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arXiv 2201.05164astro-ph.EP
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1847颗WISE观测小行星的热性质

Thermal Properties of 1847 WISE-observed Asteroids

Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen

备注：
86 pages, 17 figures, 6 tables, accepted by PSJ with proof corrections. Table 5, now corrected, was erroneously published with a different definition for "dense lightcurve", using 15 data points as a minimum rather than 30, so several asteroids had higher numbers of dense lightcurves than presented elsewhere in the paper
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AI总结：

本研究利用WISE全低温阶段热通量数据和DAMIT形状模型等，对1847颗小行星进行TPM拟合得到热惯量等参数，验证了热惯量与直径的线性关系，为后续高精度热物理建模奠定基础。

摘要：

我们给出了1847颗小行星的新热物理模型（thermophysical model, TPM）拟合结果，推导了它们的热惯量、直径，以及邦德反照率和可见光几何反照率。我们使用的热通量测量数据来自广域红外巡天探测器（Wide-field Infrared Survey Explorer, WISE; Wright等人2010; Mainzer等人2011）的全低温运行阶段，该阶段12μm（W3）和22μm（W4）两个波段均可用。我们从反演技术小行星模型数据库（Database of Asteroid Models from Inversion Techniques, DAMIT; Ďurech等人2010）获取形状模型和自转信息，同时通过光变曲线反演，并将WISE测光数据与已有的DAMIT光变曲线相结合，推导得到新的形状模型。当我们将样本限定为拥有最可靠形状模型和热通量测量数据的小行星时，发现热惯量关系与近期研究结果大体一致。我们对归一化至1天文单位（au）的直径D（单位：km）和热惯量Γ（单位：J m⁻² s⁻⁰·⁵ K⁻¹）进行拟合，采用形式为log[Γ]=α+βlog[D]的线性关系：仅使用我们的样本时，得到α=2.667±0.059、β=-0.467±0.044；结合其他文献的估计值时，得到α=2.509±0.017、β=-0.352±0.012。由于我们的样本中慢速自转天体数量较少，几乎没有发现自转周期与热惯量之间存在相关性的证据。尽管我们推导的大部分热惯量结果不确定性较大，仅能识别热惯量与其他物理参数之间的大致趋势，但随着即将开展的红外和广域巡天项目的推进，高质量热通量测量数据和小行星形状模型的数量预计将大幅增加，未来有望开展精度更高的热物理建模研究。

英文摘要：

We present new thermophysical model (TPM) fits of 1,847 asteroids, deriving thermal inertia, diameter, and Bond and visible geometric albedo. We use thermal flux measurements obtained by the Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010; Mainzer et al. 2011) during its fully cryogenic phase, when both the 12$μ$m (W3) and 22$μ$m (W4) bands were available. We take shape models and spin information from the Database of Asteroid Models from Inversion Techniques (DAMIT; Ďurech et al. 2010) and derive new shape models through lightcurve inversion and combining WISE photometry with existing DAMIT lightcurves. When we limit our sample to the asteroids with the most reliable shape models and thermal flux measurements, we find broadly consistent thermal inertia relations with recent studies. We apply fits to the diameters $D$ (km) and thermal inertia $Γ$ (J m$^{-2}$ s$^{-0.5}$ K$^{-1}$) normalized to 1 au with a linear relation of the form $\log[Γ]=α+β\log[D]$, where we find $α= 2.667 \pm 0.059$ and $β= -0.467 \pm 0.044$ for our sample alone and $α= 2.509 \pm 0.017$ and $β= -0.352 \pm 0.012$ when combined with other literature estimates. We find little evidence of any correlation between rotation period and thermal inertia, owing to the small number of slow rotators to consider in our sample. While the large uncertainties on the majority of our derived thermal inertia only allow us to identify broad trends between thermal inertia and other physical parameters, we can expect a significant increase in high-quality thermal flux measurements and asteroid shape models with upcoming infrared and wide-field surveys, enabling even more thermophysical modeling of higher precision in the future.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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