J/AJ/164/167 400 Eurybates family members (Maschall+, 2022)
Implications for the Collisional Strength of Jupiter Trojans from the Eurybates
Family.
Maschall R., Nesvorny D., Deienno R., Wong I., Levison H.F., Bottke W.F.
<Astron. J., 164, 167 (2022)>
=2022AJ....164..167M 2022AJ....164..167M
ADC_Keywords: Models; Solar system; Minor planets; Optical; Colors
Keywords: Jupiter trojans ; Trojan asteroids ; Collision processes ;
Theoretical models ; Asteroids
Abstract:
In this work, we model the collisional evolution of the Jupiter
Trojans and determine under which conditions the Eurybates-Queta
system survives. We show that the collisional strength of the Jupiter
Trojans and the age of the Eurybates family and by extension Queta are
correlated. The collisional grinding of the Jupiter Trojan population
over 4.5Gy results in a size-frequency distribution (SFD) that remains
largely unaltered at large sizes (>10km) but is depleted at small
sizes (10m to 1km). This results in a turnover in the SFD, the
location of which depends on the collisional strength of the material.
It is to be expected that the Trojan SFD bends between 1 and 10km.
Based on the SFD of the Eurybates family, we find that the family was
likely the result of a catastrophic impact onto a 100km rubble pile
target. This corresponds to objects with a rather low collisional
strength (10 times weaker than that of basaltic material studied in
Benz & Asphaug). Assuming this weak strength, and an initial
cumulative slope of the size-frequency distribution of 2.1 between
diameters of 2m and 100km when the Trojans were captured, the
existence of Queta, the satellite of Eurybates, implies an upper limit
for the family age of 3.7Gy. Alternatively, we demonstrate that an
unconventional collisional strength with a minimum at 20m is a
plausible candidate to ensure the survival of Queta over the age of
the solar system. Finally, we show how different collisional histories
change the expected number of craters on the targets of the Lucy
mission and that Lucy will be able to differentiate between them.
Description:
In this work we have modeled the collisional evolution of the Jupiter
Trojans and determined under which conditions the Eurybates-Queta
system survives.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 82 400 *List of all 400 Eurybates family members
table4.dat 74 41 *Color data for Eurybates family members
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Note on table3.dat:Identified by the hierarchical clustering method
including the likely interloper (5258) Rhoeo (see discussion in Sec.2)
Note on table4.dat:Identified by the hierarchical clustering method
including the likely interloper (5258) Rhoeo (see discussion in Sec.2)
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See also:
J/ApJ/742/40 : Jovian Trojans asteroids with WISE/NEOWISE (Grav+, 2011)
http://sbn.psi.edu/pds/resource/fornasier.html : (Fornasier+, 2007)
http://sbn.psi.edu/pds/resource/neowisediam.html : NEOWISE data (Mainzer+,2019)
http://minorplanetcenter.net/ : Minor Planet Center
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- NR [3548/546752]? Asteroid number
8- 17 A10 --- ProDes Provisional designation
19- 23 F5.2 mag Hmag [9.85/15.1] Absolute magnitude (1)
25- 30 F6.3 km Diam [8.86/63.9]? Diameter (2)
32- 36 F5.3 km e_Diam [0.2/4.5]? Uncertainty in Diam
38- 44 F7.5 AU aprop [5.26/5.33] Proper Semi-major axis (3)
46- 52 F7.5 AU e_aprop [5e-05/0.004] Uncertainty in aprop
54- 60 F7.5 --- eprop [0.03/0.07] Proper eccentricity (3)
62- 68 F7.5 --- e_eprop [2e-05/0.005] Uncertainty in eprop
70- 75 F6.4 deg iprop [6.98/7.86] Proper inclination (3)
77- 82 F6.4 deg e_iprop [0.0003/0.08] Uncertainty in iprop
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Note (1): Minor Planet Center; 2020-12-08,
http://minorplanetcenter.net//iau/lists/JupiterTrojans.html
Note (2): NEOWISE data v2.0, Mainzer+, 2019,
http://sbn.psi.edu/pds/resource/neowisediam.html
Note (3): Mira Broz (Holt+, 2020MNRAS.495.4085H 2020MNRAS.495.4085H)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- NR [3548/313024] Asteroid number
8- 17 A10 --- ProDes Provisional designation
19- 23 F5.2 mag Hmag [9.85/13.9] Absolute magnitude (1)
25- 30 F6.3 km Diam [10.805/63.885]? Diameter (2)
32- 36 F5.3 km e_Diam [0.234/4.429]? Uncertainty in Diam
38- 42 F5.3 mag g-i [0.53/0.96]? SDSS (g-i) color (3)
44- 48 F5.3 mag e_g-i [0.02/0.1]? Uncertainty in g-i
50- 54 F5.2 --- S [-0.53/4.64]? Spectral slope between
0.3-0.9microns (%/um) (4)
56- 59 F4.2 --- e_S [0.5/1]? Uncertainty in S
61- 64 F4.2 mag g-r [0.39/0.6]? ZTF (g-r) color (5)
66- 69 F4.2 mag E_g-r [0.02/0.2]? Upper uncertainty in g-r
71- 74 F4.2 mag e_g-r [0.02/0.2]? Lower uncertainty in g-r
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Note (1): Minor Planet Center; 2020-12-08,
http://minorplanetcenter.net//iau/lists/JupiterTrojans.html
Note (2): NEOWISE data v2.0, Mainzer+, 2019,
http://sbn.psi.edu/pds/resource/neowisediam.html
Note (3): Sloan Digital Sky Survey (SDSS) Moving Object Catalog
(Ivezic+, 2001, 2001AJ....122.2749I 2001AJ....122.2749I)
https://sbn.psi.edu/pds/resource/sdssmoc.html
Note (4): Fornasier+, 2007Icar..190..622F 2007Icar..190..622F,
http://sbn.psi.edu/pds/resource/fornasier.html
Note (5): Schemel & Brown, 2021PSJ.....2...40S 2021PSJ.....2...40S
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 25-Nov-2022