Observations and radiation transfer modelling of the solar chromosphere

阿塔卡马大毫米阵列(ALMA)是一种主要的新型天文仪器，波长为毫米和亚毫米。在2017年，ALMA的第一次定期太阳观测打开了在这些波长的太阳的新视野。我们小组已经获得了ALMA的观测时间来研究太阳大气(如暗条、日冕、活动区苔藓)，并将继续寻找更多的观测时间来研究太阳最低活动附近的太阳。这些观测将得到一系列陆基和天基仪器的广泛支持，通过光谱的光学和红外部分实现从极端紫外线到射电领域的全面覆盖。学生将进行ALMA和其他观测的分析和解释，并利用它们来促进我们对太阳等离子体内的条件以及与微小尺度结构的加热和冷却相关的过程的理解。他还将为在ALMA和其他英国设施上进一步观察时间的申请做出贡献。随着工作的进展和详细的物理问题的出现，数据分析和解释最终将得到辐射传输模型的补充。

The Atacama Large Millimetre Array (ALMA) is a major new instrument for Astronomy at mm and sub-mm wavelengths. During 2017 the first regular solar observations with ALMA opened up a new view of the Sun at those wavelengths. Our group has obtained observing time with ALMA to study the solar atmosphere (e.g. filaments, prominences, active region moss) and will continue to seek more observing time to study the Sun around its minimum activity. These observations will be widely supported by a range of ground-based and space-based instruments, bringing a comprehensive coverage from the extreme-ultraviolet to the radio domains via optical and infrared parts of the spectrum. The student will carry out the analysis and interpretation of ALMA and other observations, and use them to advance our understanding of the conditions within the solar plasma and of processes associated with heating and cooling of fine-scale structures. He will also contribute to applications for further observing time on ALMA and other UK facilities. As the work progresses and detailed physical questions emerge, data analysis and interpretation will eventually be supplemented by radiation transfer modelling.