The physics of accretion in X-ray binary pulsars - relativistic effects, pulse profiles, and emission properties

X 射线双星脉冲星吸积物理 - 相对论效应、脉冲轮廓和发射特性

• 批准号: 259364563
• 负责人: Professor Dr. Jörn Wilms
• 金额: --
• 依托单位: Dr. Remeis-Sternwarte Bamberg - Astronomisches Institut -
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2014
• 资助国家: 德国
• 起止时间: 2013-12-31 至 2022-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/259364563?language=en
• 关键词: physics; accretion; ray; binary; pulsars

X-ray pulsars provide an unique opportunity to study the physical mechanisms operating under extreme conditions that are reached in the vicinity of accreting neutron stars, such as temperatures above 1e7 K, magnetic fields above 1e12 G, or the physics of how a plasma that has an initial velocity of ~0.5c is decelerated. Although studies of these objects have already led to a basic understanding of their complex phenomenology, key points such as the size and shape of the emitting region or the physics of interaction between the infalling plasma and the neutron star's magnetic field are still unclear.This application aims at a comprehensive effort to further study and understand the accretion phenomena in X-ray pulsars, especially to answer the questions opened by recent observations of the brightest sources, which cannot be resolved in the frame of the current physical picture of these systems. To achieve this goal, we will mostly concentrate on a sample of bright accreting pulsars which have been or will be observed with the currently operating X-ray missions, to large extent as a result of successful observational proposals by our groups. The application continues the previous successful collaboration of our three research groups at the Institut für Astronomie and Astrophysik (IAAT) of the University of Tübingen, the Erlangen Centre for Astroparticle Physics (ECAP)/Dr. Remeis Sternwarte, Bamberg, of FAU Erlangen-Nürnberg, and the Sternberg Astronomical Institute of the Lomonosov University of Moscow. Our objectives are to develop and improve current theoretical models for the accretion process in strongly magnetized neutron star X-ray binaries and to test these models with new observational methods.

X射线天文望远镜提供了一个独特的机会来研究在吸积中子星附近达到的极端条件下运行的物理机制，例如温度高于1 e7 K，磁场高于1 e12 G，或者具有约0.5c初始速度的等离子体如何减速的物理学。虽然对这些天体的研究已经使人们对它们复杂的现象学有了基本的了解，但诸如发射区的大小和形状或下落等离子体与中子星星磁场之间相互作用的物理学等关键点仍然不清楚。这项申请旨在全面努力进一步研究和了解X射线天体中的吸积现象，特别是回答最近对最亮光源的观测所提出的问题，这些问题在这些系统的当前物理图像框架内无法解决。为了实现这一目标，我们将主要集中在明亮的吸积星的样本，已经或将与目前运行的X射线任务，在很大程度上由于我们的小组成功的观测建议观察。该应用程序延续了我们在蒂宾根大学天文学和天体物理学研究所（IAAT）、埃尔朗根-纽伦堡天文学研究所的埃尔兰根天体粒子物理中心（ECAP）/Remeis Sternwarte博士、班贝格和莫斯科罗蒙诺索夫大学斯滕贝格天文研究所的三个研究小组以前成功合作的成果。我们的目标是发展和改进强磁化中子星星X射线双星吸积过程的现有理论模型，并用新的观测方法检验这些模型。