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首页> 外文期刊>Planetary and space science >Linear high resolution dust mass spectrometer for a mission to the Galilean satellites
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Linear high resolution dust mass spectrometer for a mission to the Galilean satellites

机译：线性高分辨率尘埃质谱仪，用于执行伽利略卫星的任务

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摘要

The discovery of volcanic activity on Enceladus stands out amongst the long list of findings by the Cassini mission to Saturn. In particular the compositional analysis of Enceladus ice particles by Cassini's Cosmic Dust Analyser (CDA) (Srama et al., 2004) has proven to be a powerful technique for obtaining information about processes below the moon's ice crust. Small amounts of sodium salts embedded in the particles' ice matrices provide direct evidence for a subsurface liquid water reservoir, which is, or has been, in contact with the moon's rocky core (Postberg et al., 2009, 2011b).Jupiter's Galilean satellites Ganymede, Europa, and Callisto are also believed to have subsurface oceans and are therefore prime targets for future NASA and ESA outer Solar System missions. The Galilean moons are engulfed in tenuous dust clouds consisting of tiny pieces of the moons' surfaces (Krueger et al., 1999), released by hypervelocity impacts of micrometeoroids, which steadily bombard the surfaces of the moons. In situ chemical analysis of these grains by a high resolution dust spectrometer will provide spatially resolved mapping of the surface composition of Europa, Ganymede, and Callisto, meeting key scientific objectives of the planned missions. However, novel high-resolution reflectron-type dust mass spectrometers (Sternovsky et al., 2007; Srama et al., 2007) developed for dust astronomy missions (Gruen et al., 2009) are probably not robust enough to be operated in the energetic radiation environment of the inner Jovian system. In contrast, CDA's linear spectrometer is much less affected by harsh radiation conditions because its ion detector is not directly facing out into space. The instrument has been continuously operated on Cassini for 11 years. In this paper we investigate the possibility of operating a CDA-like instrument as a high resolution impact mass spectrometer. We show that such an instrument is capable of reliably identifying traces of organic and inorganic materials in the ice matrix of ejecta expected to be generated from the surfaces of the Galilean moons. These measurements are complementary, and in some cases superior, compared to other traditional techniques such as infrared remote sensing or in situ ion or neutral mass spectrometers.
机译：卡塞尼号飞赴土星的一长串发现中，在土卫二上的火山活动发现突出。特别是通过卡西尼号的宇宙尘埃分析仪（CDA）对土卫二冰粒的成分分析（Srama等，2004）已被证明是一种获取月球冰壳下方过程信息的有力技术。木星的伽利略卫星是埋藏在颗粒冰基质中的少量钠盐的直接证据，表明它已经或已经与月球的岩心接触（Postberg等，2009,2011b）。人们还认为木卫三，欧罗巴和卡利斯托具有地下海洋，因此是未来NASA和ESA太阳系外任务的主要目标。伽利略卫星被微小的类流星体的超高速撞击所释放，并吞没了由微小的月球表面组成的微弱的尘埃云（Krueger等，1999），并不断轰击月球表面。通过高分辨率尘埃光谱仪对这些谷物进行原位化学分析，将提供欧罗巴，木卫三和卡利斯托的表面成分的空间分辨地图，可满足计划任务的关键科学目标。但是，为尘埃天文学任务（Gruen等，2009）开发的新型高分辨率反射电子式尘埃质谱仪（Sternovsky等，2007； Srama等，2007）可能不够坚固，无法在尘埃天文学中使用。内部木星系统的高能辐射环境。相比之下，CDA的线性光谱仪受苛刻的辐射条件的影响要小得多，因为其离子检测器不会直接面向太空。该仪器已在卡西尼号上连续运行11年。在本文中，我们研究了将类CDA仪器用作高分辨率冲击质谱仪的可能性。我们表明，这种仪器能够可靠地识别出预期从伽利略卫星的表面产生的喷射的冰基质中的有机和无机物质的痕迹。与其他传统技术（例如红外遥感或原位离子或中性质谱仪）相比，这些测量是互补的，在某些情况下甚至更好。

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  • 来源
    《Planetary and space science》 |2012年第1期|p.10-20|共11页
  • 作者

    Sascha Kempf; Ralf Srama; Eberhard Gruen; Anna Mocker; Frank Postberg; Jon K. Hillier; Mihaly Horanyi; Zoltan Sternovsky; Bernd Abel; Alexander Beinsen; Roland Thissen; Jiirgen Schmidt; Frank Spahn; Nicolas Altobelli;

  • 作者单位

    MSP and CCLDAS, University of Colorado, 1234 Innovation Drive, Boulder, CO 80303, USA,Institut fuer Ceophysik und extraterrestrische Physik, Universitaet Braunschweig, Mendelssohnstr. 3, 38106 Braunschweig, Germany;

    Institut fuer Raumfahrtsysteme, Universitaet Stuttgaert, Pfaffenwaldring 31, 70569 Stuttgart, Germany;

    Max-Ptanck-Institut fuer Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany,MSP and CCLDAS, University of Colorado, 1234 Innovation Drive, Boulder, CO 80303, USA;

    Institut fuer Raumfahrtsysteme, Universitaet Stuttgaert, Pfaffenwaldring 31, 70569 Stuttgart, Germany;

    Institut fuer Geowissenschaften, Universitaet Heidelberg, Im Neuenheimer Feld 236, 69120 Heidelberg, Germany;

    Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK;

    MSP and CCLDAS, University of Colorado, 1234 Innovation Drive, Boulder, CO 80303, USA;

    MSP and CCLDAS, University of Colorado, 1234 Innovation Drive, Boulder, CO 80303, USA;

    Wilhelm-Ostwald-Institut fur Physikalische und Theoretische Chemie, Universitat Leipzig, Linne-Strasse 2, 04103 Leipzig, Germany;

    Wilhelm-Ostwald-Institut fur Physikalische und Theoretische Chemie, Universitat Leipzig, Linne-Strasse 2, 04103 Leipzig, Germany;

    UJF-Grenoble 1/CNRS-INSU, Institut de Planetologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble F-38041, France;

    Institut fur Physik, Universitat Potsdam, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam-Golm, Germany;

    Institut fur Physik, Universitat Potsdam, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam-Golm, Germany;

    ESA-ESAC, P.O. Box 78, E-28691 Villanueva de la Canada, Madrid, Spain;

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  • 正文语种 eng
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  • 关键词

    europa; ganymede; callisto; surface composition; mass spectroscopy; dust;

    机译：欧罗巴ganymede卡利斯托表面成分质谱;灰尘;

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