Table 2
Different models of physical parameters of Kamo‘oalewa used to estimate the thermal inertia.
| Parameter | Model 1 | Model 2 | Model 3 | Model 4 |
|---|---|---|---|---|
| Absolute magnitude, H | 24.28 ± 0.18 | 24.28 ± 0.18 | 24.28 ± 0.18 | 24.28 ± 0.18 |
| Albedo, pV | 0.1 ± 0.03 | 0.1 ± 0.03 | 0.24 ± 0.05 | 0.24 ± 0.05 |
| Bulk density, ρ | 2720 ± 540 kg m−3 | 2720 ± 540 kg m−3 | 2720 ± 540 kg m−3 | 2720 ± 540 kg m−3 |
| Rotation Period, P | 0.4716 ± 0.03 h | 0.4716 ± 0.03 h | 0.4716 ± 0.03 h | 0.4716 ± 0.03 h |
| Obliquity, γ | 107 ± 10 deg | NEA Population | 107± 10 deg | NEA Population |
| Heat capacity, C | 800 J kg−1 K−1 | 800 J kg−1 K−1 | 800 J kg−1 K−1 | 800 J kg−1 K−1 |
| Absorption coefficient, α | 0.95 | 0.95 | 0.90 | 0.90 |
| Emissivity, ε | 0.984 | 0.984 | 0.984 | 0.984 |
| Non-sphericity correction factor, ξ | 0.75 | 0.75 | 0.75 | 0.75 |
Notes. The absolute magnitude is computed by fitting photometric data with an a-priori distribution of G extrapolated from S-type asteroids data. The low albedo value is chosen according to the measured value on LL chondrite powder analogue (Zhang et al. 2024), while the high albedo value is representative of S-type asteroids (Marsset et al. 2022). The bulk density refers to the average of S-type asteroids (Carry 2012). The rotation period is taken from Sharkey et al. (2021). The value of obliquity is taken from Zhang et al. (2025), while the NEA population obliquity distribution is taken from Tardioli et al. (2017). Heat capacity is assumed as a reasonable value for NEAs. The absorption coefficient is obtained by assuming a slope parameter of G = 0.25 and the assumed albedo. The emissivity corresponds to the average value measured on a large sample of meteorites (Ostrowski & Bryson 2019). The non-sphericity correction factor, ξ, is obtained from light-curve amplitude of 1.07 mag (Sharkey et al. 2021).
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