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

x射线脉冲星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，例如高于1e7 K的温度，高于1e12 G的磁场，或者具有~0.5c初始速度的等离子体如何减速的物理学。尽管对这些天体的研究已经使人们对它们复杂的现象有了基本的了解，但诸如发射区域的大小和形状，或者下落的等离子体与中子星磁场之间相互作用的物理学等关键点仍然不清楚。该应用程序旨在全面地进一步研究和理解x射线脉冲星中的吸积现象，特别是回答最近对最亮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中无法解决。为了实现这一目标，我们将主要集中在一个明亮的吸积脉冲星样本上，这些样本已经或将被目前正在运行的x射线任务观测到，这在很大程度上是我们小组成功的观测建议的结果。该应用程序延续了我们在<s:1>宾根大学<s:1>天文学和天体物理学研究所（IAAT）、埃尔兰根天体粒子物理中心(ECAP)/埃尔兰根博士的三个研究小组之前的成功合作。来自FAU erlangen - n<s:1> rnberg的remis Sternwarte和莫斯科罗蒙诺索夫大学的Sternberg天文研究所。我们的目标是发展和改进目前的强磁化中子星x射线双星吸积过程的理论模型，并用新的观测方法测试这些模型。

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.