EVOLUTION OF THE DUST SIZE DISTRIBUTION OF COMET 67P/CHURYUMOV-GERASIMENKO FROM 2.2 au TO PERIHELION

被引：169

作者：

Fulle, M. ^{[1
]}

Marzari, F. ^{[2
]}

Della Corte, V. ^{[3
]}

Fornasier, S. ^{[4
]}

Sierks, H. ^{[5
]}

Rotundi, A. ^{[3
,6
]}

Barbieri, C. ^{[7
]}

Lamy, P. L. ^{[8
,9
]}

Rodrigo, R. ^{[10
,11
]}

Koschny, D. ^{[12
]}

Rickman, H. ^{[13
,14
]}

Keller, H. U. ^{[15
]}

Lopez-Moreno, J. J. ^{[16
]}

Accolla, M. ^{[17
]}

Agarwal, J. ^{[5
]}

A'Hearn, M. F. ^{[18
]}

Altobelli, N. ^{[19
]}

Barucci, M. A. ^{[4
]}

Bertaux, J. -L. ^{[20
]}

Bertini, I. ^{[21
]}

Bodewits, D. ^{[18
]}

Bussoletti, E. ^{[6
]}

Colangeli, L. ^{[12
]}

Cosi, M. ^{[22
]}

Cremonese, G. ^{[23
]}

Crifo, J. -F. ^{[20
]}

Da Deppo, V. ^{[24
]}

Davidsson, B. ^{[13
]}

Debei, S. ^{[25
]}

De Cecco, M. ^{[26
]}

Esposito, F. ^{[27
]}

Ferrari, M. ^{[3
]}

Giovane, F. ^{[28
]}

Gustafson, B. ^{[29
]}

Green, S. F. ^{[30
]}

Groussin, O. ^{[8
,9
]}

Gruen, E. ^{[31
]}

Gutierrez, P. ^{[16
]}

Guettler, C. ^{[5
]}

Herranz, M. L. ^{[17
]}

Hviid, S. F. ^{[32
]}

Ip, W. ^{[33
]}

Ivanovski, S. L. ^{[3
]}

Jeronimo, J. M. ^{[16
]}

Jorda, L. ^{[8
,9
]}

Knollenberg, J. ^{[32
]}

Kramm, R. ^{[5
]}

Kuehrt, E. ^{[32
]}

Kueppers, M. ^{[19
]}

Lara, L. ^{[16
]}

机构：

[1] INAF Osservatorio Astron, Via Tiepolo 11, I-34143 Trieste, Italy

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

[3] INAF Ist Astrofis & Planetol Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome, Italy

[4] Univ Paris 06, Sorbonne Univ, Univ Paris Diderot, Observ Paris,LESIA,Observ Paris,PSL Res Univ,CNRS, 5 Pl J Janssen, F-92195 Meudon, France

[5] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany

[6] Univ Napoli Parthenope, Dip Sci & Tecnol, CDN IC4, I-80143 Naples, Italy

[7] Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy

[8] CNRS, UMR 7326, Lab Astrophys Marseilles, F-13388 Marseille 13, France

[9] Aix Marseille Univ, F-13388 Marseille 13, France

[10] Ctr Astrobiol INTA CSIC, E-28691 Madrid, Spain

[11] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland

[12] European Space Agcy, ESA ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

[13] Uppsala Univ, Dept Phys & Astron, Box 516, SE-75120 Uppsala, Sweden

[14] PAS Space Res Ctr, Bartycka 18A, PL-00716 Warsaw, Poland

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

[16] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain

[17] INAF Osservatorio Astrofis Catania, Via Santa Sofia 78, I-95123 Catania, Italy

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

[19] ESA ESAC, Camino Bajo Castillo S-N, Madrid 28692, Spain

[20] CNRS UVSQ IPSL, LATMOS, 11 Blvd Alembert, F-78280 Guyancourt, France

[21] Univ Padua, CISAS, Via Venezia 15, I-35100 Padua, Italy

[22] Selex ES, Via A Einstein 35, I-50013 Campi Bisenzio, FI, Italy

[23] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[24] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy

[25] Univ Padua, Dept Mech Engn, Via Venezia 1, I-35131 Padua, Italy

[26] Univ Trent, UNITN, Via Mesiano 77, I-38100 Trento, Italy

[27] INAF Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80133 Naples, Italy

[28] Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA

[29] Univ Florida, Gainesville, FL 32611 USA

[30] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England

[31] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany

[32] DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany

[33] Natl Cent Univ, Inst Space Sci, 300 Chung Da Rd, Chungli 32054, Taiwan

[34] INAF Osservatorio Astron Roma, Via Frascati 33, Rome, Italy

[35] Univ Kent, Sch Phys Sci, Canterbury CT2 7NZ, Kent, England

[36] UnispaceKent, Canterbury CT2 8EF, Kent, England

[37] Univ Granada, Fac Ciencias, Dept Fis Aplicada, Avda Severo Ochoa S-N, E-18071 Granada, Spain

[38] Univ Padua, Dept Informat Engn, Via Gradenigo 6, I-35131 Padua, Italy

[39] Observ Haute Provence, OSU Pythas UMS CNRS AMU 2244, F-04870 St Michel lObservatoire, France

[40] 1 Univ New Mexico, Dept Earth & Planetary Sci, MSC03 2040, Albuquerque, NM 87131 USA

[41] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland

[42] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA

来源：

ASTROPHYSICAL JOURNAL | 2016年 / 821卷 / 01期

关键词：

comets: general; comets: individual (67P/Churyumov-Gerasimenko); space vehicles: instruments; ROSETTA MISSION; NUCLEUS; ICE; PARTICLES; ORBITS; OSIRIS;

D O I：

10.3847/0004-637X/821/1/19

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Rosetta probe, orbiting Jupiter-family comet 67P/Churyumov-Gerasimenko, has been detecting individual dust particles of mass larger than 10(-10) kg by means of the GIADA dust collector and the OSIRIS Wide Angle Camera and Narrow Angle Camera since 2014 August and will continue until 2016 September. Detections of single dust particles allow us to estimate the anisotropic dust flux from 67P, infer the dust loss rate and size distribution at the surface of the sunlit nucleus, and see whether the dust size distribution of 67P evolves in time. The velocity of the Rosetta orbiter, relative to 67P, is much lower than the dust velocity measured by GIADA, thus dust counts when GIADA is nadir-pointing will directly provide the dust flux. In OSIRIS observations, the dust flux is derived from the measurement of the dust space density close to the spacecraft. Under the assumption of radial expansion of the dust, observations in the nadir direction provide the distance of the particles by measuring their trail length, with a parallax baseline determined by the motion of the spacecraft. The dust size distribution at sizes > 1 mm observed by OSIRIS is consistent with a differential power index of -4, which was derived from models of 67P's trail. At sizes <1 mm, the size distribution observed by GIADA shows a strong time evolution, with a differential power index drifting from -2 beyond 2 au to -3.7 at perihelion, in agreement with the evolution derived from coma and tail models based on ground-based data. The refractory-to-water mass ratio of the nucleus is close to six during the entire inbound orbit and at perihelion.

引用

页数：14

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