共查询到20条相似文献，搜索用时 93 毫秒
1.
用在brick模型基础上发展起来的membrane模型 ,计算了缘于任意自旋场的非静态黑洞———Vaidya黑洞的自由能和熵。结果表明 ,玻色子场 (自旋s =1,2 )和费米子场 (自旋s =1/2 )的熵都恰好与黑洞的视界面积成正比 ,这与静态和稳态的情况相同。而且 ,玻色子和费米子场的熵具有相同的形式 ,二者相差一个系数 相似文献
2.
运用在砖墙模型方法的基础上发展起来的薄膜模型计算了1 1维和2 1维动态时空中的黑洞的熵。结果表明在低维动态时空中，黑洞熵仍满足Bekenstein—Hawking熵与面积的关系。 相似文献
3.
采用在brick模型基础上发展起来的membrane模型，计算了缘于任意自旋场的非静态黑洞——Vaidya黑洞的自由能和熵。结果表明，玻色子场(自旋s=1，2)和费米子场(自旋s=1／2)的熵都恰好与黑洞的视界面积成正比，这与静态和稳态的情况相同。而且，玻色子和费米子场的熵具有相同的形式，二相差一个系数。 相似文献
4.
运用在砖墙模型方法的基础上发展起来的薄膜模型计算了 1 1维和 2 1维动态时空中的黑洞的熵。结果表明在低维动态时空中 ,黑洞熵仍满足Bekenstein -Hawking熵与面积的关系 相似文献
5.
运用在brick-wall方法的基础上发展起来的薄膜模型计算了六维动态黑洞的自由能和玻色子熵，然后应用Г矩阵方法计算了费米子熵．结果显示六维动态黑洞的玻色子熵和费米子熵有相同的形式，它们之间只相差一个系数．并且仍然满足Bekenstein-Hawking的熵与面积的关系． 相似文献
6.
De Sitter背景时空中NUT-Kerr-Newman黑洞的玻色子熵 总被引：1，自引：0，他引：1
众所周知，一般黑洞的欧拉示性数都为2(或者为0)，而NUT—Kerr—Newman黑洞是个例外，其欧拉示性数大于2.因此计算NUT—Kerr—Newman黑洞的玻色子熵有特殊的意义．运用在brick-wall方法的基础上发展起来的膜模型计算了NUT-Kerr—Newman黑洞在de Sitter时空背景下的玻色子熵．结果表明，在选取适当的截断因子的情况下，该黑洞的熵仍满足Bekenstein—Hawking面积定律． 相似文献
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8.
本文利用共动度规讨论了非理想流体开放体系在自引力作用下的坍缩过程之熵变,结果表明,形成视界之前,体系的总熵不增,这说明黑洞的高熵产生于突变之中。 相似文献
9.
利用′ｔＨｏｏｆｔ的边界条件和“准周期”边界条件分别求解了１＋１维黑洞背景时空中的ＫｌｅｉｎＧｏｒｄｏｎ方程和Ｄｉｒａｃ方程,并计算了相应的玻色子熵与费米子熵,发现它们具有同一发散形式,两者仅相差一个系数 相似文献
10.
汪定雄 《中国天文和天体物理学报》1996,(4)
本文详细讨论了在Blandford－Znajek过程中吸积盘中心黑洞的角动量和质量的总变化率与质量吸积率和能量提取率之比的关系，在此基础上讨论了BlandfordZnajek过程对黑洞吸积盘内边缘半径r_(ms)演化的影响，并证明在此过程中中心黑洞的熵总是增大的。 相似文献
11.
We analyze the spectroscopic and photometric observations of the active galactic nucleus (AGN) 1E 0754.6+3928 performed at Crimean Astrophysical Observatory in 1998–2004. Based on formal spectroscopic criteria for the optical wavelength range, we can classify this object as a narrow-line Seyfert 1 (NLS1) galaxy. Over the period of its observations, the AGN 1E 0754.6+3928 showed a very low rms flux variability amplitude in both continuum and Hβ (～3%). The Hβ time lag relative to the continuum has been found from the cross-correlation function centroid to be τ cent = 112 ?67 +215 days. This result and the Hβ line dispersion estimate have allowed us to determine the central black hole mass by the reverberation method: 1.05 × 108 M ⊙. The position of 1E 0754.6+3928 in the black hole mass-luminosity diagram agrees with the positions of other NLS1 galaxies and can be explained by an enhanced mass accretion rate in the central source. 相似文献
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A possible link between EPR‐type quantum phenomena and astrophysical objects like black holes, under a new general definition of entanglement, is established. A new approach, involving backward time evolution and topology changes, is presented bringing to a definition of the system black hole‐worm hole‐white hole as an entangled system. 相似文献
14.
In this paper we present various classes of solutions for perfect fluid disks rotating around Schwarzschild black holes. We study the profiles of pressure, density and specific angular momentum and the formation of cusp-like structures at the inner edge of the disks. Using the trial function method, we calculate the frequency of the global axi-symmetric oscillations. We compare the results with those of the corresponding Newtonian calculations to find the general relativistic effects. 相似文献
15.
We present the results of our analysis of the RXTE observations for two transient sources, IGR J17091-3624 and IGR J18539+0727, in April 2003. The derived energy spectra of the sources and the power-density spectra of their light curves make it possible to classify them as low/hard-state X-ray binaries. The parameters of the power spectrum for IGR J18539+0727 lead us to tentatively conclude that the compact object in this binary is a black hole. 相似文献
16.
We consider the possibility of low-mass primordial black holes being formed in terms of the inflationary theory of the early Universe. We found a condition on the reheating temperature under which the relic remnants of primordial black holes had been formed by now. These relic remnants may account for a part of the dark matter in our Universe. 相似文献
17.
We present a model describing the evolution of a Super Massive Black Holes (SMBHs) population within the framework of hierarchical
models of galaxy formation. The occurrence of SMBHs binaries at different redshifts and the influence of the interacting SMBHS
on the host galaxies are studied by means of Montecarlo realizations of halo merging histories, coupled with a semi-analytical
treatment of the interactions between the systems. We find that the main parameters governing the coalescence timescale, and
hence the fraction of binary systems, are the initial mass and the accretion history of the SMBHs.
This revised version was published online in September 2006 with corrections to the Cover Date. 相似文献
18.
We study the properties of the ’Newtonian forces’ acting on a test particle in the field of the Kerr black hole geometry.
We show that the centrifugal force and the Coriolis force reverse signs at several different locations. We point out the possible
relevance of such reversals particularly in the study of the stability properties of the compact rotating stars and the accretion
discs in hydrostatic equilibria
Received honourable mention in the 1989 Gravity Research Foundation essay competition. 相似文献
19.
观测表明, 黑洞双星的B型准周期振荡(Quasi-Periodic Oscillation, QPO)频率与幂律通量之间存在正相关性. 试图基于阿尔文波振荡模型定量解释该相关性. 标准薄吸积盘辐射通量极大值处的阿尔文波振荡产生QPO. 标准薄盘上的软光子与冕或喷流基部的热电子介质发生逆康普顿散射产生幂律通量. 通过吸积率的连续变化, 得到QPO频率与幂律通量关系的分析解和数值解. 模拟得到的相关性在合理的参数范围内与观测值相吻合. QPO频率与幂律通量的正相关性可以理解为, 较强的磁场导致较高的阿尔文波频率和较高的电子温度从而得到较高的幂律通量. 结果表明B型QPO可能与吸积盘或喷流中的环向磁场的活动有关. 相似文献
20.
Oldřich Semerák 《Astrophysics and Space Science》1997,250(2):235-243
In a classical-like language introduced in a previous paper, the fact that the ring singularity of the Kerr spacetime cannot be left/reached by timelike geodesic which is not bound to the equatorial plane is interpreted as a result of the interplay of the gravitational and – mainly – the centrifugal forces. 相似文献