MIRO: Microwave Instrument for Rosetta Orbiter
MIRO: Microwave Instrument for Rosetta Orbiter
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DOI：
10.1007/s11214-006-9032-y
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发表时间：
2007-05
影响因子：
10.3
通讯作者：
S. Gulkis;M. Frerking;J. Crovisier;G. Beaudin;P. Hartogh;P. Encrenaz;T. Koch;C. Kahn;Y. Salinas;R. Nowicki;R. Irigoyen;M. Janssen;P. Stek;M. Hofstadter;M. Allen;C. Backus;L. Kamp;C. Jarchow;E. Steinmetz;A. Deschamps;J. Krieg;M. Gheudin;D. Bockelée-Morvan;N. Biver;T. Encrenaz;D. Despois;W. Ip;E. Lellouch;I. Mann;D. Muhleman;H. Rauer;P. Schloerb;T. Spilker
中科院分区：
文献类型：
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作者：
S. Gulkis;M. Frerking;J. Crovisier;G. Beaudin;P. Hartogh;P. Encrenaz;T. Koch;C. Kahn;Y. Salinas;R. Nowicki;R. Irigoyen;M. Janssen;P. Stek;M. Hofstadter;M. Allen;C. Backus;L. Kamp;C. Jarchow;E. Steinmetz;A. Deschamps;J. Krieg;M. Gheudin;D. Bockelée-Morvan;N. Biver;T. Encrenaz;D. Despois;W. Ip;E. Lellouch;I. Mann;D. Muhleman;H. Rauer;P. Schloerb;T. Spilker
2004年3月2日，欧洲航天局向67 P/丘留莫夫-格拉西缅科彗星发射的罗塞塔号航天器携带了一个相对较小且重量较轻的毫米-亚毫米光谱仪，这是第一个发射到深空的同类仪器。该仪器将用于研究目标彗星释气水和其他分子随日心距离的变化。在2008年和2010年分别飞越小行星（2867）Steins和（21）Lutetia期间，该仪器将测量这些小行星附近的热辐射并寻找水蒸气，该仪器名为MIRO（罗塞塔轨道器微波仪器），包括一个直径30厘米的偏置抛物面反射镜望远镜和两个外差接收器。接收器的中心带工作频率接近190 GHz（1.6 mm）和562 GHz（0.5 mm）。在两个频带上都采用了宽带连续通道，用于测量67 P/Churyumov-Gerasimenko彗星和小行星（2867）Steins和（21）Lutetia的近表面温度和温度梯度。具有180 MHz总带宽和44 kHz分辨率的4096通道CTS（线性调频变换光谱仪）光谱仪除了连续通道之外还连接到亚毫米接收器。亚毫米辐射计/光谱仪是固定调谐测量四个挥发性物种- CO，CH 3OH，NH3和三个，氧相关的同位素水，H216 O，H217 O和H218 O。用MIRO仪器测量的基本数量是表面温度、气体产生率和相对丰度、每种物质的速度和激发温度沿着空间和时间变异性。本文提供了一个简短的讨论调查的科学目标，并详细讨论了MIRO仪器系统。
The European Space Agency Rosetta Spacecraft, launched on March 2, 2004 toward Comet 67P/Churyumov-Gerasimenko, carries a relatively small and lightweight millimeter-submillimeter spectrometer instrument, the first of its kind launched into deep space. The instrument will be used to study the evolution of outgassing water and other molecules from the target comet as a function of heliocentric distance. During flybys of the asteroids (2867) Steins and (21) Lutetia in 2008 and 2010 respectively, the instrument will measure thermal emission and search for water vapor in the vicinity of these asteroids.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 (0.5 mm). Broadband continuum channels are implemented in both frequency bands for the measurement of near surface temperatures and temperature gradients in Comet 67P/Churyumov-Gerasimenko and the asteroids (2867) Steins and (21) Lutetia. A 4096 channel CTS (Chirp Transform Spectrometer) spectrometer having 180 MHz total bandwidth and 44 kHz resolution is, in addition to the continuum channel, connected to the submillimeter receiver. The submillimeter radiometer/spectrometer is fixed tuned to measure four volatile species – CO, CH3OH, NH3and three, oxygen-related isotopologues of water, H216O, H217O and H218O. The basic quantities measured with the MIRO instrument are surface temperature, gas production rates and relative abundances, and velocity and excitation temperature of each species, along with their spatial and temporal variability. This paper provides a short discussion of the scientific objectives of the investigation, and a detailed discussion of the MIRO instrument system.