正则静态黑洞的薄吸积盘

依照Penrose的宇宙检察猜想,自然界不存在裸奇性.所以,值得进一步考虑的是自然界根本不存在奇性.讨论了没有奇点的正则黑洞,并研究史瓦西黑洞和正则黑洞在天体物理学中的区别.研究围绕正则黑洞的薄吸积盘,比较了不同正则黑洞之间薄吸积盘的能量通量,辐射温度和吸积效率.结果显示,正则黑洞薄吸积盘内的相互作用比史瓦西的更加强.此外,随着正则黑洞质量不断地减少,薄吸积盘会更有效地消耗能量.这些特征提供了一种区分出正则黑洞的可能性.     

Kerr-AdS黑洞的复杂度

规范/引力对偶为人们提供了一个研究物理的全新视角.由规范/引力对偶可知,边界上的共形场论等价于其内部的Anti-de Sitter时空.这个对偶为人们研究边界共形场论带来了极大的方便.最近,Susskind团队提出了一个复杂度/作用量对偶假设:认为黑洞边界上态的量子计算复杂度等价于其在Wheeler-DeWitt片中的作用量.复杂度代表了进行量子计算的困难程度,这意味着黑洞也许与量子计算有联系,这也加深了人们对黑洞的认识.基于这个假设,考虑类光关节项的贡献,改进了Susskind团队的原有方案,更精确地计算了Kerr-AdS黑洞的Wheeler-DeWitt片的作用量增长率,最终得到了边界态复杂度的增长率.     

Direct detection of a magnetic field in the innermost regions of an accretion disk

Models predict that magnetic fields play a crucial role in the physics of astrophysical accretion disks and their associated winds and jets. For example, the rotation of the disk twists around the rotation axis the initially vertical magnetic field, which responds by slowing down the plasma in the disk and by causing it to fall towards the central star. The magnetic energy flux produced in this process points away from the disk, pushing the surface plasma outwards, leading to a wind from the disk and sometimes a collimated jet. But these predictions have hitherto not been supported by observations. Here we report the direct detection of the magnetic field in the core of the protostellar accretion disk FU Orionis. The surface field reaches strengths of about 1 kG close to the centre of the disk, and it includes a significant azimuthal component, in good agreement with recent models. But we find that the field is very filamentary and slows down the disk plasma much more than models predict, which may explain why FU Ori fails to collimate its wind into a jet.     

含径向对流吸积盘的径向—环向不稳定性研究

从流体力学方程组出发,用微扰法得出含烃向对流吸积盘的径向。－环向不稳定性的色散方程,并根据盘的不同结构研究了四种模的不稳定性质,着重研究了径向粘滞力对含径向对流吸积的径向－环不稳定性的影响。结果表明：径向粘滞力对声模有较大的影响,但不改变粘滞模和热模的稳定性质,这一模型有利于解释银河系中黑洞候选体的ＱＰＯ现象。     

反常粘滞吸积薄盘的稳定结构

根据描述吸积盘的流体动力学方程,给出无磁场情况下的质量、动量和能量守恒方程。在所给定方程的基础上,利用新的反常粘滞计算了黑洞周围吸积盘内区的结构。数值结果表明盘内区的气体不是做开普勒旋转,温度随吸积率变化比较明显,在M=10M_⊙,M ^.=100M ^._E的情况下,吸积盘的最大温度可达到3.35×10⁷K。 同时文中也给出了面密度和径向速度的分布规律。     

The formation of a massive protostar through the disk accretion of gas

The formation of low-mass stars like our Sun can be explained by the gravitational collapse of a molecular cloud fragment into a protostellar core and the subsequent accretion of gas and dust from the surrounding interstellar medium. Theoretical considerations suggest that the radiation pressure from the protostar on the in-falling material may prevent the formation of stars above ten solar masses through this mechanism, although some calculations have claimed that stars up to 40 solar masses can in principle be formed via accretion through a disk. Given this uncertainty and the fact that most massive stars are born in dense clusters, it was suggested that high-mass stars are the result of the runaway merging of intermediate-mass stars. Here we report observations that clearly show a massive star being born from a large rotating accretion disk. The protostar has already assembled about 20 solar masses, and the accretion process is still going on. The gas reservoir of the circumstellar disk contains at least 100 solar masses of additional gas, providing sufficient fuel for substantial further growth of the forming star.     

耗散过程对吸积盘磁不稳定性的影响

在新的反常黏滞机制的基础上,利用微扰方法导出色散方程,分析了耗散过程对吸积盘磁不稳定性的影响。 结果表明:耗散率随半径的增大而减小;在磁场较小时,耗散过程的影响不可忽略。这不同于在微观黏滞和阻抗基础上得到的结论。     

非线性电动力学黑洞的复杂度

在Einstein引力与非线性电动力学耦合的理论中,会出现一类双视界的黑洞解,称为非线性电动力学黑洞.针对这种理论,从一般形式的作用量和球对称度规出发,计算了带电黑洞的电势以及Wheeler-DeWitt片的作用量,证明了该作用量等于内外视界上的电势差与电荷的乘积.采用Susskind等人最近提出的复杂度/作用量对偶猜想,该作用量可以解释为Anti-de Sitter边界上的量子态的计算复杂度.在Reissner-Nordstrom黑洞和Born-Infeld黑洞两种特殊情况下,利用本文得到的一般结果与文献中已有的结果完全符合.     

开放型大尺度磁场对黑洞吸积盘过渡区能量的提取

在黑洞磁层理论的基础上,利用改进的等效电路方法推导出黑洞吸积盘过渡区的喷流功率的表达式(简称TL功率),并进一步比较TL与BZ、DL功率的相对重要性,结果表明:对于低自转黑洞,TL功率比BZ、DL功率明显占优势.此外,利用该文提出的模型获得的TL功率能很好地拟合两个3CRFRI射电星系的强喷流功率.     

五维Myers-Perry黑洞的离壳ADT荷

基于离壳推广的Abbott-Deser-Tekin(ADT)定义,给出了五维时空中双转动的Myers-Perry黑洞的离壳ADT质量与角动量等守恒荷。在此基础上,验证了这些守恒荷严格满足黑洞热力学第一定律的微分与积分形式。此外,通过离壳推广的ADT方法与ADM定义以及Komar公式的比较,我们发现,对于五维Myers-Perry黑洞来说,此3种方法给出的守恒荷完全一致。     

Active galactic nuclei as scaled-up Galactic black holes

A long-standing question is whether active galactic nuclei (AGN) vary like Galactic black hole systems when appropriately scaled up by mass. If so, we can then determine how AGN should behave on cosmological timescales by studying the brighter and much faster varying Galactic systems. As X-ray emission is produced very close to the black holes, it provides one of the best diagnostics of their behaviour. A characteristic timescale--which potentially could tell us about the mass of the black hole--is found in the X-ray variations from both AGN and Galactic black holes, but whether it is physically meaningful to compare the two has been questioned. Here we report that, after correcting for variations in the accretion rate, the timescales can be physically linked, revealing that the accretion process is exactly the same for small and large black holes. Strong support for this linkage comes, perhaps surprisingly, from the permitted optical emission lines in AGN whose widths (in both broad-line AGN and narrow-emission-line Seyfert 1 galaxies) correlate strongly with the characteristic X-ray timescale, exactly as expected from the AGN black hole masses and accretion rates. So AGN really are just scaled-up Galactic black holes.