通过协变反常研究GHS和非极值D1-D5黑洞的霍金辐射

GHS黑洞的霍金辐射、有效action和协变边界条件

Hawking radiation in GHS blackhole, Effective action and Covariant Boundary condition

我们利用反常（手征）有效作用量的表达式，在事件视界上仅利用协变边界条件，得到了最一般的球对称黑洞$(\sqrt{-g}\neq1)$中GHS（弦状）黑洞的霍金辐射.从有效作用量的观点出发，建立了反常和正常能量动量张量之间的联系。

通过协变反常和有效action研究具有整体扰动的Reissner-Nordström黑洞的霍金辐射

Hawking radiation in Reissner-Nordström blackhole with a global monopole via Covariant anomalies and Effective action

我们采用协变反常抵消方法和有效作用量方法，在事件视界上仅利用协变边界条件，得到了具有最一般的球对称带电黑洞$(\sqrt{-g}\neq1)$的整体辐射的Reissner-Nordström黑洞的霍金辐射.

反常、视界与霍金辐射

Anomalies, Horizons and Hawking radiation

利用事件视界附近的手征反常和事件视界处的协变边界条件，得到了具有整体对称性的Reissner-Nordström黑洞和最一般的球对称黑洞类$(\sqrt{-g}\neq1)$中的Garfinkle-Horowitz-Strominger黑洞的霍金辐射.该方法不同于异常抵消方法，因为除了协变边界条件外，视界附近的手征异常是导出霍金通量的唯一输入。

Calculation of Hawking Radiation in Local Field Theory

Hawking radiation of the blackhole is calculated based on the principle of local field theory. In our approach, the radiation is a unitary process, therefore no information loss will be recorded. In fact, observers in different regions of the space communicate using the Hawking radiation, when the systems in the different regions are entangled with each other. The entanglement entropy of the blackhole is also calculated in the local field theory. We found that the entanglement entropy of the systems separated by the blackhole horizon is closely connected to the Hawking radiation in our approac…

Information Missing Puzzle, Where Is Hawking's Error?

Matters falling into and consisting of a blackhole can oscillate periodically across instead of accumulate statically on the central point and form singularities there. In quantum language, this oscillation not only resolves central singularities of the blackhole but also blurs its horizon remarkably. This blurring makes the horizon not a zero-thickness geometric surface any more, but an extended physic region whose thickness is comparable with the horizon radius itself. It is our negligence of this fact that leads to the information missing puzzle, and other related question in blackhole phys…

脏黑洞：热力学和视界结构

Dirty blackholes: Thermodynamics and horizon structure

最近人们对（静态球对称）黑洞与各种经典物质场（如电磁场、介子场、轴子场、阿贝尔希格斯场、非阿贝尔规范场、{ \sl等}）的相互作用表现出相当大的兴趣。这些研究的一个共同特点是，这些系统的霍金温度相对于等视界面积的真空黑洞似乎被抑制了，这一点以前还没有提到过。即：$k T_H \leq \hbar/(4πr_H) \equiv \hbar/\sqrt{4πA_H}$。本文认为，这种抑制是通用的。具体地说，它将被证明，\[ k T_H = {\hbar\over4πr_H} \; e^{-ϕ(r_H)} \; \left( 1 - 8πG \; ρ_H \; r_H^2 \right). \]这里$ϕ(r_H)$是一个积分量，取决于物质的分布，这是保证是积极的，如果弱能量条件得到满足。将讨论这种行为的几个例子。将这种行为推广到非对称动态黑洞。