对动态缓变Reissner-Nordstrm黑洞量子辐射特征的研究

考虑到Reissner Nordstr m黑洞的质量M和荷电量Q随时间t缓慢变化的情况 ,研究了此黑洞的量子辐射特征 .结果表明 ,在动态缓变Reissner Nordstr m时空中荷电Dirac粒子的量子热辐射谱与其黑洞蒸发率及随时间t缓变的M(t)和Q(t)等因素有关 ;动态缓变Reissner Nordstr m黑洞量子非热辐射的最大能量与量子热辐射谱中的化学势相等     

对动态缓变Reissner-Nordström黑洞量子辐射特征的研究

考虑到Reissner-Nordstrom黑洞的质量M和荷电量Q随时间t缓慢变化的情况,研究了此黑洞的量子辐射特征.结果表明,在动态缓变Reissner-Nordstrom时空中荷电Dirac粒子的量子热辐射谱与其黑洞蒸发率及随时间t缓变的M(t)和Q(t)等因素有关;动态缓变Reissner-Nordstrom黑洞量子非热辐射的最大能量与量子热辐射谱中的化学势相等.     

缓变动态Kerr-Newman黑洞的量子热力学性质

引入局域热平衡概念，用Damour-Ruffini方法和薄膜模型研究了缓变动态Kerr-Newman黑洞的Hawking辐射和熵.得到了黑洞的Hawking温度和辐射谱公式，Hawking温度随时间和视界面上的位置而变化，辐射谱为准黑体谱；计算了黑洞熵，当取与静态球对称黑洞情况相同的截断关系时便得到了黑洞的Bekenstein-Hawking熵.结果表明，缓变动态黑洞的温度是局域量，缓变动态黑洞的熵与稳态黑洞情况一样正比于黑洞视界面面积. 关键词： 缓变动态黑洞 Hawking辐射 黑洞熵     

对动态缓变Reissner-Nordstroem黑洞量子辐射特征的研究

考虑到Reissner-Nordstroem黑洞的质量M和荷电量Q随时间t缓慢变化的情况，研究了此黑洞的量子辐射特征．结果表明，在动态缓变Reissner-Nordstroem时空中荷电Dirac粒子的量子热辐射谱与其黑洞蒸发率及随时间t缓变的M(t)和Q(t)等因素有关；动态缓变Reissner-Nordstroem黑洞量子非热辐射的最大能量与量子热辐射谱中的化学势相等．     

Reissner-Nordstr(o)m de Sitter黑洞的量子隧穿效应

运用Parikh的量子隧穿模型,研究了Reissner-Nordstr(o)m de Sitter黑洞的量子隧穿效应.结果表明,在能量守恒的条件下,黑洞外视界和宇宙视界处的粒子出射率与Bekenstein-Hawking熵有关,辐射谱不再是严格的纯热谱.     

变加速直线运动黑洞的量子热效应

给出了作变加速直线运动的蒸发黑洞的辐射温度。此温度不仅随时间变化,而且在视界的同时面上不是常数。这种黑洞的视界位置随时间变化,而且形状不是球对称的。 关键词：     

对Reissner-Nordstr(o)m-anti-de Sitter黑洞Hawking隧穿辐射的研究

在考虑粒子间的自引力相互作用后;首先采用Parikh-Wilczek的半经典隧穿方法对带电粒子与不带电粒子在Reissner-Nordstrm-anti-de Sitter黑洞视界处的隧穿辐射特征进行了研究.其次;推广复路径方法对该黑洞的辐射谱进行研究.两种方法所得的结果都支持Parikh-Wilczek的观点;即黑洞的隧穿率Bekenstein-Hawking熵变有关;真实的辐射谱不是纯热谱.     

Reissner-Nordstr?m de Sitter黑洞的量子隧穿效应

运用Parikh的量子隧穿模型，研究了Reissner-Nordstrm de Sitter黑洞的量子隧穿效应.结果表明，在能量守恒的条件下，黑洞外视界和宇宙视界处的粒子出射率与Bekenstein-Hawking熵有关，辐射谱不再是严格的纯热谱.     

黑洞量子理论

简述引力场中物质的量子效应——黑洞的Ｈａｗｋｉｎｇ辐射，并进一步讨论黑洞的量子理论，给出一些结论。     

黑洞量子隧穿过程的时间

讨论了弯曲时空中黑洞量子隧穿的时间.在假定了黑洞量子隧穿是一个瞬时过程的情况下,通过利用WKB法得出了有静止质量粒子的量子隧穿辐射谱.该辐射谱表明对于在黑洞视界处有静止质量粒子的出射也满足量子力学中的幺正性原理,支持Parikh-Wilczek的结论.结果的合理性表明,在黑洞视界处的量子隧穿过程可以看成是一个瞬时过程.     

Internal instability in a Reissner-Nordström black hole

The question of the effect of asynumetries in gravitational collapse is investigated by considerations of test electromagnetic fields in an extended Reissner-Nordström background. It is found, with ths aid of computer calculations, that instabilities in the test field arise at the inner (Cauchy or anti-event) horizon, though not at the ouier (event) horizon. Thus it is reasonable to infer that in the full coupled Einstein-Maxwell theory the inner horizon will not survive as a non-singular bypersurface when asymmetric perturbations are present, but will instead become a space-time curvature singularity.     

Globally regular solutions of a schwarzschild black hole and a Reissner-Nordström black hole

A new physical concept about globally regular solutions is suggested. The globally regular solutions corresponding to the Schwarzschild black hole and the Reissner-Nordström black hole are examined.     

Stationary interacting fields around an extreme Reissner-Nordström black hole

The stationary multipole solutions of the Einstein-Maxwell equations, representing interacting gauge-invariant perturbations of an extreme Reissner-Nordström black hole, are given. They are considerably simpler than perturbations of a Schwarzschild black hole. Applications are outlined.     

On the theories of the interacting perturbations of the Reissner-Nordström black hole

A complete account of the Hamiltonian approach to the coupled perturbations of the Reissner-Nordström black hole, initiated by Moncrief, is given. All Hamiltonian equations are expressed explicitly in suitable forms; the metric and electromagnetic field perturbations are found in terms of Moncrief's gauge invariant canonical variables in the Regge-Wheeler gauge. The basic (both tetrad and coordinate) gauge invariant scalars occurring in the perturbation studies based on the Newman-Penrose formalism are then related to Moncrief's variables. The strikingly simple relations obtained enable us to show that the fundamental pair of decoupled equations, derived recently within the Newman-Penrose formalism by Chandrasekhar, can be cast into gauge invariant form, and that it can be obtained from Moncrief's formalism.It is demonstrated how the fundamental equations, supplemented by another combination of the Newman — Penrose equations, generalize the Bardeen-Press equations for uncoupled electromagnetic and gravitational perturbations of the Schwarzschild black hole.The odd and the even parityl=1 perturbations are also considered in detail. In the Appendix the relations to Zerilli's work on coupled perturbations of the Reissner-Nordström black hole are given.     

Pair production in Reissner-Nordstr(o)m-Anti de Sitter black holes

We studied the pair production of charged scalar particles of a five-dimensional near extremal Reissner-Nordstr(o)m-Anti de Sitter (RN-AdS5) black hole.The pair...