J/A+A/681/A23 Very young asteroid families (Vokrouhlicky+, 2024)
Debiased population of very young asteroid families.
Vokrouhlicky D., Nesvorny D., Broz M., Bottke W.F.
<Astron. Astrophys., 681, A23 (2024)>
=2024A&A...681A..23V 2024A&A...681A..23V (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Minor planets
Keywords: celestial mechanics - minor planets, asteroids: general
Abstract:
Asteroid families that are less than one million years old offer a
unique possibility to investigate recent asteroid disruption events
and test ideas about their dynamical evolution. Observations provided
by powerful all-sky surveys have led to an enormous increase in the
number of detected asteroids over the past decade. When the known
populations are well characterized, they can be used to determine
asteroid detection probabilities, including those in young families,
as a function of their absolute magnitude.
We use observations from the Catalina Sky Survey (CSS) to determine
the bias-corrected population of small members in four young families
down to sizes equivalent to several hundred meters.
Using the most recent catalog of known asteroids, we identified
members from four young families for which the population has grown
appreciably over recent times. A large fraction of these bodies have
also been detected by CSS. We used synthetic populations of asteroids,
with their magnitude distribution controlled by a small number of
parameters, as a template for the bias-corrected model of these
families. Applying the known detection probability of the CSS
observations, we could adjust these model parameters to match the
observed (biased) populations in the young families.
In the case of three families, Datura, Adelaide, and Rampo, we find
evidence that the magnitude distribution transitions from steep to
shallow slopes near 300 to 400 meters. Conversely, the Hobson family
population may be represented by a single power-law model. The
Lucascavin family has a limited population; no new members have been
discovered over the past two decades. We consider a model of parent
body rotational fission with the escaping secondary tidally split into
two components (thereby providing three members within this family).
In support of this idea, we find that no other asteroid with absolute
magnitude H≤18.3 accompanies the known three members in the
Lucascavin family. A similar result is found for the archetypal
asteroid pair Rheinland-Kurpfalz.
Description:
We provide an information about membership in the very young asteroid
families studied in this paper.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea.dat 81 290 Osculating heliocentric orbital elements at
epoch MJD 60000.0 from the MPC catalog
(tables A1-A7 of the paper)
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See also:
B/astorb : Orbits of Minor Planets (Bowell+, 2014-)
Byte-by-byte Description of file: tablea.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Fam Family code (1)
4 A1 --- Case [S-] S for Singleopposition members (2)
6- 11 I6 --- Ast ? Asteroid number
13- 22 A10 --- Name Asteroid name
24- 28 F5.2 mag H Absolute magnitude H
30- 38 F9.7 au a Semimajor axis
40- 48 F9.7 --- e Eccentricity
50- 57 F8.5 deg i Inclination
61- 69 F9.5 deg OMEGA Longitude of node
71- 79 F9.5 deg omega Argument of perihelion
81 A1 --- CSS [Y] Y when asteroid has been detected by CSS
during the phase 2 operations
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Note (1): Family codes as follows:
A1 = Datura family as of June 2023.
We note two very small, single opposition asteroids 2016 PL51 and
2022 RB57, very likely members of the Datura family too. However, their
orbits, based on observations spanning short arcs (less than a week in
the case of 2016 PL51), are still very uncertain.
We include (429988) 2013 PZ36 residing on a rather chaotic orbit (most
likely interacting with the exterior E3/10 mean motion resonance with
the Earth), such that proving its membership to the Datura family would
require an extensive work beyond the scope of this paper (see also
Fig. 1). Luckily, the results discussed in Sect. 4 are not overly
sensitive to the decision about Datura membership of this body.
A2 = Adelaide family as of June 2023.
We note asteroid (159941) 2005 WV178 in the near vicinity of the
Adelaide family, which we discard from the membership due to a dubious
convergence to (525) Adelaide in the past Myr.
A3 = Hobson family as of June 2023.
We note a very small, single opposition asteroids 2019 NF93, 2021 JQ73,
2023 JD27 and 2023 NV2 very likely members of the Hobson family too.
However, their orbits, especially for 2019 NF93 based on observations
spanning less than a week, are still very uncertain.
A4 = Rampo family as of June 2023.
We note two very small, single opposition asteroids 2015 KM284 and
2015 KG287, very likely members of the Rampo family too. However, their
orbits, based on observations spanning less than a week, are still very
uncertain.
A5 = Wasserburg family as of June 2023.
A6 = Martes family as of June 2023.
A7 = Lucascavin family as of June 2023.
Note (2): S indicates single opposition asteroids.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 23-Apr-2024