Understanding modern radioastronomical observations via advanced numerical simulations

通过先进的数值模拟了解现代射电天文观测

• 批准号: 431893099
• 负责人: Professor Dr. Jörg Büchner
• 金额: --
• 依托单位: Max-Planck-Institut für Sonnensystemforschung (MPS)
• 依托单位国家: 德国
• 项目类别: Research Grants
• 资助国家: 德国
• 项目状态: 未结题
• 来源: https://gepris.dfg.de/gepris/projekt/431893099?language=en
• 关键词: Understanding; modern; radioastronomical; observations; via

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.

天文观测见证了 OCSCARS 和 ALMA 等具有前所未有的分辨率、灵敏度和节奏的新型射电望远镜的蓬勃发展，这些新仪器提供了更高质量水平的数据，原则上可以约束宇宙中的等离子体过程模型。为了比以前更好地利用这些信息，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，新一代模型应该描述从能源到预测的过程链。在地球上可检测到的信号是由微观物理机制引起的，必须首先在大尺度上考虑宏观能源，然后必须描述能量向动能尺度的转移以及辐射过程。直接或需要等离子体不稳定性的发射必须针对整个发射体积得出，并且必须考虑它们到无线电天线的传播以及仪器效应。我们计划从以下位置开始考虑该过程链的所有部分。磁的重新连接，大规模释放磁能，形成可观测的相干无线电波，我们首先关注太阳喷发引起的相干发射——对此，最详细的信息可用于约束理论模型和脉冲星发射的相干无线电波。 （ALMA 观测）。对可观测无线电信号形成的各个方面的全面处理需要超出一组研究人员的能力和经验，因此我们计划与我们的小组密切合作进行研究。他们的背景互补和专业知识：在德国方面，SMART 研究小组继续了 MPS Göttingen 的前 TSSSP 小组的工作，现在位于柏林工业大学，在动力学、混合、Vlasov、PIC 代码 HPC 等离子体方面拥有长期经验- 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以及捷克科学院天文研究所射电天文学小组密切合作的 MHD 模拟Ondrejov 科学学院拥有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，包括自己的仪器以及 ALMA 的开发和数据使用，托管了其中之一欧洲区域 ALMA 中心的节点。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喷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。