Radiation Energy Flux and Radiation Power of Schwarzschild Black Hole

2010 ◽  
Vol 49 (8) ◽  
pp. 1739-1745 ◽  
Author(s):  
Qing-Miao Meng ◽  
Ji-Jian Jiang ◽  
Jing-Lun Liu ◽  
Zhong-Rang Li
Keyword(s):  
Black Hole ◽  
Energy Flux ◽  
Radiation Power ◽  
Radiation Energy ◽  
Schwarzschild Black Hole ◽  
Radiation Energy Flux

Lifespan of rotating black hole in the frame of generalized uncertainty principle

2016 ◽  
Vol 31 (03) ◽  
pp. 1650008
Author(s):  
Tangmei He ◽  
Jingyi Zhang ◽  
Jinbo Yang ◽  
Hongwei Tan
Keyword(s):  
Black Hole ◽  
Energy Flux ◽  
Uncertainty Principle ◽  
Generalized Uncertainty Principle ◽  
Radiation Energy ◽  
Minimum Mass ◽  
Dominant Term ◽  
Radiation Energy Flux ◽  
Rotating Black Hole ◽  
Flat Spacetime

In this paper, the lifespan under the generalized uncertainty principle (GUP) of rotating black hole is derived through the corrected radiation energy flux and the first law of the thermodynamics of black hole. The radiation energy flux indicates that there exist the highest temperature and the minimum mass both of which are relevant to the initial mass of the black hole in the final stage of the radiation. The lifespan of rotating black hole includes three terms: the dominant term is just the lifespan in the flat spacetime; the other two terms are individually induced by the rotation and the GUP.

Magnetic traversable wormhole as accelerator of charged particles

2020 ◽  
Vol 35 (02n03) ◽  
pp. 2040026
Author(s):  
A. A. Kirillov ◽  
E. P. Savelova
Keyword(s):  
Synchrotron Radiation ◽  
Kinetic Energy ◽  
Magnetic Fields ◽  
Stationary State ◽  
Energy Flux ◽  
Charged Particles ◽  
Radiation Energy ◽  
Traversable Wormhole ◽  
Radiation Energy Flux

We show that the scattering of radiation on a traversable wormhole forms a vortex in the radiation energy flux. Then, if the wormhole possesses also a magnetic fields, the vortex accelerates charged particles along the magnetic lines and such a system works as an accelerator. If the vortex is small, the system reaches the stationary state, when the income of the kinetic energy reradiates completely in the form of the synchrotron radiation. Such a mechanism allows us to relate a part of observed sources of the synchrotron radiation to magnetic wormholes.

Radiation energy flux of Dirac field of static spherically symmetric black holes

2010 ◽  
Vol 19 (9) ◽  
pp. 090402
Author(s):  
Meng Qing-Miao ◽  
Jiang Ji-Jian ◽  
Li Zhong-Rang ◽  
Wang Shuai
Keyword(s):  
Black Holes ◽  
Energy Flux ◽  
Radiation Energy ◽  
Dirac Field ◽  
Spherically Symmetric ◽  
Radiation Energy Flux

Investigation of the Effect of Microwave-Radiation Energy Flux on the Structure and Properties of Polymeric Insulating Materials

2016 ◽  
Vol 52 (3-4) ◽  
pp. 212-216 ◽  
Author(s):  
E. M. Abutalipova ◽  
D. E. Bugai ◽  
A. N. Avrenyuk ◽  
O. B. Strel’tsov ◽  
I. R. Sungatullin
Keyword(s):  
Microwave Radiation ◽  
Energy Flux ◽  
Radiation Energy ◽  
Structure And Properties ◽  
Insulating Materials ◽  
Radiation Energy Flux

scholarly journals Phenomenological description of the interior of the Schwarzschild black hole

2015 ◽  
Vol 30 (15) ◽  
pp. 1550091 ◽  
Author(s):  
Hikaru Kawai ◽  
Yuki Yokokura
Keyword(s):  
Black Hole ◽  
Hawking Radiation ◽  
Weyl Tensor ◽  
Radial Direction ◽  
Heat Bath ◽  
Radiation Energy ◽  
The Other ◽  
Schwarzschild Black Hole ◽  
Self Consistent ◽  
Consistent Solution

We discuss a sufficiently large four-dimensional Schwarzschild black hole which is in equilibrium with a heat bath. In other words, we consider a black hole which has grown up from a small one in the heat bath adiabatically. We express the metric of the interior of the black hole in terms of two functions: One is the intensity of the Hawking radiation, and the other is the ratio between the radiation energy and the pressure in the radial direction. Especially in the case of conformal matters we check that it is a self-consistent solution of the semiclassical Einstein equation, Gμν = 8πG〈Tμν〉. It is shown that the strength of the Hawking radiation is proportional to the c-coefficient, that is, the coefficient of the square of the Weyl tensor in the four-dimensional Weyl anomaly.

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