Understanding modern radioastronomical observations via advanced numerical simulations

像ocscar和ALMA这样的新型射电望远镜具有前所未有的分辨率、灵敏度和节奏，天文观测见证了一波开花结果。新仪器提供的数据质量更高，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量源到预测地球上可探测到的信号的一系列过程。可探测的无线电波是由微观物理机制引起的。宏观能量来源必须首先在大尺度上考虑，然后必须描述能量向动力学尺度的转移以及辐射过程——无论是直接的还是需要等离子体不稳定性的。必须推导出整个发射体积的发射量，并且必须考虑到它们向无线电天线的传播以及仪器的影响。我们计划考虑这一系列过程的所有部分，从磁重联开始，在大尺度上释放磁能，到形成可观测的相干无线电波。我们首先关注由于太阳爆发引起的相干辐射——其中最详细的信息是可以用来约束理论模型和脉冲星发射的相干无线电波（ALMA观测）。全面研究可观测到的无线电信号形成的所有方面所需要的能力和经验，超出了一组研究人员的能力。因此，我们计划在具有互补背景和专业知识的小组之间密切合作进行调查：在德国方面，SMART研究小组继续MPS前TSSSP小组的工作Göttingen现在在柏林工业大学，在动力，混合动力，Vlasov-，与柏林理工学院（TU）天文和天体物理中心的天体物理学家以及位于昂德雷约夫的捷克科学院天文研究所的射电天文小组密切合作，获得了组装总射电发射率所需的多尺度MHD建模的专业知识，以及其在无线电/毫米波数据分析方面的重要专业知识，包括开发和数据使用欧洲区域ALMA中心的一个节点也在这里。结合两个小组的专业知识将使我们能够进一步开发和利用所有必要的工具，以更好地理解观测到的太阳爆发和脉冲星的相干射电发射，利用先进的数值模拟方法来理解现代射电天文数据。

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.