The non-convex shape of (234) Barbara, the first Barbarian

被引：15

作者：

Tanga, P. ^{[1
]}

Carry, B. ^{[2
]}

Colas, F. ^{[2
]}

Delbo, M. ^{[1
]}

Matter, A. ^{[1
,3
]}

Hanus, J. ^{[1
,4
]}

Lagoa, V. Ali ^{[1
]}

Andrei, A. H. ^{[5
,6
,7
]}

Assafin, M. ^{[5
]}

Audejean, M. ^{[8
,9
]}

Behrend, R. ^{[8
,10
]}

Camargo, J. I. B. ^{[6
]}

Carbognani, A. ^{[11
]}

Cedres Reyes, M. ^{[12
]}

Conjat, M. ^{[13
]}

Cornero, N. ^{[8
,14
]}

Coward, D. ^{[15
]}

Crippa, R. ^{[8
,16
]}

de Ferra Fantin, E. ^{[12
,17
]}

Devogele, M. ^{[18
]}

Dubos, G. ^{[14
]}

Frappa, E. ^{[19
]}

Gillon, M. ^{[18
]}

Hamanowa, H. ^{[8
,20
]}

Jehin, E. ^{[18
]}

Klotz, A. ^{[21
]}

Kryszczynska, A. ^{[22
]}

Lecacheux, J. ^{[23
]}

Leroy, A. ^{[8
,24
]}

Manfroid, J. ^{[18
]}

Manzini, F. ^{[8
,25
]}

Maquet, L. ^{[2
]}

Morelle, E. ^{[8
]}

Mottola, S. ^{[26
]}

Polinska, M. ^{[22
]}

Roy, R. ^{[8
,27
]}

Todd, M. ^{[15
]}

Vachier, F. ^{[2
]}

Vera Hernandez, C. ^{[12
]}

Wiggins, P. ^{[28
]}

机构：

[1] Observ Cote Azur, UNS, CNRS, UMR7293,Lab Lagrange, F-06304 Nice, France

[2] Observ Paris, CNRS, UMR8028, IMCCE, F-75014 Paris, France

[3] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[4] Charles Univ Prague, Fac Math & Phys, Astron Inst, CR-18000 Prague, Czech Republic

[5] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio de Janeiro, Brazil

[6] MCTI, Observ Nacl, BR-20921400 Rio De Janeiro, Brazil

[7] Observ Paris, SYRTE, F-75014 Paris, France

[8] Observ Geneva, CdR & CdL Grp Lightcurves Minor Planets & Variabl, CH-1290 Sauverny, Switzerland

[9] Observ Chinon, F-37500 Chinon, France

[10] Observ Geneva, CH-1290 Sauverny, Switzerland

[11] Osservatorio Astron Reg Autonoma Valle Aosta, I-11020 Nus, Aosta, Italy

[12] Agrupac Astron Fuerteventura, E-35600 Puerto Del Rosario, Spain

[13] Observ Cabris, F-06530 Cabris, France

[14] AUDE, F-75014 Paris, France

[15] Curtin Univ Technol, Dept Imaging & Appl Phys, Bentley, WA 6102, Australia

[16] Osservatorio Astron Tradate, I-21049 Tradate, Italy

[17] Acad Ciencias & Ingienerias Lanzarote, E-35500 Arrecife, Spain

[18] Univ Liege, Inst Astrophys Geophys & Oceanog, B-4000 Liege, Belgium

[19] Euraster, F-42000 St Etienne, France

[20] Hamanowa Astron Observ, Fukushima 072010, Japan

[21] CNRS, IRAP, F-31028 Toulouse, France

[22] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, PL-67712 Poznan, Poland

[23] Univ Paris 06, CNRS, Observ Paris, LESIA, F-92195 Meudon, France

[24] Assoc T60, F-65400 Arrens Marsous, France

[25] Stn Astron Sozzago, I-28060 Sozzago, Italy

[26] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany

[27] Blauvac Observ, F-66240 St Esteve, France

[28] Wiggins Observ, Tooele, UT 84074 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 448卷 / 04期

关键词：

Techniques: photometric; Techniques: polarimetry; occultations; Minor planets; asteroids:; individual:; 234; Barbara; MAIN BELT ASTEROIDS; ANGULAR-MOMENTUM TRANSFER; SOLAR-SYSTEM BODIES; COLLISIONAL EVOLUTION; POLARIMETRIC BEHAVIOR; LIGHTCURVE INVERSION; DESPINNING ASTEROIDS; OPTIMIZATION METHODS; MASS DISPERSAL; ROTATION;

D O I：

10.1093/mnras/stv229

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Asteroid (234) Barbara is the prototype of a category of asteroids that has been shown to be extremely rich in refractory inclusions, the oldest material ever found in the Solar system. It exhibits several peculiar features, most notably its polarimetric behaviour. In recent years other objects sharing the same property (collectively known as 'Barbarians') have been discovered. Interferometric observations in the mid-infrared with the ESO VLTI (Very Large Telescope Interferometer) suggested that (234) Barbara might have a bi-lobated shape or even a large companion satellite. We use a large set of 57 optical light curves acquired between 1979 and 2014, together with the timings of two stellar occultations in 2009, to determine the rotation period, spin-vector coordinates, and 3-D shape of (234) Barbara, using two different shape reconstruction algorithms. By using the light curves combined to the results obtained from stellar occultations, we are able to show that the shape of (234) Barbara exhibits large concave areas. Possible links of the shape to the polarimetric properties and the object evolution are discussed. We also show that VLTI data can be modelled without the presence of a satellite.

引用

页码：3382 / 3390

页数：9

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