The big lobe of 67P/Churyumov-Gerasimenko comet: morphological and spectrophotometric evidences of layering as from OSIRIS data

被引:7
作者
Ferrari, Sabrina [1 ]
Penasa, L. [1 ]
La Forgia, F. [2 ]
Massironi, M. [1 ,3 ]
Naletto, G. [1 ,4 ,5 ]
Lazzarin, M. [2 ]
Fornasier, S. [6 ]
Hasselmann, P. H. [6 ]
Lucchetti, A. [7 ]
Pajola, M. [7 ]
Ferri, F. [1 ]
Cambianica, P. [1 ]
Oklay, N. [8 ]
Tubiana, C. [9 ]
Sierks, H. [9 ]
Lamy, P. L. [10 ,11 ]
Rodrigo, R. [12 ,13 ]
Koschny, D. [14 ]
Davidsson, B. [15 ]
Barucci, M. A. [6 ]
Bertaux, J. -L. [16 ]
Bertini, I. [2 ]
Bodewits, D. [17 ]
Cremonese, G. [7 ]
Da Deppo, V. [5 ]
Debei, S. [18 ]
De Cecco, M. [19 ]
Deller, J. [9 ]
Franceschi, M. [3 ]
Frattin, E. [2 ,7 ]
Fulle, M. [20 ]
Groussin, O. [21 ]
Gutierrez, P. J. [22 ]
Guettler, C. [9 ]
Hviid, S. F. [8 ]
Ip, W. -H. [23 ,24 ]
Jorda, L. [21 ]
Keller, H. U. [8 ,25 ]
Knollenberg, J. [8 ]
Kuehrt, E. [8 ]
Kuppers, M. [26 ]
Lara, L. M. [22 ]
Lopez-Moreno, J. J. [22 ]
Marzari, F. [4 ]
Shi, X. [9 ]
Simioni, E. [7 ]
Thomas, N. [27 ,28 ]
Vincent, J. -B. [8 ]
机构
[1] Univ Padua, Ctr Studies & Act Space CISAS G Colombo, Via Venezia 15, I-35131 Padua, Italy
[2] Univ Padua, Dept Phys & Astron G Galilei, Vic Osservatorio 3, I-35122 Padua, Italy
[3] Univ Padua, Geosci Dept, Via G Gradenigo 6, I-35131 Padua, Italy
[4] Univ Padua, Dept Phys & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy
[5] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy
[6] Univ Paris 06, UPMC, Sorbonne Paris Cite,Observ Paris,LESIA, Sorbonne Univ,CNRS,Univ Paris Diderot,PSL Res Uni, 5 Pl Jules Janssen, F-92195 Meudon, France
[7] INAF OAPD Astron Observ Padova, Vic Osservatorio 5, I-35122 Padua, Italy
[8] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, Rutherfordstr 23, D-12489 Berlin, Germany
[9] Max Planck Inst Solar Syst Res, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany
[10] CNRS, UMR 7326, Lab Astrophys Marseille, F-13388 Marseille 13, France
[11] Aix Marseille Univ, F-13388 Marseille 13, France
[12] CSIC INTA, Ctr Astrobiol, E-28850 Madrid, Spain
[13] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland
[14] European Space Res & Technol Ctr ESA, Sci Support Off, Keplerlaan 1,Postbus 299, NL-2201 AZ Noordwijk, Netherlands
[15] Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA
[16] LATMOS, CNRS UVSQ IPSL, 11 Blvd Alembert, F-78280 Guyancourt, France
[17] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
[18] Univ Padua, Dept Ind Engn, Via Venezia 1, I-35131 Padua, Italy
[19] Univ Trento, Fac Engn, Via Mesiano 77, I-38121 Trento, Italy
[20] INAF Osservatorio Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy
[21] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France
[22] Inst Astrofis Andalucia CSIC, C Glorieta Astron S-N, E-18008 Granada, Spain
[23] Natl Cent Univ, Grad Inst Astron, 300 Chung Da Rd, Chungli 32054, Taiwan
[24] Macau Univ Sci & Technol, Space Sci Inst, Ave Wai Long, Taipa, Macao, Peoples R China
[25] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Mendelssohnstr 3, D-38106 Braunschweig, Germany
[26] European Space Astron Ctr ESA, Operat Dept, POB 78, E-28691 Madrid, Spain
[27] Univ Bern, Phys Inst, Sidlerstr 5, CH-3012 Bern, Switzerland
[28] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland
关键词
methods: data analysis; techniques: image processing; comets: general; comets: individual: 67P/Churyumov-Gerasimenko; WATER ICE; NUCLEUS;
D O I
10.1093/mnras/sty1656
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Between 2014 and 2016, ESA's Rosetta OSIRIS cameras acquired multiple-filters images of the layered nucleus of comet 67P/Churyumov-Gerasimenko, ranging from ultraviolet to near-infrared wavelengths. No correlation between layers disposition and surface spectral variegation has been observed so far. This paper investigates possible spectral differences among decametre-thickness outcropping layers of the biggest lobe of the comet by means of OSIRIS image dataset. A two-classes maximum likelihood classification was applied on consolidated outcrops and relative deposits identified on post-perihelion multispectral images of the big lobe. We distinguished multispectral data on the basis of the structural elevation of the onion-shell Ellipsoidal Model of 67P. The spatial distribution of the two classes displays a clear dependence on the structural elevation, with the innermost class resulting over 50 per cent brighter than the outermost one. Consolidated cometarymaterials located at different structural levels are characterized by different brightness and revealed due to the selective removal of large volumes. This variegation can be attributed to a different texture of the outcrop surface and/or to a different content of refractory materials.
引用
收藏
页码:1555 / 1568
页数:14
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