小行星对的旋转分辨光谱：没有光谱变化表明Fission之后是尘埃沉降
Rotationally Resolved Spectroscopy of Asteroid Pairs: No Spectral Variation Suggests Fission is followed by Settling of Dust
摘要：
我们研究的光谱特性的小行星对，在过去的200万年被打乱，检查裂变的网站是否可以揭示。我们研究的可能性，子表面的材料，也许在一个半球，具有不同于原来的风化表面的光谱特性，通过执行旋转分辨光谱观测，以寻找当地的变化，因为小行星旋转。我们在近红外和可见光范围内观察到11颗成对的小行星。还进行了测光，以确定小行星光变曲线光谱的旋转相位。我们没有检测到任何旋转的光谱变化内的信号-噪声，这使我们能够限制任何现有的表面异质性的程度。对于每个观测到的光谱的一个小行星的纵向段，我们估计的最大尺寸的未检测到的“点”的光谱特征不同于平均值。对于5颗小行星来说，这样一个斑点的最大直径比次级成员的直径小两倍。因此，裂变的位置大于具有唯一光谱参数的任何区域，并且裂变的位置不具有唯一光谱。在S-复合小行星的情况下，裂变地点预计将呈现非风化光谱，如果旋转-裂变过程之后是尘埃扩散，重新积聚在主小行星上并均匀覆盖它，则可以解释缺乏裂变点。年轻的小行星6070呈现出SQ型光谱，而它的内部物质，可能是在它的次级成员54827的表面上发现的，具有更新鲜的Q型光谱。在小行星P/2013 R3的分裂事件中观察到的尘埃扩散可能是这种过程的一个例子，并表明它确实是在旋转裂变事件中形成的。
英文摘要：
We examine the spectral properties of asteroid pairs that were disrupted in the last 2 Myrs to examine whether the site of the fission can be revealed. We studied the possibility that the sub-surface material, perhaps on one hemisphere, has spectral characteristics differing from the original weathered surface, by performing rotationally-resolved spectroscopic observations to look for local variations as the asteroid rotates. We observed 11 asteroids in pairs in the near-IR and visible range. Photometry was also conducted to determine the rotational phases of a spectrum on the asteroid lightcurves. We do not detect any rotational spectral variations within the signal-to-noise, which allow us to constrain the extent of any existing surface heterogeneity. For each observed spectrum of a longitudinal segment of an asteroid, we estimate the maximal size of an un-detected "spot" with a spectral signature different than the average. For 5 asteroids the maximal diameter of such a spot is smaller by a factor of two than the diameter of the secondary member. Therefore, the site of the fission is larger than any area with a unique spectral parameters and the site of the fission does not have a unique spectrum. In the case of an S-complex asteroid, where the site of fission is expected to present non-weathered spectra, a lack of a fission spot can be explained if the rotational-fission process is followed by the spread of dust that re-accumulates on the primary asteroid and covers it homogeneously. This is demonstrated for the young asteroid 6070 that presents an Sq-type spectrum while its inner material, that is presumably revealed on the surface of its secondary member, 54827, has a fresher, Q-type spectrum. The spread of dust observed in the disruption event of asteroid P/2013 R3, might be an example of such a process and an indication that it was indeed formed in a rotational-fission event.
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