权益分类	功能权益	普通用户	{{item.name}}会员
{{category.name}}	{{benefitItem.name}}

Interaction of supernova remnants with interstellar clouds

超新星遗迹与星际云的相互作用

基本信息

批准号：
165336121
负责人：
Dr. Udo Ziegler
金额：
--
依托单位：
Leibniz-Institut für Astrophysik Potsdam (AIP)
依托单位国家：
德国
项目类别：
Research Grants
财政年份：
2010
资助国家：
德国
起止时间：
2009-12-31 至 2013-12-31
项目状态：
已结题

来源：
https://gepris.dfg.de/gepris/projekt/165336121?language=en
关键词：
Interaction supernova remnants interstellar clouds

项目摘要

Cloud compression by external shocks is believed to be an important triggering mechanism for star formation in the interstellar medium. Yet, the physics of shockcloud interactions is still far from being completely understood. Past work on the problem often ignored crucial physical processes or relied on too restrictive assumptions concerning the geometric setup. For instance, there is no research to date which explores the complex interplay between radiative cooling, magnetic fields, and (anisotropic) thermal conduction in a three-dimensional model. In this project we intend to bridge this gap by performing such sophisticated simulations applying our NIRVANA code in massively-parallel mode. The use of adaptive mesh refinement techniques will be a key ingredient in order to adequately resolve both the shock front and details of the cloud structure emanating from the shock impact. We consider clouds struck by a spherical supernova remnant as an attempt to model more realistically the pre-stage of shock-induced star formation by a nearby exploding star than planar shock scenarios can do. We investigate the importance of the mentioned physical processes for different cloud distances from the blast wave origin corresponding to different evolutionary stages of the remnant at the time it collides with the cloud. With this study, we expect to gain improved insight under which conditions shock-triggered star formation may become possible.

外部冲击造成的云压缩被认为是星际介质中恒星形成的重要触发机制。然而，冲击云相互作用的物理原理还远没有被完全理解。过去对该问题的研究经常忽略关键的物理过程或依赖于有关几何设置的过于严格的假设。例如，迄今为止还没有研究探索三维模型中的辐射冷却、磁场和（各向异性）热传导之间的复杂相互作用。在这个项目中，我们打算通过在大规模并行模式下应用我们的 NIRVANA 代码执行如此复杂的模拟来弥补这一差距。自适应网格细化技术的使用将是充分解决冲击波前沿和冲击波产生的云结构细节的关键因素。我们将球形超新星遗迹撞击的云视为一种尝试，比平面激波场景更真实地模拟附近爆炸恒星激波诱发的恒星形成的前期阶段。我们研究了上述物理过程对于距爆炸波源的不同云距离的重要性，对应于残余物与云碰撞时的不同演化阶段。通过这项研究，我们希望能够更好地了解在哪些条件下激波触发的恒星形成可能成为可能。