Understanding modern radioastronomical observations via advanced numerical simulations

天文观测见证了一波开花的新射电望远镜与前所未有的分辨率，灵敏度，节奏像OCSCARS和阿尔马。新的仪器提供了更高质量的数据，原则上可以比以前更好地约束宇宙中等离子体过程的模型。为了利用这些信息，还需要新的、更定量的天体物理等离子体、波发射和传播过程模型。新一代的模型应该描述从能源到预测在地球上可探测到的信号的过程链。可探测的无线电波是由微物理机制引起的。宏观能源必须首先考虑在大尺度上，然后向动力学尺度的能量转移必须描述以及辐射过程-无论是直接或需要等离子体不稳定性。必须推导出整个发射量的发射量，并考虑到它们向无线电天线的传播以及仪器效应。我们计划考虑从磁重联开始的这一过程链的所有部分，释放大尺度的磁能，形成可观察到的相干无线电波。我们专注于相干发射首先由于太阳爆发-其中最详细的是信息是可用于约束理论模型和相干无线电波发射的恒星（阿尔马观测）。对可观察到的无线电信号的形成的所有方面的充分处理需要能力和经验，这超出了一个单一研究小组的能力。因此，我们计划与我们的团队密切合作，利用他们互补的背景和专业知识进行调查：在德国方面的研究小组SMART继续前TSSSP小组的工作，现在在柏林工业大学，其长期的经验，动力，混合动力，弗拉索夫，PIC代码HPC-等离子体-以及与柏林理工学院（TU）天文学和天体物理学中心的天体物理学家和无线电-位于Ondrejov的捷克科学院天文研究所的天文学小组，该小组已经获得了组装总无线电发射率所需的多尺度MHD建模方面的专业知识，以及其在无线电/毫米波数据分析方面的重要专业知识，包括自己的仪器和阿尔马的开发和数据使用，将两个小组的专门知识结合起来，将使我们能够进一步开发和利用所有必要的工具，利用先进的数值模拟方法更好地了解所观测到的太阳爆发和日冕的相干无线电发射，以了解现代射电天文学数据。

Astronomical observations witness a wave of blossom by new radio-telescopes with unprecedented resolution, sensitivity, cadence like OCSCARS and ALMA. The new instruments provide data at a qualitatively higher level which allow, in principle, to constrain models of plasma-processes in the Universe much better than before. To utilize this information also new, more quantitative models of astrophysical plasma-, wave-emission and - propagation processes are needed. The new generation of models should describe the chain of processes starting from the energy sources towards predicting the signals, detectable at Earth. Detectable radio waves are caused by micro-physical mechanisms. The macroscopic energy sources have to be considered first at large scales, then the transfer of energy towards kinetic scales has to be decribed as well as radiation processes – either direct or those requiring plasma instabilities. The emissions have to be derived for the entire emitting volumes and their propagation to the radio antenna has to be taken into account as well as instrument effects.We plan to consider all parts of this chain of processes starting from magnetic reconnection, releasing magnetic energy at large scales, to the formation of observable coherent radio waves. We focus on coherent emissions first due to solar eruptions - for which the most detailed is information is available to constrain theoretical models and on coherent radio waves emitted by pulsars (ALMA observations). The full treatment of all aspects of the formation of the observable radio-signals requires capacities and experience which lead beyond the abilities of one single group of researchers. We therefore plan carry out our investigations in close collaboration between our groups with their complementary background and expertise: on the German side the research group SMART that continues the work of the former TSSSP group of the MPS Göttingen now at the TU Berlin with its long-term experience in kinetic, hybrid-, Vlasov-, PIC-code HPC-plasma- as well as MHD simulations in close collaboration with the astrophysicists of the Center for Astronomy and Astrophysics of the Berlin Institute of Technology (TU) and the radio-astronomy group of the Astronomical Institute of Czech Academy of Sciences at Ondrejov that has acquired expertise in multi-scale MHD modeling necessary for assembling the total radio emissivity and its significant expertise in radio/mm wave data analyses including the development and data use of own instruments as well as of ALMA, hosting one of the nodes of the European Regional ALMA Center.Combining the expertise of the two groups will allow us to further develop and utilize all necessary tools to better understand observed coherent radio emissions of solar eruptions and of pulsars utilizing advanced numerical simulation methods for understanding modernradio-astronomical data.