Millimeter and submillimeter measurements of asteroid (2867) Steins during the Rosetta fly-by

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• 作者：S. Gulkis ; S. Keihm ; L. Kamp ; C. Backus ; M. Janssen ; S. Lee ; B. Davidsson ; G. Beaudin ; N. Biver ; D. Bockelé ; e-Morvan ; J. Crovisier ; P. Encrenaz ; T. Encrenaz ; P. Hartogh ; M. Hofstadter ; W. Ip ; E. L
• 关键词：Rosetta spacecraft ; Asteroid (2867) Steins ; Millimeter and submillimeter radiometer/spectrometer
• 刊名：Planetary and Space Science
• 出版年：2010
• 出版时间：July 2010
• 年：2010
• 卷：58
• 期：9
• 页码：1077-1087
• 全文大小：792 K

文摘

The European Space Agency Rosetta Spacecraft passed within 803 km of the main belt asteroid (2867) Steins on 5 September 2008. The Rosetta Spacecraft carries a number of scientific instruments including a millimeter and submillimeter radiometer and spectrometer. The instrument, named MIRO (Microwave Instrument for the Rosetta Orbiter), consists of a 30-cm diameter, offset parabolic reflector telescope followed by two heterodyne receivers. Center-band operating frequencies of the receivers are near 190 GHz (1.6 mm) and 562 GHz (0.53 mm). Broadband continuum channels are implemented in both frequency bands for the measurement of near surface temperatures and temperature gradients. A 4096 channel CTS (chirp transform spectrometer) having 180 MHz total bandwidth and 44 kHz resolution is also connected to the submillimeter receiver. We present the continuum observations of asteroid (2867) Steins obtained during the fly-by with the MIRO instrument. Spectroscopic data were also collected during the fly-by using the MIRO spectrometer fixed-tuned to rotational lines of several molecules. Results of the spectroscopic investigation will be the topic of a separate publication.<p>Comparative thermal models and radiative transfer calculations for Steins are presented. Emissivities of Steins were determined to be 0.6–0.7 and 0.85–0.9 at wavelengths of 0.53 and 1.6 mm, respectively. The thermal inertia of Steins was estimated to be in the range 450–850 J/(mp>2p> sp>0.5p> K). Assuming that the emissivity of Steins is determined by the Fresnel reflection coefficients of the surface material, the area-averaged dielectric constant of the surface material is in the range 4–20. These values are rock-like, and are unlike the powdered-regolith surface of the Moon.