Rotating dust particles in the coma of comet 67P/Churyumov-Gerasimenko

被引：28

作者：

Fulle, M. ^{[1
]}

Ivanovski, S. L. ^{[2
]}

Bertini, I. ^{[3
]}

Gutierrez, P. ^{[4
]}

Lara, L. ^{[4
]}

Sierks, H. ^{[5
]}

Zakharov, V. ^{[6
]}

Della Corte, V. ^{[2
]}

Rotundi, A. ^{[2
,7
]}

Barbieri, C. ^{[8
]}

Lamy, P. L. ^{[9
,10
]}

Rodrigo, R. ^{[11
,12
]}

Koschny, D. ^{[13
]}

Rickman, H. ^{[14
,15
]}

Keller, H. U. ^{[16
]}

Agarwal, J. ^{[5
]}

A'Hearn, M. F. ^{[17
]}

Barucci, M. A. ^{[6
]}

Bertaux, J. -L. ^{[18
]}

Bodewits, D. ^{[17
]}

Cremonese, G. ^{[19
]}

Da Deppo, V. ^{[20
]}

Davidsson, B. ^{[14
]}

Debei, S. ^{[21
]}

De Cecco, M. ^{[22
]}

Fornasier, S. ^{[6
]}

Groussin, O. ^{[9
,10
]}

Guettler, C. ^{[5
]}

Hviid, S. F. ^{[23
]}

Ip, W. ^{[24
]}

Jorda, L. ^{[9
,10
]}

Knollenberg, J. ^{[23
]}

Kramm, R. ^{[5
]}

Kuehrt, E. ^{[23
]}

Kueppers, M. ^{[25
]}

Lazzarin, M. ^{[8
]}

Lopez-Moreno, J. J. ^{[4
]}

Marzari, F. ^{[26
]}

Michalik, H. ^{[27
]}

Naletto, G. ^{[3
,21
,28
]}

Oklay, N. ^{[5
]}

Sabau, L. ^{[29
]}

Thomas, N. ^{[30
]}

Tubiana, C. ^{[5
]}

Vincent, J. -B. ^{[5
]}

Wenzel, K. -P. ^{[13
]}

机构：

[1] INAF Osservatorio Astron, I-34143 Trieste, Italy

[2] INAF Ist Astrofis & Planetol Spaziali, Area Ric Tor Vergata, I-00133 Rome, Italy

[3] Univ Padua, CISAS, I-35100 Padua, Italy

[4] Inst Astrofis Andalucia CSIC, Granada 18008, Spain

[5] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany

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

[7] Univ Napoli Parthenope, Dip Sci & Tecnol, I-80143 Naples, Italy

[8] Univ Padua, Dept Phys & Astron, I-35122 Padua, Italy

[9] CNRS, UMR 7326, Lab Astrophys Marseille, F-13388 Marseille, France

[10] Aix Marseille Univ, F-13388 Marseille, France

[11] Ctr Astrobiol INTA CSIC, Madrid 28691, Spain

[12] Int Space Sci Inst, CH-3012 Bern, Switzerland

[13] European Space Agcy, Sci Support Off, NL-2201 Noordwijk, Netherlands

[14] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden

[15] PAS Space Res Ctr, PL-00716 Warsaw, Poland

[16] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany

[17] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[18] CNRS UVSQ IPSL, LATMOS, F-78280 Guyancourt, France

[19] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[20] CNR IFN UOS Padova LUXOR, I-35131 Padua, Italy

[21] Univ Padua, Dept Mech Engn, I-35131 Padua, Italy

[22] Univ Trento, UNITN, I-38100 Trento, Italy

[23] DLR, Inst Planetary Res, D-12489 Berlin, Germany

[24] Natl Cent Univ, Inst Space Sci, Chungli 32054, Taiwan

[25] ESA ESAC, Madrid 28692, Spain

[26] Univ Padua, Dept Phys, I-35131 Padua, Italy

[27] Inst Datentech & Konununikat Netze, D-38106 Braunschweig, Germany

[28] Univ Padua, Dept Informat Engn, I-35131 Padua, Italy

[29] Inst Nacl Tecn Aeroespacial, Madrid 28850, Spain

[30] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 583卷

关键词：

comets: general; comets: individual: 67P/Churyumov-Gerasimenko; methods: numerical; space vehicles; DIRECT MONTE-CARLO; DYNAMICS; NUCLEUS;

D O I：

10.1051/0004-6361/201526158

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. During September and October 2014, the OSIRIS cameras onboard the ESA Rosetta mission detected millions of single particles. Many of these dust particles appear as long tracks (due to both the dust proper motion and the spacecraft motion during the exposure time) with a clear brightness periodicity. Aims. We interpret the observed periodic features as a rotational and translational motion of aspherical dust grains. Methods. By counting the peaks of each track, we obtained statistics of a rotation frequency. We compared these results with the rotational frequency predicted by a model of aspherical dust grain dynamics in a model gas flow. By testing many possible sets of physical conditions and grain characteristics, we constrained the rotational properties of dust grains. Results. We analyzed on the motion of rotating aspherical dust grains with different cross sections in flow conditions corresponding to the coma of 67P/Churyumov-Gerasimenko qualitatively and quantitatively. Based on the OSIRIS observations, we constrain the possible physical parameters of the grains.

引用

页数：8

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