The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys
The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys
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DOI：
10.1016/j.icarus.2013.06.027
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发表时间：
2013-09-01
期刊：
影响因子：
3.2
通讯作者：
Carry, B.
中科院分区：
文献类型：
--
作者：
DeMeo, F. E.;Carry, B.
人们对小行星在主带上的分布进行了数十年的研究，以了解当前的成分分布以及它告诉我们太阳系的形成和演化的信息。全天空调查现在提供的数据比定向调查多几个数量级。我们提出了一种根据大小、距离和反照率对斯隆数字巡天（SDSS）中观测到的小行星群进行偏差校正的方法。我们按照 Bus 和 Binzel（Bus, S.J., Binzel, R.P. [2002]. Icarus 158, 146-177）和 Bus-DeMeo 等人对这个数据集进行分类分类。 (DeMeo, F.E., Binzel, R.P., Slivan, S.M., Bus, S.J. [2009]. Icarus 202(July), 160-180) 系统并呈现由此产生的分类分布。该数据集包括小至 5 公里的小行星，直径比 Mothe-Diniz 等人之前的工作小三倍。 （Mothe-Diniz, T.、Carvano, J.M.A.、Lazzaro, D. [2003]。Icarus 162（三月），10-21）。由于我们的样本尺寸范围广泛，我们按数量、表面积、体积和质量来呈现分布，而以前的工作仅按数量呈现。虽然按数量分布是一个有用的量并且已经使用了几十年，但这些额外的量为总材料的分布提供了新的见解。我们在内部主带中发现了 D 型的证据，根据行星迁移期间天体从外太阳系植入内太阳系的动力学模型，它们是意想不到的（Levison, H.F., Bottke, W.F., Gounelle, M., Morbidelli, A, Nesvorny, D., Tsiganis, K. [2009]. Nature 460(July), 364-366）。我们在特洛伊木马和希尔达斯中没有发现 S 型或其他意外类别的证据，尽管有利于这种检测的偏见。最后，我们首次估计了内太阳系中每一类物质的总量。主带的最大质量等级依次为 C、B、P、V 和 S。排除严重扭曲数值的四颗质量最大的小行星（1）谷神星、（2）智神星、（4）灶神星和（10）健神星，原始物质（C型、P型）占主带和特洛伊小行星质量的一半以上，剩余质量大部分为S型。所有其他类别都是火星和木星之间物质的次要贡献者。 (C) 2013 Elsevier Inc. 保留所有权利。
The distribution of asteroids across the main belt has been studied for decades to understand the current compositional distribution and what that tells us about the formation and evolution of our Solar System. All-sky surveys now provide orders of magnitude more data than targeted surveys. We present a method to bias-correct the asteroid population observed in the Sloan Digital Sky Survey (SDSS) according to size, distance, and albedo. We taxonomically classify this dataset consistent with the Bus and Binzel (Bus, S.J., Binzel, R.P. [2002]. Icarus 158, 146-177) and Bus-DeMeo et al. (DeMeo, F.E., Binzel, R.P., Slivan, S.M., Bus, S.J. [2009]. Icarus 202(July), 160-180) systems and present the resulting taxonomic distribution. The dataset includes asteroids as small as 5 km, a factor of three in diameter smaller than in previous work such as by Mothe-Diniz et al. (Mothe-Diniz, T., Carvano, J.M.A., Lazzaro, D. [2003]. Icarus 162(March), 10-21). Because of the wide range of sizes in our sample, we present the distribution by number, surface area, volume, and mass whereas previous work was exclusively by number. While the distribution by number is a useful quantity and has been used for decades, these additional quantities provide new insights into the distribution of total material. We find evidence for D-types in the inner main belt where they are unexpected according to dynamical models of implantation of bodies from the outer Solar System into the inner Solar System during planetary migration (Levison, H.F., Bottke, W.F., Gounelle, M., Morbidelli, A, Nesvorny, D., Tsiganis, K. [2009]. Nature 460(July), 364-366). We find no evidence of S-types or other unexpected classes among Trojans and Hildas, albeit a bias favoring such a detection. Finally, we estimate for the first time the total amount of material of each class in the inner Solar System. The main belt's most massive classes are C, B, P, V and S in decreasing order. Excluding the four most massive asteroids, (1) Ceres, (2) Pallas, (4) Vesta and (10) Hygiea that heavily skew the values, primitive material (C-, P-types) account for more than half main-belt and Trojan asteroids by mass, most of th remaining mass being in the S-types. All the other classes are minor contributors to the material between Mars and Jupiter. (C) 2013 Elsevier Inc. All rights reserved.