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Formation of asteroid pairs by rotational fission

Author

Listed:
  • P. Pravec

    (Astronomical Institute AS CR, Fričova 1, CZ-25165 Ondřejov, Czech Republic)

  • D. Vokrouhlický

    (Institute of Astronomy, Charles University, V Holešovičkách 2, CZ-18000 Prague, Czech Republic)

  • D. Polishook

    (Tel-Aviv University)

  • D. J. Scheeres

    (University of Colorado)

  • A. W. Harris

    (Space Science Institute)

  • A. Galád

    (Astronomical Institute AS CR, Fričova 1, CZ-25165 Ondřejov, Czech Republic
    Modra Observatory, Comenius University)

  • O. Vaduvescu

    (Instituto de Astronomia, Universidad Catolica del Norte
    Isaac Newton Group of Telescopes, E-38700 Santa Cruz de la Palma, Canary Islands, Spain)

  • F. Pozo

    (Instituto de Astronomia, Universidad Catolica del Norte)

  • A. Barr

    (Instituto de Astronomia, Universidad Catolica del Norte)

  • P. Longa

    (Instituto de Astronomia, Universidad Catolica del Norte)

  • F. Vachier

    (IMCCE-CNRS-Observatoire de Paris, 77 avenue Denfert Rochereau, 75014 Paris, France)

  • F. Colas

    (IMCCE-CNRS-Observatoire de Paris, 77 avenue Denfert Rochereau, 75014 Paris, France)

  • D. P. Pray

    (Carbuncle Hill Observatory)

  • J. Pollock

    (Appalachian State University)

  • D. Reichart

    (University of North Carolina)

  • K. Ivarsen

    (University of North Carolina)

  • J. Haislip

    (University of North Carolina)

  • A. LaCluyze

    (University of North Carolina)

  • P. Kušnirák

    (Astronomical Institute AS CR, Fričova 1, CZ-25165 Ondřejov, Czech Republic)

  • T. Henych

    (Astronomical Institute AS CR, Fričova 1, CZ-25165 Ondřejov, Czech Republic)

  • F. Marchis

    (University of California at Berkeley
    SETI Institute)

  • B. Macomber

    (University of California at Berkeley
    SETI Institute)

  • S. A. Jacobson

    (University of Colorado)

  • Yu. N. Krugly

    (Institute of Astronomy of Kharkiv National University, Sumska Str. 35, Kharkiv 61022, Ukraine)

  • A. V. Sergeev

    (Institute of Astronomy of Kharkiv National University, Sumska Str. 35, Kharkiv 61022, Ukraine)

  • A. Leroy

    (Observatoire Midi Pyrénées and Association T60)

Abstract

Asteroids two-by-two The increased interest in the observation of main-belt asteroids in recent years has led to the identification of tens of asteroid pairs, which follow near-identical orbits around the Sun even though they are not physically bound together. Rotational fission of larger bodies has been hypothesized as a mechanism for their formation, an idea that gains support with some new observations. Theory predicts that the mass ratios of two asteroids in a pair will be than about 0.2 and that as the mass ratio approaches this upper limit, the spin period of the larger body is extended. Accordingly, photometric observations of 35 asteroid pairs reveal none with mass ratios greater than 0.2, and as mass ratios approach 0.2, primary periods grow longer. This suggests that asteroid pairs form by rotational fusion of a parent asteroid into a short-lived proto-binary system.

Suggested Citation

  • P. Pravec & D. Vokrouhlický & D. Polishook & D. J. Scheeres & A. W. Harris & A. Galád & O. Vaduvescu & F. Pozo & A. Barr & P. Longa & F. Vachier & F. Colas & D. P. Pray & J. Pollock & D. Reichart & K., 2010. "Formation of asteroid pairs by rotational fission," Nature, Nature, vol. 466(7310), pages 1085-1088, August.
    • Handle: RePEc:nat:nature:v:466:y:2010:i:7310:d:10.1038_nature09315
    DOI: 10.1038/nature09315
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    Cited by:

    1. Adriano Campo Bagatin & Aldo Dell’Oro & Laura M. Parro & Paula G. Benavidez & Seth Jacobson & Alice Lucchetti & Francesco Marzari & Patrick Michel & Maurizio Pajola & Jean-Baptiste Vincent, 2024. "Recent collisional history of (65803) Didymos," Nature Communications, Nature, vol. 15(1), pages 1-9, December.

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