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Formation of asteroid pairs by rotational fission

机译：通过旋转裂变形成小行星对

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摘要

Pairs of asteroids sharing similar heliocentric orbits, but not bound together, were found recently. Backward integrations of their orbits indicated that they separated gently with low relative velocities, but did not provide additional insight into their formation mechanism. A previously hypothesized rotational fission process4 may explain their formation-critical predictions are that the mass ratios are less than about 0.2 and, as the mass ratio approaches this upper limit, the spin period of the larger body becomes long. Here we report photometric observations of a sample of asteroid pairs, revealing that the primaries of pairs with mass ratios much less than 0.2 rotate rapidly, near their critical fission frequency. As the mass ratio approaches 0.2, the primary period grows long. This occurs as the total energy of the system approaches zero, requiring the asteroid pair to extract an increasing fraction of energy from the primary's spin in order to escape. We do not find asteroid pairs with mass ratios larger than 0.2. Rotationally fissioned systems beyond this limit have insufficient energy to disrupt. We conclude that asteroid pairs are formed by the rotational fission of a parent asteroid into a proto-binary system, which subsequently disrupts under its own internal system dynamics soon after formation.
机译：最近发现了成对的小行星，它们共享相似的日心中心轨道，但没有被束缚在一起。它们轨道的向后积分表明它们以较低的相对速度平缓地分离，但是没有提供对它们形成机制的进一步了解。先前假设的旋转裂变过程4可以解释其形成关键的预测，即质量比小于约0.2，并且当质量比接近此上限时，较大物体的旋转周期变长。在这里，我们报告了对小行星对样本的光度学观察，发现质量比远小于0.2的小行星对的原核在接近其临界裂变频率时迅速旋转。当质量比接近0.2时，初生期延长。当系统的总能量接近零时，会发生这种情况，这要求小行星对从小行星的自旋中提取越来越多的能量才能逃逸。我们找不到质量比大于0.2的小行星对。超过此极限的旋转裂变系统没有足够的能量来破坏。我们得出的结论是，小行星对是由母体小行星的旋转裂变形成原始二元系统而形成的，该二元系统随后在其自身内部系统动力学形成后很快受到破坏。

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  • 来源
    《Nature》 |2010年第7310期|P.1085-1088iii|共5页
  • 作者

    P. Pravec; D. Vokrouhlicky; D. Polishook; D. J. Scheeres; A. W. Harris; A. Galad; O. Vaduvescu; F. Pozo; A. Barr; P. Longa; F. Vachier; F. Colas; D. P. Pray; J. Pollock; D. Reichart; K. Ivarsen; J. Haislip; A. LaCluyze; P. Kusnirak; T. Henych; F. Marchis; B. Macomber; S. A. Jacobson; Yu. N. Krugly; A. V. Sergeev; A. Leroy;

  • 作者单位

    Astronomical Institute AS CR, Fricova 1, CZ-25165 Ondrejov, Czech Republic;

    rnInstitute of Astronomy, Charles University, V Holesovickach 2, CZ-18000 Prague, Czech Republic;

    Wise Observatory and Department of Geophysics and Planetary Sciences, Tel-Aviv University, Tel-Aviv 69978, Israel;

    rnDepartment of Aerospace Engineering Sciences, University of Colorado, Boulder, Colorado 80309, USA;

    rnSpace Science Institute, 4603 Orange Knoll Avenue, La Canada, California 91011, USA;

    rnAstronomical Institute AS CR, Fricova 1, CZ-25165 Ondrejov, Czech Republic Modra Observatory, Comenius University, Bratislava SK-84248, Slovakia;

    rnlnstituto de Astronomia, Universidad Catolica del Norte, Avenida Angamos 0610, Antofagasta, Chile lsaac Newton Group of Telescopes, E-38700 Santa Cruz de la Palma, Canary Islands, Spain;

    rnlnstituto de Astronomia, Universidad Catolica del Norte, Avenida Angamos 0610, Antofagasta, Chile;

    rnlnstituto de Astronomia, Universidad Catolica del Norte, Avenida Angamos 0610, Antofagasta, Chile;

    rnlnstituto de Astronomia, Universidad Catolica del Norte, Avenida Angamos 0610, Antofagasta, Chile;

    rnIMCCE-CNRS-Observatoire de Paris, 77 avenue Denfert Rochereau, 75014 Paris, France;

    rnIMCCE-CNRS-Observatoire de Paris, 77 avenue Denfert Rochereau, 75014 Paris, France;

    rnCarbunde Hill Observatory, West Brookfield, Massachusetts 01585, USA;

    rnPhysics and Astronomy Department, Appalachian State University, Boone, North Carolina 28608, USA;

    rnPhysics and Astronomy Department, University of North Carolina, Chapel Hill, North Carolina 27514, USA;

    rnPhysics and Astronomy Department, University of North Carolina, Chapel Hill, North Carolina 27514, USA;

    rnPhysics and Astronomy Department, University of North Carolina, Chapel Hill, North Carolina 27514, USA;

    rnPhysics and Astronomy Department, University of North Carolina, Chapel Hill, North Carolina 27514, USA;

    rnAstronomical Institute AS CR, Fricova 1, CZ-25165 Ondrejov, Czech Republic;

    rnAstronomical Institute AS CR, Fricova 1, CZ-25165 Ondrejov, Czech Republic;

    rnUniversity of California at Berkeley, Berkeley, California 94720, USA SETI Institute, Mountain View, California 94043, USA;

    rnUniversity of California at Berkeley, Berkeley, California 94720, USA SETI Institute, Mountain View, California 94043, USA;

    rnDepartment of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA;

    rnlnstitute of Astronomy of Kharkiv National University, Sumska Str. 35, Kharkiv 61022, Ukraine;

    rnlnstitute of Astronomy of Kharkiv National University, Sumska Str. 35, Kharkiv 61022, Ukraine;

    rnObservatoire Midi Pyrenees and Association T60, Pic du Midi, France;

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