Asteroid pairs: a complex picture

Autor: Josef Hanus, Petr Pravec, Alexey V. Sergeyev, K. E. Ergashev, Štefan Gajdoš, F. Manzini, N. M. Gaftonyuk, Sh. A. Ehgamberdiev, Daniel J. Scheeres, P. Scheirich, Amadeo Aznar, Adrian Galad, J. L. Ortiz, Yu. N. Krugly, Donald P. Pray, Doeon Kim, T. Hromakina, David Vokrouhlický, Walter R. Cooney, Marek Husárik, Audrey Thirouin, O. A. Burkhonov, Joe Pollock, Peter Kusnirak, N. Moskovitz, P. Fatka, Dirk Terrell, Miquel Serra-Ricart, Nicolás Morales, Frédéric Vachier, Stephen M. Slivan, Julian Oey, François Colas, Jozef Vilagi, Leonard Kornoš, Igor Molotov, Rupak Roy, David Polishook, Josef Ďurech, V. R. Ayvazian, Kamil Hornoch, I. Slyusarev, R. Ya. Inasaridze, F. Marchis, Hana Kučáková, John Gross, Brian A. Skiff, J. Vrastil, Raoul Behrend, Peter Vereš
Přispěvatelé: Junta de Andalucía, Slovak Academy of Sciences, Shota Rustaveli National Science Foundation, Ministry of Innovative Development (Uzbekistan), Charles University (Czech Republic), Ministerio de Economía, Industria y Competitividad (España), l'Observatoire de Paris, Government of Czech Republic, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Jazyk: angličtina
Rok vydání: 2019
Předmět:
Zdroj: Digital.CSIC. Repositorio Institucional del CSIC
instname
Icarus
Icarus, Elsevier, 2019, 333, pp.429-463. ⟨10.1016/j.icarus.2019.05.014⟩
Icarus, 2019, 333, pp.429-463. ⟨10.1016/j.icarus.2019.05.014⟩
ISSN: 0019-1035
1090-2643
DOI: 10.1016/j.icarus.2019.05.014⟩
Popis: We studied a sample of 93 asteroid pairs, i.e., pairs of genetically related asteroids that are on highly similar heliocentric orbits. We estimated times elapsed since separation of pair members (i.e., pair age) that are between 7 × 10 yr and a few 10 yr. With photometric observations, we derived the rotation periods P for all the primaries (i.e., the larger members of asteroid pairs) and a sample of secondaries (the smaller pair members). We derived the absolute magnitude differences of the studied asteroid pairs that provide their mass ratios q. For a part of the studied pairs, we refined their WISE geometric albedos and collected or estimated their taxonomic classifications. For 17 asteroid pairs, we also determined their pole positions. In two pairs where we obtained the spin poles for both pair components, we saw the same sense of rotation for both components and constrained the angles between their original spin vectors at the time of their separation. We found that the primaries of 13 asteroid pairs in our sample are actually binary or triple systems, i.e., they have one or two bound, orbiting secondaries (satellites). As a by-product, we found also 3 new young asteroid clusters (each of them consisting of three known asteroids on highly similar heliocentric orbits). We compared the obtained asteroid pair data with theoretical predictions and discussed their implications. We found that 86 of the 93 studied asteroid pairs follow the trend of primary rotation period vs mass ratio that was found by Pravec et al. (2010). Of the 7 outliers, 3 appear insignificant (may be due to our uncertain or incomplete knowledge of the three pairs), but 4 are high mass ratio pairs that were unpredicted by the theory of asteroid pair formation by rotational fission. We discuss a (remotely) possible way that they could be created by rotational fission of flattened parent bodies followed by re-shaping of the formed components. The 13 asteroid pairs with binary primaries are particularly interesting systems that place important constraints on formation and evolution of asteroid pairs. We present two hypotheses for their formation: The asteroid pairs having both bound and unbound secondaries could be “failed asteroid clusters”, or they could be formed by a cascade primary spin fission process. Further studies are needed to reveal which of these two hypotheses for formation of the paired binary systems is real.
The work at Ondfejov Observatory and Charles University Prague and observations with the Danish 1.54-m telescope on the ESO La Silla station were supported by the Grant Agency of the Czech Republic, Grant 17-00774S. Petr Fatka was supported by the Charles University, project GA UK No. 842218. Access to computing and storage facilities owned by parties and projects contributing to the National Grid Infrastructure MetaCentrum provided under the program >Projects of Large Research, Development, and Innovations Infrastructures> (CESNET LM2015042), and the CERIT Scientific Cloud LM2015085, is greatly appreciated. Operations at Sugarloaf Mountain Observatory and Blue Mountains Observatory were supported by a Gene Shoemaker NEO grant from the Planetary Society. We thank to A. Golubaev for his contribution to processing of the observations from Kharkiv Observatory. The observations at Maidanak Observatory were supported by grants F2 -FA -F026 and VA -FA -F-2-010 of the Ministry of Innovative Development of Uzbekistan. Jose Luis Ortiz acknowledges a support by the Spanish project AYA2017-89637-R and Andalusian project P12-FQM1776.The work at Tatranska Lomnica was supported by the Slovak Grant Agency for Science VEGA, Grant No. 2/0023/18, and project ITMS No. 26220120029, based on the supporting operational Research and Development program financed from the European Regional Development Fund. David Polishook is grateful to the AXA research fund for their generous postdoctoral fellowship. Josef Hanug> work was also supported by the Charles University Research program No. UNCE/SCl/023. The work at Abastumani was supported by the Shota Rustaveli National Science Foundation, Grant FR/379/6300/14. The work at Modra was supported by the Slovak Grant Agency for Science VEGA, Grant 1/0911/17. We thank the AGORA association which administrates the 60 -cm telescope at Reunion Les Makes observatory, under a financial agreement with Paris Observatory.
Databáze: OpenAIRE
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