Formation of asteroid pairs by rotational fission

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. Ivarsen, J. Haislip, A. LaCluyze, P. Kušnirák, T. Henych, F. Marchis, B. Macomber, S. A. Jacobson, Yu. N. Krugly, A. V. Sergeev and A. Leroy
Additional contact information
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
O. Vaduvescu: Instituto de Astronomia, Universidad Catolica del Norte
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
B. Macomber: University of California at Berkeley
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

Nature, 2010, vol. 466, issue 7310, 1085-1088

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.

Date: 2010
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DOI: 10.1038/nature09315

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