In-situ-analysis of ice particles in the solar system: application, methods, instrument developement

太阳系外凝聚态物质的大部分(大致从小行星带开始)由水冰组成。目前关于冰面和冰粒组成的发现几乎完全基于吸收光谱，特别是在红外范围内。然而，通过这种方式，嵌入到水冰基质中的化合物只能在一定程度上进行研究。这尤其适用于无机组分，它们在红外范围内通常只有轻微的活性或甚至不活性。许多有机化合物也很难用吸收光谱学来识别，更不用说定量了。所请求的资金与海森伯格奖学金相结合的综合目标是通过一种新方法来描述太阳系冰体的化学特征。这是通过对太空中的冰粒进行原位质谱分析来完成的，这些冰粒以高速与适当的探测器相撞。如果粒子的起源是已知的，也可以确定母体的组成和地球化学性质。卡西尼号的宇宙尘埃分析器(CDA)已经令人印象深刻地展示了这种方法的能力，它特别适合于冰冷物质，并补充了吸收光谱。在拟议的研究方案框架内，应应用并进一步发展现场质谱学。为此目的，将分析当前空间飞行任务(卡西尼号、罗塞塔号)的数据，并为未来的飞行任务做好最佳科学返回的准备。这一点得到了一系列实验室实验的支持，这些实验使用的是结冰的模拟材料。在分项目1中，以前使用Cassini-CDA数据的工作将扩展到一个质的新水平。该目标是对土星系统中冰物质组成的全面、系统的描述。由此，可以对土星环系及其冷火山活动的冰面卫星土卫二的组成有全面的了解。土卫二冰泉从月球冰壳的温暖裂缝中涌出，由液态水提供，可能提供有关月球天体生物潜力的有价值的信息。CDA质谱学解释的一个核心资源将是使用分项目2中所述的模拟实验。这些装置模拟冰粒高速撞击探测器板，对解释空间数据非常有帮助。然而，这种方法不仅适用于CDA光谱，而且还适用于其他当前或未来空间飞行任务的数据，例如Rosetta。将利用和进一步扩大现有的国家和国际合作和投资

The better part of condensed matter in the outer solar system (beginning roughly at the asteroid belt) consists of water ice. Current findings on the composition of icy surfaces and particles are almost exclusively based on absorption-spectroscopy, particularly in the infrared range. However, in this way, compounds that are embedded in a water ice matrix can only be investigated to a certain degree. This applies in particular to anorganic components, which are often only slightly active or even inactive in the infrared range. Many organic compounds are also difficult to identify, much less to quantify, by absorption-spectroscopy.The comprehensive goal of the requested funds, conjoint with a Heisenberg Fellowship, is the chemical characterisation of icy bodies in the solar system by means of a new method. This is done through in situ mass spectrometry of ice particles in space, which collide with the appropriate detectors at high speed. If the particles' origins are known, the composition and geochemistry of the mother body can also be characterised. This approach, the capabilities of which have been impressively shown through Cassini's Cosmic Dust Analyser (CDA), is particularly well suited to icy materials and complements absorption-spectroscopy. Within the framework of the proposed research programme, the in situ mass spectrometry shall be applied and further developed. For that purpose, data from current space missions (Cassini, Rosetta) will be analysed and future missions will be prepared for an optimal science return. This is supported by a series of lab experiments with icy analogue materials. In sub-project 1, the previous work with Cassini-CDA data will be expanded to a qualitatively new level. The target is a comprehensive, systematic description of the composition of icy materials in the Saturnian system. From this, comprehensive insights into the composition of Saturn's ring system and its cryo-volcanic active icy moon Enceladus can be derived. Enceladus ice fountains, which emerge through warm cracks in the moon's icy crust, are fed by liquid water and may provide valuable information about the moon's astrobiological potential. A core resource for the interpretation of CDA mass spectra will be the use of the analogue experiments as described in sub-project 2. These devices simulate high-speed impacts of ice particles onto the detector plate and are extremely helpful in the interpretation of space data. However, this method applies not only to CDA spectra, but also to the data of other current or future space missions, e.g. Rosetta. Existing national and international cooperations and investments will be used and further expanded