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射线脉冲星提供了一个独特的机会，可以研究在接受中子恒星附近达到的极端条件下运行的物理机制，例如高于1E7 K的温度，高于1E12 g的磁场或具有〜0.5C初始速度的血浆的物理学。尽管对这些物体的研究已经导致对它们的复杂现象学有基本的了解，但诸如发射区域的大小和形状或相互作用之间的关键点或中性恒星的磁场之间的相互作用之间的相互作用尚不清楚。该应用仍在全面地努力，以进一步研究并无法在X射线脉冲中拟合的问题，尤其是在X射线脉冲中的问题，尤其是在X射线脉冲中，尤其是在X射线脉动中，尤其是在X射线脉动中的促销，这些问题是开放的，尤其是在X射线脉冲中的宣传，这些问题是在X射线脉动的开放，这些问题是，这些问题是在X-Ray脉冲上的。这些系统当前物理图片的框架。为了实现这一目标，我们将主要集中在当前运行的X射线任务中观察到的明亮接受的脉冲星样本，这在很大程度上是由于我们小组成功的观察性建议。该应用程序继续在Tübingen大学，Erlangen Astroparpicle Physics（ECAP）/dr的Tübingen大学（ECAP）中心的三个研究小组（IAAT）的三个研究小组（IAAT）延续了以前的成功合作。 Fau Erlangen-Nürnberg的Remeis Sternwarte，Bamberg和莫斯科Lomonosov大学的Sternberg天文学院。我们的目标是开发和改善在强磁中性恒星X射线二进制中的积聚过程的当前理论模型，并使用新的观察方法测试这些模型。