TY  - JOUR
T1  - Asteroid pairs: A complex picture
A1  - Pravec, P.
A1  - Fatka, P.
A1  - Vokrouhlický, D.
A1  - Scheirich, P.
A1  - Ďurech, J.
A1  - Scheeres, D. J.
A1  - Kušnirák, P.
A1  - Hornoch, K.
A1  - Galád, A.
A1  - Pray, D. P.
A1  - Krugly, Yu. N.
A1  - Burkhonov, O.
A1  - Ehgamberdiev, Sh. A.
A1  - Pollock, J.
A1  - Moskovitz, N.
A1  - Thirouin, A.
A1  - Ortiz, J. L.
A1  - Morales, N.
A1  - Husárik, M.
A1  - Inasaridze, R. Ya.
A1  - Oey, J.
A1  - Polishook, D.
A1  - Hanuš, J.
A1  - Kučáková, H.
A1  - Vraštil, J.
A1  - Világi, J.
A1  - Gajdoš, Š.
A1  - Kornoš, L.
A1  - Vereš, P.
A1  - Gaftonyuk, N. M.
A1  - Hromakina, T.
A1  - Sergeyev, A. V.
A1  - Slyusarev, I. G.
A1  - Ayvazian, V. R.
A1  - Cooney, W. R.
A1  - Gross, J.
A1  - Terrell, D.
A1  - Colas, F.
A1  - Vachier, F.
A1  - Slivan, S.
A1  - Skiff, B.
A1  - Marchis, F.
A1  - Ergashev, K. E.
A1  - Kim, D. -H.
A1  - Aznar, A.
A1  - Serra-Ricart, M.
A1  - Behrend, R.
A1  - Roy, R.
A1  - Manzini, F.
A1  - Molotov, I. E.
JA  - Icarus
Y1  - 2019
VL  - 333
SP  - 429
EP  - 463
SN  - 0019-1035
UR  - https://ui.adsabs.harvard.edu/abs/2019Icar..333..429P
KW  - Asteroids
KW  - Astrophysics - Earth and Planetary Astrophysics
KW  - Dynamics
KW  - Photometry
KW  - Rotation
N2  - We studied a sample of 93 asteroid pairs, i.e., pairs of genetically
M1  - ={related asteroids that are on highly similar heliocentric orbits. We
M1  -  estimated times elapsed since separation of pair members (i.e.
M1  -  pair
M1  -  age) that are between 7 × 10<SUP>3</SUP> yr and a few 10<SUP>6</SUP> yr.
M1  -  With photometric observations
M1  -  we derived the rotation periods
M1  -  P<SUB>1</SUB> for all the primaries (i.e.
M1  -  the larger members of
M1  -  asteroid pairs) and a sample of secondaries (the smaller pair members).
M1  -  We derived the absolute magnitude differences of the studied asteroid
M1  -  pairs that provide their mass ratios q. For a part of the studied pairs
M1  -  we refined their WISE geometric albedos and collected or estimated their
M1  -  taxonomic classifications. For 17 asteroid pairs
M1  -  we also determined
M1  -  their pole positions. In two pairs where we obtained the spin poles for
M1  -  both pair components
M1  -  we saw the same sense of rotation for both
M1  -  components and constrained the angles between their original spin
M1  -  vectors at the time of their separation. We found that the primaries of
M1  -  13 asteroid pairs in our sample are actually binary or triple systems
M1  -  i.e.
M1  -  they have one or two bound
M1  -  orbiting secondaries (satellites). As
M1  -  a by-product
M1  -  we found also 3 new young asteroid clusters (each of them
M1  -  consisting of three known asteroids on highly similar heliocentric
M1  -  orbits). We compared the obtained asteroid pair data with theoretical
M1  -  predictions and discussed their implications. We found that 86 of the 93
M1  -  studied asteroid pairs follow the trend of primary rotation period vs
M1  -  mass ratio that was found by Pravec et al. (2010). Of the 7 outliers
M1  -  3
M1  -  appear insignificant (may be due to our uncertain or incomplete
M1  -  knowledge of the three pairs)
M1  -  but 4 are high mass ratio pairs that were
M1  -  unpredicted by the theory of asteroid pair formation by rotational
M1  -  fission. We discuss a (remotely) possible way that they could be created
M1  -  by rotational fission of flattened parent bodies followed by re-shaping
M1  -  of the formed components. The 13 asteroid pairs with binary primaries
M1  -  are particularly interesting systems that place important constraints on
M1  -  formation and evolution of asteroid pairs. We present two hypotheses for
M1  -  their formation: The asteroid pairs having both bound and unbound
M1  -  secondaries could be "failed asteroid clusters"
M1  -  or they could be formed
M1  -  by a cascade primary spin fission process. Further studies are needed to
M1  -  reveal which of these two hypotheses for formation of the paired binary
M1  -  systems is real.
M1  -  10.1016/j.icarus.2019.05.014
M1  -  eprint: arXiv:1901.05492}
ER  -