Thermal inertia and roughness of the nucleus of comet 67P/Churyumov-Gerasimenko from MIRO and VIRTIS observations

被引:43
|
作者
Marshall, D. [1 ,2 ]
Groussin, O. [3 ]
Vincent, J. -B. [4 ]
Brouet, Y. [5 ]
Kappel, D. [4 ]
Arnold, G. [4 ]
Capria, M. T. [6 ]
Filacchione, G. [6 ]
Hartogh, P. [1 ]
Hofstadter, M. [7 ]
Ip, W. -H. [8 ]
Jorda, L. [3 ]
Kuehrt, E. [4 ]
Lellouch, E. [9 ]
Mottola, S. [4 ]
Rezac, L. [1 ]
Rodrigo, R. [10 ]
Rodionov, S. [3 ]
Schloerb, P. [7 ]
Thomas, N. [5 ]
机构
[1] Max Planck Inst Stromungsforsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany
[2] Univ Gottingen, Friedrich Hund Pl 1, D-37077 Gottingen, Germany
[3] Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
[4] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch Asteroiden & Kometen, Rutherfordstr 2, D-12489 Berlin, Germany
[5] Univ Bern, Phys Inst, Sidlerstr 5, CH-3012 Bern, Switzerland
[6] INAF, IAPS, Rome, Italy
[7] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA
[8] Natl Cent Univ, Grad Inst Astron, 300 Chung Da Rd, Chungli 32054, Taiwan
[9] Univ Paris Diderot, UPMC, CNRS, LESIA Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France
[10] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland
来源
ASTRONOMY & ASTROPHYSICS | 2018年 / 616卷
基金
欧盟地平线“2020”;
关键词
comets: individual: 67P/Churyumov-Gerasimenko; planets and satellites: surfaces; instrumentation: spectrographs; methods: data analysis; DIELECTRIC-PROPERTIES; SPECTROMETER; SHAPE;
D O I
10.1051/0004-6361/201833104
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. Using data from the Rosetta mission to comet 67P/Churyumov-Gerasimenko, we evaluate the physical properties of the surface and subsurface of the nucleus and derive estimates for the thermal inertia (TI) and roughness in several regions on the largest lobe of the nucleus. Methods. We have developed a thermal model to compute the temperature on the surface and in the uppermost subsurface layers of the nucleus. The model takes heat conduction, self-heating, and shadowing effects into account. To reproduce the brightness temperatures measured by the MIRO instrument, the thermal model is coupled to a radiative transfer model to derive the TI. To reproduce the spatially resolved infrared measurements of the VIRTIS instrument, the thermal model is coupled to a radiance model to derive the TI and surface roughness. These methods are applied to Rosetta data from September 2014. Results. The resulting TI values from both instruments are broadly consistent with each other. From the millimetre channel on MIRO, we determine the TI in the subsurface to be < 80 JK(-1) m(2) s 0 : 5 for the Seth, Ash, and Aten regions. The submillimetre channel implies similar results but also suggests that higher values could be possible. A low TI is consistent with other MIRO measurements and in situ data from the MUPUS instrument at the final landing site of Philae. The VIRTIS results give a best-fitting value of 80 JK(-1) m(2) s 0 : 5 and values in the range 40-160 JK(-1) m(2) s 0 : 5 in the same areas. These observations also allow the subpixel scale surface roughness to be estimated and compared to images from the OSIRIS camera. The VIRTIS data imply that there is significant roughness on the infrared scale below the resolution of the available shape model and that, counter-intuitively, visually smooth terrain (centimetre scale) can be rough at small (micrometre-millimetre) scales, and visually rough terrain can be smooth at small scales.
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页数:13
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