Table 5
Thermal properties of 11 selected asteroids.
| Ast. name | r | ρbulk | ρsurf. | κ | C | p v | ϵ | P | Spin |
| [m] | [kg/m3] | [kg/m3] | [W/K/m] | [J/kg/K] | (pV) | [h] | |||
|
|
|||||||||
| (956) Elisa | 5237 ± 800 | 3000 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.1468 ± 0.0221 [5] | 0.95 [8] | 16.492 ± 0.001 [6] | random |
| (4278) Harvey | 2245 ± 227 | 3000 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.318 ± 0.035 [1] | 0.95 [8] | 3.118 ± 0.315 [2] | random |
| (728) Leonisis | 3634 ± 328 | 2700 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.2557 ± 0.0272 [5] | 0.95 [8] | 5.5783 ± 0.0002 [6] | random |
| (4375) Kiyomori | 2920 ± 835 | 2700 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.298 ± 0.143 [1] | 0.95 [8] | 6.4709 ± 0.0004 [6] | random |
| (2780) Monnig | 3045 ± 253 | 2700 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.2287 ± 0.0206 [5] | 0.95 [8] | 4.229 ± 0.350 [2] | random |
| (4556) Gumilyov | 2612 ± 257 | 2700 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.2825 ± 0.0321 [5] | 0.95 [8] | 3.628 ± 0.356 [2] | random |
| (809) Lundia | 4550 ± 500 [3] | 2500 ± 200 [4] | 1500 [8] | 0.001 [8] | 680 [9] | 0.3266 ± 0.0572 [5] | 0.95 [8] | 15.41574 ± 0.00001 [4] | λ = 122° ± 5°β = 22° ± 5° [4] |
| (122192) 2000 KK82 | 748 ± 76 | 3000 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.318 ± 0.035 [1] | 0.95 [8] | 1.0388 ± 0.105 [2] | random |
| (124360) 2001 QR133 | 807 ± 82 | 3000 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.318 ± 0.035 [1] | 0.95 [8] | 1.1201 ± 0.113 [2] | random |
| (151563) 2002 TM135 | 523 ± 53 | 3000 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.318 ± 0.035 [1] | 0.95 [8] | 0.7262 ± 0.073 [2] | random |
| (103418) 2000 AM150 | 630 ± 64 | 3000 [7] | 1500 [8] | 0.001 [8] | 680 [9] | 0.318 ± 0.035 [1] | 0.95 [8] | 0.8749 ± 0.088 [2] | random |
Notes. r [m] − if not determined: calculated by diameter formula by Fowler & Chillemi (1992); [1] Typical (mean) values of albedos determined by Usui et al. (2013); [2] rotation period, if not determined: P [s] = 5(D [m] /2) = 5R [m]. [3] Equivalent of r value for Lundia (single-body approximation); [4] Kryszczynska et al. (2014); [5] Masiero et al. (2011); [6] JPL small body browser; [7] typical densities of V and A asteroids, used as default (Carruba et al. 2014); [8] commonly used surface densities, ϵ and κ values (Carruba et al. 2014), (Brož 2006); values expected for regolith-covered MBA. (Brož 2006); We adapted densities, κ, C, and ϵ values used by most authors without uncertainties (as typical, default values).
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