On the Problem of the Super Reason in Astrophysics

The Giant Silence of the Universe or the absence of "Space Miracles" is in obvious contradiction with the rapid evolution of our civilization. The most striking fact is that both these phenomena, if taken separately, are in crying contradiction with "materialistic common sense", and are to be considered real "Space Miracles" themselves. In fact, this is the main problem of modern natural science. This crisis may be overcome if we recognize the Super Reason, that is, God discovered scientifically.     

Numerical Astrophysics

E119 3D Simulations of Weakly Magnetized Accretion Disks E147 The MRI in stratified accretion discs E212 Comparison between observed and simulated globular clusters E219 Presentation of simulation results of our 3D PIC Code E244 MAGMA: A 3D Lagrangian hydrodynamics code E254 FEARLESS – A new modelling approach for turbulent astrophysical flows E256 Cosmic ray transport in MHD turbulence: Numerical calculation of D_μμ (μ) and D_μμ (p) E261 FEARLESS modeling of turbulent flows applied to numerical simulations of galaxy clusters E264 FEARLESS – Subgrid Scale Turbulence modeling and Applications to Star Formation     

Stereo pairs in Astrophysics

Stereoscopic visualization is seldom used in Astrophysical publications and presentations compared to other scientific fields, e.g., Biochemistry, where it has been recognized as a valuable tool for decades. We put forth the view that stereo pairs can be a useful tool for the Astrophysics community in communicating a truer representation of astrophysical data. Here, we review the main theoretical aspects of stereoscopy, and present a tutorial to easily create stereo pairs using Python. We then describe how stereo pairs provide a way to incorporate 3D data in 2D publications of standard journals. We illustrate the use of stereo pairs with one conceptual and two Astrophysical science examples: an integral field spectroscopy study of a supernova remnant, and numerical simulations of a relativistic AGN jet. We also use these examples to make the case that stereo pairs are not merely an ostentatious way to present data, but an enhancement in the communication of scientific results in publications because they provide the reader with a realistic view of multi-dimensional data, be it of observational or theoretical nature. In recognition of the ongoing 3D expansion in the commercial sector, we advocate an increased use of stereo pairs in Astrophysics publications and presentations as a first step towards new interactive and multi-dimensional publication methods.     

The Schwarzschild distribution and stellar disks

Exact radially-dependent particular solutions to the hydrodynamic equations for a disk galaxy are found. The mass density is calculated for a known Schwarzschild distribution function and also a distribution function is calculated from a known mass density.     

天体物理学中动力学研究的计算机模拟

简要介绍了计算机模拟的基本原理和方法 ,以及数值模拟计算在天体物理学中的主要应用结果和前景     

Fundamental Problems in Astrophysics

Progress of modern astrophysics requires the access to the electromagnetic spectrum in the broadest energy range. The Ultraviolet is a fundamental energy domain since it is one of the most powerful tool to study plasmas at temperatures in the 3,000–300,000 K range as well as electronic transitions of the most abundant molecules in the Universe. Moreover, the UV radiation field is a powerful astrochemical and photoionizing agent.The objective of this review is to describe the crucial issues that require access to the UV range. A summary has been added to the end with a more classic view of UV needs by astronomical object type; this approach is followed at length in the rest of the contributions of this issue.     

伽马天文观测技术综述

伽马射线作为宇宙中极端事件的独特探针,探测伽马射线是人们了解宇宙构成、星体演化和宇宙线起源等的重要途经.伽马天文涉及了宇宙中的各种前沿科学问题并且观测所需能谱跨度极宽(102 keV–102 TeV),针对不同的科学目标和细分谱段,必须利用不同的伽马望远镜探测技术.总结了空间和地面的共5大类伽马射线观测技术,分别是编码孔径望远镜、康普顿望远镜、电子对望远镜、成像大气切伦科夫望远镜和广延大气簇射阵列;回顾了70 yr来在观测设备和技术进步的推动下伽马射线天文学领域的巨大进展,其中包含高能和甚高能谱段取得的大量成就,中低能段由于已有观测任务有限以及灵敏度低,超高能和极高能段由于观测难度大、起步时间晚,数据和成果相对其他谱段产出较少;展望了未来已经规划的伽马望远镜任务、能力及预期科学产出,其中,中低能段空间望远镜增强型ASTROGAM望远镜(e-ASTROGAM)、全天区中能伽马射线观测站(AMEGO)和甚高能段地面望远镜阵列高海拔宇宙线观测站(LHAASO)、切伦科夫望远镜阵列(CTA),由于灵敏度较同谱段已有任务灵敏度有大幅提升,极有可能在20 yr内从不同角度再度扩展人类对伽马宇宙的认知.     

分形和混沌理论在天体物理中的应用

本文对当前应用日益广泛的非线性科学的两个重要分支──分形和混沌动力系统理论──作概述性的介绍，并简介了这两种非线性方法在天体物理中应用的重要结果，特别强调一些天体物理中典型的分形和混沌现象，诸如星系大尺度结构（分形）和星系动力学（混沌）。     

实验室X射线天体物理

正在进行的实验室天体物理测量解决了X射线天文学的一些问题，这些实验产生了大量可靠的原子数据，它们既可用于电荷分布中电离与复合截面的计算，又可用于对X射线谱线形成的线表、激发截面及双电子复合系数的理解。另有一部分实验注重于解决天体观测的难题，以及验证现有的和寻找新的X射线谱线诊断。讨论了上述实验产生的数据类型，并展示了实验室测量如何为卫星（ASCA、EUVE、Chandra、XMM和ASTRO-E2）观测提供实验依据．     

主成分分法在天体物理中的应用

主成分分析法是从观测数据中获取主要信息的一种多种变量统计方法，它用数目少得多的新主代会原有观测量，以寻找原观测量之间的相互关系，且不损失原始数据的主要信息，尤其是对于大样本，多参量情况，该方法更为简捷而有效，目前，主成分分析法被广泛应用于三体物诸多研究领域中,介绍了主成分分法的原理和它在天体物理和它在天体物理中的广泛应用。     

The Kepler Mission: Astrophysics and Eclipsing Binaries

The Kepler Mission is a photometric space mission that will continuously observe a single 100 square degree field of view (FOV) of the sky of more than 100,000 stars in the Cygnus-Lyra region for four or more years with a precision of 14 parts per million (ppm) for a 6.5 hour integration including shot noise for a twelfth magnitude star. The primary goal of the mission is to detect Earth-size planets in the habitable zone of solar-like stars. In the process, many eclipsing binaries (EB) will also be detected. Prior to launch, the stellar characteristics will have been determined for all the stars in the FOV with K<14.5. As part of the verification process, stars with transits (about 5%) will need to have follow-up radial velocity observations performed to determine the component masses and thereby separate grazing eclipses caused by stellar companions from transits caused by planets. The result will be a rich database on EBs. The community will have access to the archive for uses such as for EB modeling of the high-precision light curves. A guest observer program is also planned for objects not already on the target list.     

The plane trajectories of spin particles in the Schwarzschild field

Plane motions of spin particles in the Schwarzschild field are investigated. Cases of parallel transport of spin tensor (PTS) and of geodesic motion (GM) as well as of the motion under additional Pirani (PC) and Dixon (DC) conditions are considered. Using these assumptions analogues of the Binnet formula are obtained. In the case of PTS and PS the stability of circular orbits the way Liapunov interprets it is examined.     

The spherically-symmetrical trajectories of spin particles in the Schwarzschild field

The motion of spin particles in the Schwarzschild field is examined in this paper. It is shown that Mathisson-Papapetrou equations under additional conditions , where is the Lie derivative of the Killing vector _j , permit only radial motion, motion in the equatorial plane and in the equilibrium points. All these types of motion are considered more in detail.