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Table 4

Dynamical time scales and cumulative numbers of 1-km asteroids in the main belt (mb) and the near-Earth region (neo).

1-km 1-km 1-km 1-km 1-km 1-km
Num. Family Res. τg18 τneo τmb ρ Nmb Nneo obs. obs. Notes
Myr Myr Myr g cm−3 103 1 1 %
4 Vesta (HED) v6 6.98 4.39 1713 2.5! 11.4 29.2
25 Phocaea(H) v6 6.98 5.91 796 2.5 2.7 20.0!
170 Maria (H) 3:1 1.83 0.954 1533 3.0 5.5 3.4
808 Merxia (H) 5:2 0.68 0.24 866 2.5 2.0 0.6
847 Agnia (H) 5 2 0.68 0.19 1004 2.5 3.1 0.6
158 Koronis (H) 5:2 0.68 0.824 1438 3.0 9.2 5.2
158′ Koronis2 (H) 5:2 0.68 (a) (a) 3.0 0.4 0.0
832 Karin (H) 5:2 0.68 (a) (a) 2.5 1.1 0.0
20 Massalia (L) 3:1 1.83 0.45 1140 2.5 1.3? 0.5?
20′ Massalia2 (L) 3:1 1.83 0.45 1140 2.5 1.3? 0.5?
1272 Gefion (L) 5:2 0.68 0.69 749 2.5 3.8 3.5
3 Juno (L) 8:3 1.70 2.55 519 2.5 4.2 20.6
8 Flora (LL) V6 6.98 11.93 722 2.5 7.2 119.5
15 Eunomia (LL) 3:1 1.83 4.48 3078 3.54 7.0 10.2
44 Nysa (LL) 3:1 1.83 4.04 789 2.5 2.9 14.6
144 Vibilia (CM) 8:3 1.70 0.60u 2412u 1.7 0.7 0.2 All CM are CM/CR
145 Adeona (CM) 8:3 1.70 1.76 864 1.7 10.9 22.2
163 Erigone (CM) 3:1 1.83 4.64(a) 932(a) 1.7 2.7 0.0 Only sub-km nearby 3:1
410 Chloris (CM) 8:3 1.70 1.19 399 1.7 0.9 2.7
490 Veritas (CM) 2:1 0.40 (a) (a) 1.7 30.6 0.0
668 Dora (CM) 5:2 0.68 0.36 322 1.7 6.2 6.9
778 Theobalda (CM) 2:1 0.40 (a) (a) 1.7 15.9 0.0
1128 Astrid (CM) 5:2 0.68 0.23 786 1.7 8.1 2.4
3815 König (CM) 3:1 1.83 (a) (a) 1.7 3.9 0.0
10 Hygiea (CI) 2:1 0.40 0.27u 1899u 2.1 20.0e 2.8 All CI are CI/IDP
24 Themis (CI) 2:1 0.40 0.62 1292 1.3 20.0e 9.6
31 Euphrosyne (CI) 2:1 0.40 0.56 399 1.6 28.0e 39.3 High-i C-type NEOs
128 Nemesis (CI) 8:3 1.70 (a) (a) 3.5 6.3 0.0
142 Polana (CI) 3:1 1.83 5.12! 1261 1.7 14.2 57.7 Low-i C-type NEOs
302 Clarissa (CI) 3:1 1.83 (a) (a) 1.7 0.8 0.0
375 Ursula (CI) 2:1 0.40 0.30u 2187u 1.7 10.4e 1.4
569 Misa (CI) 8:3 1.70 0.63u 2002u 1.7 2.8 0.9
618 Elfriede (CI) 2:1 0.40 (a) (a) 1.7 10.6 0.0
656 Beagle (CI) 2:1 0.40 (a) (a) 1.3 1.3 0.0
702 Alauda (CI) 2:1 0.40 0.30 1041 1.7 12.1 3.5
845 Naema (CI) 5:2 0.68 0.24 469 1.7 4.1 2.1
1726 Hoffmeister (CI) 2:1 0.40 0.16 432 1.7 19.5 7.2
3556 Lixiaohua (CI) 2:1 0.40 (a) (a) 1.7 14.1e 0.0
283 Emma (IDP) 9:4 0.40 0.22 1689 1.7 3.3e 0.4
363 Padua (IDP) 8:3 1.70 0.13u 2522u 1.7 2.1 0.1
2 Pallas (B) 5:2 0.68 9.54! 824 2.9 0.3 3.5 High-i B-type NEOs
221 Eos (CO/CV/CK) 7:3 0.20 0.28 1816 3.1 44.0 6.5
729 Watsonia (CO/CV/CK) 5:2 0.68 1.24 1391 3.1 0.3 0.3 CAI-like
298 Baptistina (?) v6 6.98 8.31 2833 3.1 3.0 8.8 Low-i 1.00-µ NEOs
396 Aeolia (?) 5:2 0.68 (a) (a) 1.7 1.9 0.0
4203 Brucato (?) 8:3 1.70 (a) (a) 1.7 2.1 0.0
22 Kalliope (M) 5:2 0.68 0.31 1635 4.1 0.6 0.1
293 Brasilia (M) 5:2 0.68 0.83 285 3.5 4.4 12.8 CH?
369 Aëria (M) 8:3 1.70 (a) (a) 3.5 0.8 0.0
606 Brangäne (M) 3:1 1.83 (a) (a) 3.1 0.7 0.0 CB?
1222 Tina (M) 5:2 0.68 1.31 539 3.5 1.7 3.6
44′ Nysa (E) 3:1 1.83 4.04 789 2.5 2.9 14.6 Faint Xn-type NEOs
434 Hungaria (E) 5:1 36.0 14.70! 1752 3.1 0.6 5.0 High-i E-type NEOs
87 Sylvia (P) 2:1 0.40 0.33 1207 1.3 7.0e 1.9
2732 Witt (?) 5:2 0.68 0.15 2070 2.5 2.8 0.2
3200 Phaethon (CY?) 1.7 3.0
4652 Iannini (Aca/Lod) 11:4 (a) (a) 2.5 0.3 0.0
HED 11.4 29.2 16 1.8% Marsset et al. (2022)
H 23.6 29.8 Brož et al. (2024)
L 10.6 25.1 Brož et al. (2024)
LL 17.1 144.3 Brož et al. (2024)
CM 79.9 34.4
CI 164.2 124.5
IDP 5.4 0.5
B 0.3 3.5! 70 7.6% Outliers of CI-like?
CO/CV/CK 44.3 6.8 8 0.9% Reclassified K- and L-type
CR CM-type?
CH M-type?
CB M-type?
M 8.2 16.5 29 3.1%
E 3.5 19.6 5 0.5%
P 7.0 1.9! 26 2.8% Outliers of CI-like?
D 45 4.9% Jupiter-family comets?
Aca/Lod 0.3 0.0
? 4.9 8.8 24 2.6% Reclassified K- and L-type
? 2.1 0.0
CM+CI+IDP+B+CO/CV/CK+CR+CH+CB 304.1 178.5 303 32.8%
H+L+LL 51.3! 199.2 287 31.1%
all bodies 1360H 925H

Notes. For all families, we report the neighbouring resonances, the NEO life time τg18 from Granvik et al. (2018), the NEO life times τneo from this work, computed for 1-km bodies, the main belt life times τmb, the volumetric density of simulated bodies, the observed cumulative number Nmb(> 1 km) of main belt bodies, the computed cumulative number Nneo of NEOs and meteoroids. Additional notes: H Harris & Chodas (2021), N Nesvorný et al. (2023), (a) after ≈ 100 Myr or more, e extrapolated using a collisional model, u undersampled, ? uncertain value, ! exceptional value.

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