 11.9 | 156.5 | 103.6 | 156.5 | 29Aug | 163.8 | 23.5 | 23.1 | 0.21 | JPL,tw
SDS | 0.439 | 0.803 | 0.3 | 5.8 | 255.6 | 185.8 | 29Sep | 178.6 | 0.3 | 26.7 | - | tw
24 meteors | 0.426 | 0.798 | 8.2 | 12.6 | 243.9 | 192.6 | 05Oct | 179.6 | -8.0 | 28.4 | 0.15 | MODC
2002TZ59 | 0.41 | 0.842 | 16.5 | 7.4 | 249.7 | 187.4 | 1Oct | 172.0 | -12.4 | 29.3 | 0.20 | JPL,tw
2004CK39 | 0.393 | 0.829 | 12.3 | 359.5 | 265.1 | - | - | - | - | - | 0.20 | JPL

The theoretically predicted northern branch of the daytime shower doesn’t
identify with any known shower. The southern branch of the daytime shower was
identified with 24 meteors from the MODC database, their mean radiants
positions and the activity dates allow classifying them as the Daytime October
$beta$-Virginids (Table 8). As the theoretical daytime shower of the asteroids
belonging to the $eta$ -Virginids family were also identified with the Daytime
October $beta$-Virginids it may be concluded that the Virginid complex in fact
includes a lot of close meteor showers and subshowers.

As seen, a mutual association of asteroids is also established. The present-
day orbit of 2013 CU82 corresponds to the northern branch of nighttime shower,
the potentially hazardous asteroid 2002 BK25 relates to the northern branch of
daytime shower, and asteroids 2002 TZ59 and 2004 CK39 match to the southern
branch of daytime shower. Presumed impacts of these asteroids will have the
features similar to who’s of the relevant showers, namely, the identical
dates, velocities and the coordinates of positions from which the entering
will be realized. Particularly, for the potentially hazardous asteroid
2002BK25 the coordinates of the position from which it will be directed to the
Earth are $\alpha_{g}$=163.8∘ and $\delta_{g}$=23.5∘, the geocentric velocity
is 23.1 km/s, and the date is 30 August.

Found association with the stream and active showers confirms that asteroids
under consideration having the comet-like orbits have produced meteoroids,
from which the stream was formed, during very long period, hence they might be
at present extinct comets.

###  5.4 Asteroids associated with the $mu$-Virginid stream

It was defined that four asteroids given in the fourth section of Table 2
relate to the meteoroid stream producing the nighttime Northern and Southern
$mu$-Virginids (Cook, 1973; Sekanina, 1973, 1976; Terentjeva, 1966, 1989). The
results of identification of the theoretical and observable showers,
fireballs, and NEAs for asteroids 2010 XD11 and 2010 GO33 are given in Tables
9 and 10 where all designations are the same as in Tables 3 and 4. For the
rest asteroids of this set the outcomes are identical.

Table 9: Meteor showers, fireballs, and NEAs associated with NEA 2010 XD11 (J2000.0). Objects | $q$ | $e$ | $i^{\circ}$ | $\Omega^{\circ}$ | $\omega^{\circ}$ | $L_{\odot}^{\circ}$ | Date | $\alpha_{g}^{\circ}$ | $\delta_{g}^{\circ}$ | $V_{g}$ | $D$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---|---
| AU |  |  |  |  |  |  |  |  | km/s | SH |
NNS | 0.356 | 0.839 | 5.3 | 19.8 | 294.4 | 19.8 | 09Apr | 210.6 | -7.8 | 29.3 | - | tw
N.$\mu$-Virds | 0.530 | 0.830 | 10.0 | 35.0 | 280.0 | 35.0 | 25Apr | 221.0 | -5.0 | 29.0 | 0.20 | C
N.Virds | 0.278 | 0.785 | 4.8 | 11.9 | 310.3 | 11.9 | 01Apr | 210.4 | -8.5 | 27.4 | 0.15 | S3
N.$\mu$-Virds | 0.357 | 0.885 | 2.2 | 20.5 | 291.7 | 20.5 | 10Apr | 209.0 | -10.0 | 30.8 | 0.08 | T1
220495 | 0.499 | 0.790 | 4.1 | 31.7 | 277.5 | 31.7 | 21Apr | 215.0 | -8.9 | 25.1 | 0.17 | EN
680330 | 0.270 | 0.900 | 9.5 | 9.0 | 302.4 | 9.0 | 29Mar | 206.0 | -3.9 | 33.4 | 0.14 | PN
SNS | 0.325 | 0.853 | 5.5 | 196.4 | 117.8 | 16.4 | 06Apr | 205.8 | -15.1 | 30.3 | - | tw
651/OAV | 0.373 | 0.842 | 4.7 | 197.4 | 109.8 | 17.4 | 07Apr | 202.0 | -13.5 | 28.9 | 0.11 | J1
(S.$\mu$-Virds?) |  |  |  |  |  |  |  |  |  |  |  |
S.Virds | 0.312 | 0.828 | 0.0 | 183.7 | 121.8 | 3.7 | 24Mar | 197.4 | -7.4 | 29.2 | 0.16 | S2
S.$\mu$-Virds | 0.264 | 0.864 | 3.5 | 194.5 | 126.0 | 14.5 | 04Apr | 208.0 | -14.0 | 31.5 | 0.12 | T1
865 | 0.373 | 0.715 | 1.2 | 193.5 | 120.3 | 13.5 | 03Apr | 205.4 | -11.8 | 24.2 | 0.16 | MORP
1011 | 0.256 | 0.949 | 5.8 | 188.0 | 122.1 | 8.0 | 28Mar | 299.5 | -11.9 | 35.8 | 0.13 | MORP
680411 | 0.375 | 0.850 | 4.9 | 201.0 | 109.4 | 21.0 | 11Apr | 205.0 | -15.7 | 28.9 | 0.08 | PN
NDS | 0.329 | 0.851 | 5.2 | 251.5 | 62.7 | 251.5 | 03Dec | 237.4 | -15.9 | 30.1 | - | tw
- | Observable showers/objects not found
SDS | 0.356 | 0.839 | 5.3 | 68.7 | 245.5 | 248.7 | 01Dec | 233.8 | -23.9 | 29.2 | - | tw
2003WW26 | 0.482 | 0.798 | 6.3 | 57.7 | 254.6 | 237.7 | 20Nov | 228.8 | -25.2 | 25.7 | 0.14 | JPL,tw
Table 10:  Meteor showers, fireballs, and NEAs associated with NEA 2010 GO33 (J2000.0). Objects | $q$ | $e$ | $i^{\circ}$ | $\Omega^{\circ}$ | $\omega^{\circ}$ | $L_{\odot}^{\circ}$ | Date | $\alpha_{g}^{\circ}$ | $\delta_{g}^{\circ}$ | $V_{g}$ | $D$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---|---
| AU |  |  |  |  |  |  |  |  | km/s | SH |
NNS | 0.713 | 0.703 | 10.5 | 45.4 | 251.8 | 45.4 | 6May | 220.8 | 2.6 | 19.6 | - | tw
N.$\mu$-Virds | 0.696 | 0.748 | 3.3 | 43.2 | 253.7 | 43.2 | 3 May | 214.0 | -8.0 | 20.1 | 0.13 | T1
454/MPV | 0.650 | 0.744 | 10.4 | 41.6 | 259.7 | 41.6 | 2May | 220.2 | 0.3 | 21.7 | 0.09 | EDM2
(N.$\mu$-Virds?) |  |  |  |  |  |  |  |  |  |  |  |
307 | 0.660 | 0.563 | 11.9 | 40.5 | 267.4 | 40.5 | 30Apr | 224.7 | 4.0 | 18.0 | 0.19 | MORP
730503 | 0.636 | 0.630 | 9.6 | 42.0 | 267.5 | 42.0 | 2May | 224.0 | -1.4 | 19.4 | 0.17 | PN
SNS | 0.680 | 0.717 | 10.6 | 221.0 | 76.2 | 41.0 | 1May | 207.1 | -28.8 | 20.6 | - | tw
S.$\mu$-Virds | 0.720 | 0.696 | 2.0 | 223.1 | 72.3 | 43.1 | 3May | 210.0 | -16.0 | 18.6 | 0.16 | T1
690512 | 0.800 | 0.680 | 6.0 | 231.0 | 63.5 | 51.0 | 11May | 210.0 | -25.0 | 17.1 | 0.15 | PN
2011VG9 | 0.508 | 0.776 | 1.3 | 236.1 | 65.8 | - | - | - | - | - | 0.25 | JPL
NDS | 0.675 | 0.719 | 10.6 | 194.2 | 103.0 | 194.2 | 7Oct | 204.0 | 7.8 | 20.8 | - | tw
- | Observable showers/objects not found
SDS | 0.716 | 0.703 | 10.5 | 9.3 | 288.0 | 189.3 | 3Oct | 188.5 | -22.9 | 19.6 | - | tw
- | Observable showers/objects not found

As was mentioned, $mu$-Virginids is denoted in the IAU MDC as 47/DLI
(Porubcan, Gavajdova (1994) (P)). However, according to the radiant position
the shower should be named as $delta$-Librids, moreover the abbreviation DLI
also points to this definition. While the $mu$-Virginids should be named as
MVI. The radiants and orbits of the 47/DLI given by Rudawska et al. (2015)
(EDM1) and Jenniskens et al. (2016) (J1) are more consistent with the
$xi$1-Librid shower. By this reason, although the 47/DLI was identified with
the theoretical shower, three references P, EDM1 and J1 are excluded from the
Tables 9 and 10. The observable October $alpha$-Virginid shower (651/OAV,
Jenniskens et al. (2016) (J1)) was identified with the southern branch of
theoretical night-time shower of asteroid 2010 XD11 (Table 9), however the
shower should not be classified as October since it value of the Solar
longitude corresponds to 7 April. So that we refer the shower 651/OAV to the
Southern $mu$-Virginid shower.

A mutual relationship of the asteroids also is found. The present-day orbit of
2011 VG9 corresponds to the southern branch of nighttime shower, and the orbit
of 2003 WW26 - to the southern branch of daytime shower. At the case of
possible impacts with the Earth, for example for 2003 WW26, the coordinates of
the point of entering into the Earth’s atmosphere will be $\alpha_{g}$ =228.8∘
and $\delta_{g}$=-25.2∘, the geocentric velocity $V_{g}$=25.7 km/s and the
date - 20 November.

Theoretical daytime showers were not identified with observables, because
showers with such features are yet missed in the used databases of
observations. However, identification of the theoretical nighttime showers
allows suggesting the related association of the asteroids with the stream and
these showers. The asteroids very likely have a cometary nature and might be
extinct fragments of the parent comet of the $mu$-Virginids meteoroid stream.

##  6 Discussion

Thus, the existence of active meteor showers producing by the
$alpha-,eta-,nu-$ and $mu$-Virginid meteoroid streams, and their relationship
with four groups of asteroids are found. These streams and substreams, and
generating by them meteor showers relate to the Virginid complex. Revealed
association is very strong indicator of a cometary origin of 29 NEAs moving on
the comet-like orbits. In this case and taking into account that each group
contains a few of asteroids several scenario of their formation might be
suggested. 1. The largest object is the extinct parent Jupiter family comet of
the stream, and the rest objects are its fragments also extinct at present. 2.
All objects of each group were formed as a result of a decay of the larger
comet-progenitor of the relevant stream. 3. As a result of a break-up of the
one giant parent comet of the Virginid complex smaller comets were produced
which during evolution under gravitational and non-gravitational perturbations
generated the substreams of the Virginid complex. These inactive comets at
present compose four groups under consideration.

However, whatever the mechanism of formation, this leads to an unambiguous
conclusion, namely, the Virginid complex includes four families that we
identified. Each of them consists of the meteoroid stream generating active
showers and contains from 14 ($alpha$-Virginids stream) to 4 ($mu$-Virginid
substream) the large-sized extinct remnants of parent comets (or comet).
Besides, found association with the known meteorites points to that the large-
sized objects having more early asteroidal origin should be in the stream
which are capable to produce meteorites in future. The asteroids of a cometary
nature prove that the large bodies with the size from 110 m to 1.2 km are the
constituent part of the stream. Asteroid 2002 BK25 with the diameter of 1.22
km is already classified as the potentially hazardous object in this complex.

##  7 Conclusions

A new Virginids asteroid-meteoroid complex is established as a result of
performed investigation. The complex includes several meteoroid streams and
substreams producing the active meteor showers confirmed by the observations.
Besides, the related association of 29 near-Earth’s asteroids with the complex
is found. This and the comet-like orbits allow suggesting that asteroids with
high probability have a cometary origin. In this case they might be considered
as the fragments of a parent comet of the Virginid complex which are presently
in extinct or dormant stage.

The presented study again confirm that the meteoroid streams consist both of
small mm sized particles and large bodies of decameter size and more which
represent potentially hazard for the Earth and the space missile technology.
Our results allow forecasting the parameters of an incoming of such bodies
into the Earth’s atmosphere that is need for a development of the mitigation
strategy for preventing the consequences.

The results show that the method of identification of extinct comets among the
near-Earth’s asteroids is effective and yields the reliable outcomes. For more
sure additional observational data for the Virginid complex showers need in
order to obtain the dynamical and physical properties of meteoroids of the
streams and substreams of this complex which is associated with 29 objects of
a cometary nature.

A search for other presumed existent large fragments of parent comets should
be continued in future. They also presently are extinct and might be found
among both known NEAs and new discovered ones.

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