Exploring the non-linear dynamics of relativistic astrophysical shocks with kinetic simulations and advanced visualisation methods

通过动力学模拟和先进的可视化方法探索相对论天体物理冲击的非线性动力学

• 批准号: 14045192
• 负责人: Professor Dr. Padma Kant Shukla (†)
• 金额: --
• 依托单位: Institut für Theoretische Physik IV: Weltraum- und Astrophysik
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2005
• 资助国家: 德国
• 起止时间: 2004-12-31 至 2009-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/14045192?language=en
• 关键词: Exploring; non; linear; dynamics; relativistic

Plasmas that collide at relativistic speeds form shocks. Such plasma collisions occur at cosmological distances between the interstellar medium and, for example, the blast shell of Gamma Ray Bursts or the collimated jets of Active Galactic Nuclei. They may also form in our galactic neighborhood inside the accretion disks of black holes, (known as microquasars) and at supernovae. These shocks convert energy from the plasma bulk flow into cosmic ray radiation and a better understanding of the underlying processes is of uttermost importance for explaining the origin of the highly energetic cosmic ray radiation. We propose here to examine such energy conversion processes in plasma which are non-linear and require a relativistic treatment. We employ an electromagnetic and fully relativistic particle-in-cell code to examine them in one and two spatial dimensions at high resolutions. The resulting data sets will have a size of the order of a Terabyte and we must employ and further develop our custom-built advanced visualisation software to maximize the information we can extract from the simulation data. The proposed interdisciplinary project combines elements of astrophysics, plasma simulations and scientific visualisation. It will lead to a better understanding of the spatio-temporal evolution of relativistic shocks in a collisionless plasma in a fully kinetic framework, as well as of the peak energies up to which particles can be accelerated by these shocks.

等离子体以相对论速度碰撞形成激波。这样的等离子体碰撞发生在星际介质与伽玛射线暴的爆炸壳层或活动星系核的准直喷流之间的宇宙学距离处。它们也可能在我们银河系附近的黑洞吸积盘（称为微类星体）和超新星中形成。这些冲击将能量从等离子体体整体流转化为宇宙射线辐射，更好地理解基本过程对于解释高能宇宙射线辐射的起源至关重要。我们建议在这里检查等离子体中的能量转换过程是非线性的，需要相对论处理。我们采用电磁和完全相对论性粒子在细胞的代码来检查他们在一个和两个空间维度的高分辨率。由此产生的数据集将有一个太字节的大小，我们必须采用和进一步开发我们的定制先进的可视化软件，以最大限度地提高我们可以从模拟数据中提取的信息。拟议的跨学科项目结合了天体物理学，等离子体模拟和科学可视化的元素。它将导致更好地了解在完全动力学框架中的无碰撞等离子体中相对论性冲击的时空演变，以及这些冲击可以加速粒子的峰值能量。