论文标题
二元小行星的星体检测
Astrometric detection of binary asteroids
论文作者
论文摘要
二元小行星探测热辐射对主要皮带小行星进化的影响。我们讨论了通过在质量中心周围的灯光的星体摇摆来检测二进制次要行星系统的可能性。该方法可以探索二元小行星的相位，这很难使用常见检测技术探索。我们描述了一个向前的模型，该模型可以在观察者看到的那样，向中心质量中心地位。我们使用模拟的Gaia样数据研究了该方法的性能。我们将天文学方法应用于Gaia DR2太阳系目录的一部分，并找不到二元小行星的重要证据。这可能是因为Gaia DR2删除了天文异常值，在我们的情况下，这可能是由于天体物理信号引起的。将此方法应用于二进制小行星（4337）Arecibo，为此，Gaia DR3报告了可能的天体信号，其周期为P = 32.85 +/- 0.38小时，揭示了可能的2.2-Sigma溶液，周期为16.26小时（报告的一半）。我们发现来自Pravec等人已知的二元小行星种群中的较小，微不足道的天文噪声过量。相对于GAIA DR2太阳系目录中的整个小行星种群。我们还讨论了一些警告，例如进动和小行星旋转。
Binary asteroids probe thermal-radiation effects on the main-belt asteroids' evolution. We discuss the possibility of detecting binary minor planet systems by the astrometric wobble of the center-of-light around the center-of-mass. This method enables the exploration of the phase-space of binary asteroids, which is difficult to explore using common detection techniques. We describe a forward model that projects the center-of-light position with respect to the center-of-mass, as it is seen by the observer. We study the performance of this method using simulated Gaia-like data. We apply the astrometric method to a subset of the Gaia DR2 Solar System catalog and find no significant evidence of binary asteroids. This is likely because the Gaia DR2 removed astrometric outliers, which in our case may be due to astrophysical signals. Applying this method to binary asteroid (4337) Arecibo, for which Gaia DR3 reported a possible astrometric signal with a period of P = 32.85+/-0.38 hr, reveals a possible 2.2-sigma solution with a period of 16.26 hr (about half the reported period). We find a small, marginally significant, excess of astrometric noise in the known binary asteroid population from Pravec et al. relative to the entire asteroid population in the Gaia DR2 Solar System catalog. We also discuss some caveats like precession and asteroid rotation.
