Issue |
A&A
Volume 507, Number 2, November IV 2009
|
|
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Page(s) | 1067 - 1072 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/200912936 | |
Published online | 24 September 2009 |
A&A 507, 1067-1072 (2009)
Near-Earth asteroids among the Iota Aquariids meteoroid stream
P. B. Babadzhanov1 - I. P. Williams2 - G. I. Kokhirova1
1 - Institute of Astrophysics, Dushanbe 734042, Tajikistan
2 - Queen Mary University of London, E1 4NS, UK
Received 20 July 2009 / Accepted 10 September 2009
Abstract
It is shown that the near-Earth asteroids 2002JS2, 2002PD11, and
2003MT9 have very similar orbits to each other and probably a common
origin. We investigate the orbital evolution of these asteroids under
the perturbing action of the planets and calculated the theoretical
shower parameters for any meteor shower that may be associated with
these asteroids. Finally we searched the existing catalogues of meteor
showers and fireballs, and found that activity has been observed
corresponding to each of the theoretically predicted shower. We
conclude that this asteroid-meteoroid complex is the result of a
cometary break-up.
Key words: meteors, meteoroids - minor planets, asteroids
1 Introduction
In recent years there has been a significant amount of popular interest in near-Earth objects (NEOs) because of the potential threat that they represent to the Earth through collisions. By definition, an NEO has an orbit with a perihelion distance that is short enough to allow possible close approaches to the Earth. Lists of known NEOs, together with their orbital elements, can be found on web sites, and a review of their properties is given by Binzel & Lupishko (2006). Since the dynamical lifetimes of objects on such orbits are less than 10 Myr (Morbidelli & Gladman 1998), they must have originated in populations of bodies currently found in the Solar System.
The two most obvious populations are the main-belt asteroids and short-period comets. The difference in composition between these two populations suggests that mitigation strategy that might be employed is rather different, depending on which of the two possible origins the particular threatening object had. The first is primarily composed of stone and metal while the second is primarily ice. Their internal strength and vaporization temperature are different, implying a rather different reaction to the various proposed mitigation strategies.
For many objects, distinguishing between comets and asteroids is easy, a comet becomes active when close to the Sun, forming a visible tail while an asteroid shows no signs of such an activity. However, a dormant comet nucleus may be covered by a thick dust mantle, thus making its appearance through telescopes very similar to that of an asteroid. The dust mantle may also prevent sublimation so that activity ceases. The problem of distinguishing between a dormant comet and an asteroid is not confined to the NEO population, as discussed for example in the outer asteroid belt by Fitzsimmons et al. (1994), Williams (1997). Near the end of their lives, a comet nucleus may also fragment, leaving several small objects on very similar orbits to each other (Jenniskens & Vaubaillon 2008), none showing any signs of cometary activity and all classed as asteroids.
There have been numerous attempts to determine the fraction of extinct comets among the NEO population, for example by considering properties such as density and shape. In this paper we take a different approach. Whipple (1951) first showed that sublimation of cometary ices would cause an outflow of gasses that could carry small grains out with it through drag forces. Such grains would have a speed relative to the comet nucleus that is much less than the orbital speed and so would move on similar orbits to the parent, thus forming a meteoroid stream. Such a meteoroid stream would be observed on Earth as a meteor shower provided one of the nodal distances of the stream was close to 1 AU, since the Earth could then pass through stream. This has been regarded as the main mechanism of stream formation since that date (see e.g. Williams 2001). However, Jenniskens (2004) suggested that the fragmentation of a comet nucleus could also lead to the formation of a stream, thus reviving earlier theories based on the observations of comet Biela in 1846 (for a discussion of early progress, see Williams 2004). The relationship between 3D/Biela and the Andromedids is discussed in Jenniskens & Vaubaillon (2007). It is also possible that a meteoroid stream can be formed through mutual collisions between asteroids. This subject was reviewed by Obrubov (1999). Williams (1993) claimed that streams formed in this way would contain far less mass and be far more diffuse than those from cometary origin. There are a number of NEOs that have similar orbits to meteoroid streams. The similarity between the orbits of the Taurid meteoroid complex and a number of asteroids was first discussed by Steel et al. (1991). Porubcan et al. (2004) reviewed the whole subject of asteroids moving on similar orbits to meteoroid streams, though at that time, with the exception of the Taurid complex, they found no more than one asteroid associated with any given stream. The Taurid complex has also been revised by Porubcan et al. (2006), Babadzhanov et al. (2008a). Since the review of Porubcan et al. (2004), there have been a number of advances, the most notable perhaps being NEO 2003EH1 and its association with the Quadrantid shower (Jenniskens 2004; Williams et al. 2004), while Babadzhanov & Williams (2007) found meteor showers associated with 2000PG3 and Babadzhanov et al. (2008b) found that 4 NEOs were related to the Piscids meteoroid stream. Jenniskens & Vaubaillon (2008) showed that the Kappa Cygnids had a similar origin. An overview of the topic is given in Jenniskens (2008). We contend that the vast majority of NEOs found on orbits similar to those of meteoroid streams formed through the fragmentation of a cometary nucleus as discussed by Jenniskens & Vaubillion (2008) and that only a tiny minority arises through inter asteroid collisions.
We thus assume that any NEO moving on an orbit similar to those of comets and have a meteoroid stream associated with it is likely to be of cometary origin and that this can be a meaningful test of the probable cometary nature of an NEO. Where there are multiple asteroids moving on a similar orbit to a meteoroid stream, the above conclusion would appear to be even stronger. Hence, in this paper we search through the list of known NEOs for sets of objects moving on similar orbits. Having located such a set, we investigate whether or not there are meteor showers that might be associated with this set.
2 A search for NEOs moving on similar heliocentric orbits to each other
The orbital elements of 3143 NEOs known on 2005 January 1 can be found at http://newton.dm.unipi.it/neodys/neodys.cat,
and this data set forms the basis of our search for groups of NEOs with
orbits that are similar to each other. An important tool for
quantifying
the differences between two orbits was developed by Southworth &
Hawkins (1963) and is based on the square of the differences between the orbital elements in phase-space. The expression they found,
,
is given by
![]() |
= | ![]() |
|
![]() |
|||
![]() |
(1) |
where subscripts 1 and 2 relate to these two orbits that are being compared, e is the eccentricity, q=a(1-e) is the perihelion distance, a is the semi-major axis, i is the inclination,



The longitude of the ascending node
and the argument of perihelion
change periodically over a reasonable time scales so that
can become large simply by these changes. This makes the above
criterion unsuitable if orbits are to be compared over a long time
interval. Asher et al. (1993) proposed a simplified D criterion that avoided this, namely
![]() |
(2) |
which is more acceptable for orbital similarity of two orbits. The procedure generally used to find meteor streams in a data set is based upon an iterative procedure used by Sekanina (1970). Full details can be found also in Arter & Williams (1997). However as the numbers of NEOs with a similar orbit is likely to be small a simplified version can be used. By looking at Eq. (2), we see that a necessary condition for D<0.2 is that the difference in eccentricity is less than 0.2. Similarly the difference in semi-major axis has to be less than 0.6. With such filters it is relatively straight forward to identify sets of NEOs satisfying the criterion that D as given by Eq. (2) is less than 0.2. We found that the 3 asteroids, 2002JS2, 2002PD11, and 2003MT9 have differences in orbital elements that were less than the minimum separation laid down (i.e. D<0.2) and so may be assumed to be associated with each other.
The calculated values of the D criterion for the relative pairings of these objects are given in Table 1. It can be seen that the value of the D for any pair of these asteroids range from 0.04 to 0.16 indicating strongly that all are on very similar orbits.
Table 1: The values of the simplified D criterion.
The orbital elements of these three asteroids are given in Table 2 (equinox 2000.0). We also give other useful information about these asteroids in the same table. and
are the nodal distances of the ascending and descending nodes at the
present time. From these values we see that if a meteoroid stream had
these current values, it would not produce a meter shower as the
Earth does not intersect the current orbit.
Table 2: Orbital elements of the three near-Earth asteroids.
An other useful parameter is Tj is the Tisserand invariant and is given relative to Jupiter by
![]() |
(3) |
where aj = 5.2 AU is the semi-major axis of the Jupiters orbit. Kresak (1954) originally suggested that for comets 2.08 < Tj

The final two parameters given in Table 2 are the absolute magnitude H and the diameter d of each asteroid. The diameter was calculated using the expression (Bowell & Lumme 1982)
![]() |
(4) |
where p is the albedo. Asteroids of cometary origin are very dark and have very low values of their albedo, usually in the range from 0.02 to 0.12 (Jewitt 1992). In Table 2, the values of d were obtained assuming an albedo of 0.07.
![]() |
Figure 1:
The heliocentric distance of the ascending node |
Open with DEXTER |
3 The orbital evolution of the NEOs
As mentioned already, the orbits of NEOs evolve on a rapid time-scale because of their location in the Solar system. In most cases this evolution thus can be represented as a periodic change with minor oscillations about a sinusoidal curve. This oscillation was called ``nutation cycle'' in Jenniskens (2006). Examples of such evolution can be found in Wu & Williams (1992), Williams & Wu (1993), Babadzhanov et al. (2008a,b).
As meteoroids are ejected from their parent body with a range of
different velocities (all, as mentioned earlier, much less than
the orbital velocities) they will initially move on orbits that are
similar, but not identical to that of the parent. Any difference in the
semi-major axes is reflect in a corresponding change in the orbital
periods between the meteoroids and their parent body so that some
meteoroids lag behind the parent body more and more, while others,
overtaking it, spread along the entire orbit and form a complete loop
in a comparatively short time (Williams 1995).
Because the meteoroids occupy various positions relatively of the
parent body, particularly in true anomaly, in any given time, they
experience different planetary perturbations and so have differing
rates of orbital evolution. This means in particular that the rates and
cycles of variations in the angular orbital elements (the argument of
perihelia ,
the longitude of the ascending node
,
and the inclination to the ecliptic i)
will be different for different meteoroids. As a result, within
one such cycle, the stream meteoroids will be found on orbits similar
to all evolutionary tracks of their parent body.
Table 3: Meteor showers associated with the NEA 2002JS2.
In order to produce a meteor shower, the Earth must intersect the
meteoroid stream. The Earths orbit can only be intersected by those
stream meteoroids which have a nodal distance of about 1 AU,
i.e. it should be fulfilled the following condition:
![]() |
(5) |
In general there are 4 possible values of



In order to determine the locations of these intersections with the Earth's orbit, it is necessary to know the values of q and e at all times during one cycle of variation of the argument of perihelion. To obtain these values, it is necessary to integrate the orbit of the parent body back in time. Any of the numerical methods currently in use to follow the formation and evolution of a meteoroid stream (e.g. Wu & Williams 1993; Vaubaillon et al. 2005) are suitable, but the computational effort involved and the resulting level of detail produced varies from method to method. Hence the most efficient method to use depends on the results required and the type of orbit. For the two NEOs NEAs 2002JS2 and 2002PD11, we have used the Halphen-Goryachev integration method (Goryachev 1937) to calculate the secular variations of the orbital elements as this was shown by Babadzhanov (2001) to be quite efficient for integrating this type of orbits. NEA 2003MT9 moves on an orbit that is in 3:1 resonance with Jupiter. This potentially makes secular variational methods unsuitable for integration since the method depends on averaging the perturbations over one orbit. When resonance is present certain configurations can occur more frequently than others, making averaging over an orbit difficult. Hence, the computationally more expensive method of Everhart (1974) was used, with gravitational perturbations from the eight planets and Pluto being included, though it turns out that the evolution is very similar to that of the other two NEA's. The nutation cycle equal to one cycle of variation of the argument of perihelion for NEAs 2002JS2, 2002PD11, and 2003MT9 is 9625, 7350, and probably more than 12 000 years respectively.
Table 4: Meteor showers associated with the NEA 2002PD11.
Table 5: Meteor showers associated with the NEA 2003MT9.
In Fig. 1 we show the dependences of the heliocentric distances of the ascending node
and descending node
against
the argument of perihelion over one cycle of the variation in the
argument of perihelion for each of the 3 asteroids. From these
figures we see that each of these asteroids intersects the Earths orbit
four times during one such cycle. It is also interesting to note
that for each of the asteroids the relevant values of
are very similar. In fact all the crossings take place at locations where the value of
lies within the following ranges: 58
-63
,
117
-122
,
222
-246
,
and 294
-318
.
Because all three NEOs produce four locations where crossing of their
orbit with the Earths orbit occurs, it is theoretically possible
that a meteoroid stream associated with any of these asteroids can
produce two day-time and two night-time meteor showers. The orbital
elements, the position of the radiant (right ascention
and declination
), the geocentric velocity
(km s-1), the solar longitude
,
and the corresponding dates of maximum activity, of the possible meteor
showers associated with each of the three asteroids can be calculated
from the data above. The results of these calculations are given in
Tables 3-5,
where all values of the theoretical showers are in bold fonts
(equinox 2000.0). The table also contains the corresponding data
for possible observational counterpart, the derivation of which we
describe in the next section.
4 Search for meteor showers associated with NEOs 2002JS2, 2002PD11, and 2003 MT9
The orbital elements of theoretical meteoroid streams associated
with the three NEAs 2002JS2, 2002PD11, and 2003MT9 and also the
parameters of any related theoretical meteor showers were derived in
the previous section. It is instructive to find real meteor showers
with elements close to the theoretically predicted values. We regard
the theoretical and observational showers to be similar if the
following conditions are satisfied. The positions of the radiants have
to be closer than
in right ascention and
in declination. The difference in geocentric velocity has to be less than 5 km s-1 and the time of maximum activity within 15 days of each other. Finally, we adopted the value of
is the Southworth & Hawkins criterion given earlier has to be less than 0.25.
The data from the following published catalogues of observed meteor and fireball showers was used to find observational counterparts to the theoretical showers: Cook (1973) (indicated by C), Kashcheev et al. (1967) (K), Sekanina (1973) (S2), Sekanina (1976) (S3), Gajdosh & Porubcan (2004) (G), Cannon (2005) (C1), Betlem et al. (2001) (DMS), Porubcan & Gavajdova (1994) (PG) as well as other data sets circulated privately. The observational counterparts (meteor and fireball showers, and associations) that we found are given in Tables 3-5 (equinox 2000.0). In these tables the numbers and codes of observed showers are given according to the IAU Working List of Meteor Showers.
Matches were found for all the theoretical showers with the
exception of one of the theoretical showers associated with
NEA 2003MT9 and the values of
given in all three tables show values generally significantly less than
our adopted critical value, indicating a satisfactory agreement between
the predicted and observed showers. The most prominent match is between
the active night-time Northern and Southern Iota-Aquariids fireball
showers (Gajdosh & Porubcan 2004)
and theoretical showers associated with all three of the NEAs. Matches
were also found with the meteor showers Daytime April Piscids and
Daytime April Cetids (Kashcheev et al. 1967),
while some of the theoretical showers matched a significant number of
individual orbits found in the Meteor orbits data center (MODC). By our
initial assumption, NEOs
associated with meteor showers were to be regarded as being of cometary
origin. As all three produce the same matches, and their orbits
match each other, it is a reasonable hypothesis that all three are
fragments of a larger cometary body that no longer exists.
5 Conclusions
Our initial assumption was that NEOs that have meteor showers associated with them should be regarded as being either a dormant cometary nucleus or a surviving fragment from the break-up of a cometary nucleus. We have found three bodies, classified as asteroids, namely 2002JS2, 2002PD11, and 2003MT9, moving on orbits that are very similar to each other and all of which can also be associated with the well documented Northern and Southern Iota-Aquariids fireball showers. Fireballs also indicate that meteoroids larger than those normally associated with meteor showers exist in the stream. All these facts suggest strongly that what we now observe is all that remains of what was once a larger cometary body that no longer exists. It would be extremely instructive to obtain further observations of these three objects in order to ascertain whether or not further signatures of their cometary nature can be located.
AcknowledgementsThe authors would like to express their gratitude to the anonymous reviewer for useful comments which improved the paper. We gratefully acknowledge the support of the International Science and Technology Center Project T-1629, without which the work could not have been carried out.
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All Tables
Table 1: The values of the simplified D criterion.
Table 2: Orbital elements of the three near-Earth asteroids.
Table 3: Meteor showers associated with the NEA 2002JS2.
Table 4: Meteor showers associated with the NEA 2002PD11.
Table 5: Meteor showers associated with the NEA 2003MT9.
All Figures
![]() |
Figure 1:
The heliocentric distance of the ascending node |
Open with DEXTER | |
In the text |
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