Thermal radiation from stellar collapse to a black hole

1989 ◽  
Vol 40 (6) ◽  
pp. 1858-1867 ◽  
Author(s):  
Stuart L. Shapiro
Keyword(s):  
Black Hole ◽  
Thermal Radiation ◽  
Stellar Collapse

Black‐Hole Evolution from Stellar Collapse

2019 ◽  
Vol 67 (5) ◽  
pp. 1800114
Author(s):  
Viacheslav A. Emelyanov
Keyword(s):  
Black Hole ◽  
Stellar Collapse

Radiation from Stellar Collapse to a Black Hole

1996 ◽  
Vol 472 (1) ◽  
pp. 308-326 ◽  
Author(s):  
Stuart L. Shapiro
Keyword(s):  
Black Hole ◽  
Stellar Collapse

Models for extragalactic radio sources

1986 ◽  
Vol 119 ◽  
pp. 415-416
Author(s):  
W. Kundt
Keyword(s):  
Black Hole ◽  
Thermal Radiation ◽  
Flow Velocity ◽  
Radio Sources ◽  
Lorentz Frame ◽  
Extragalactic Radio Sources ◽  
Ss 433 ◽  
Central Engine ◽  
Made In

Doubt is cast on the reality of the following four assumptions commonly made in the treatment of extragalactic radio sources: (1) The central engine is a black hole; (2) Electrons can be accelerated in situ in the knots and heads of the jets, to large Lorentz factors γ ≥ 102, with an efficiency exceeding 30%; (3) The (non-thermal) radiation emitted by the beam fluid is isotropic in some (comoving) Lorentz frame; and (4) The flow velocity in the jets of SS 433 is v = 0.26 c.

scholarly journals THERMAL RADIATION OF VARIOUS GRAVITATIONAL BACKGROUNDS

2007 ◽  
Vol 22 (08n09) ◽  
pp. 1705-1715 ◽  
Author(s):  
EMIL T. AKHMEDOV ◽  
VALERIA AKHMEDOVA ◽  
DOUGLAS SINGLETON ◽  
TERRY PILLING
Keyword(s):  
Black Hole ◽  
Thermal Radiation ◽  
Hawking Radiation ◽  
General Procedure ◽  
Storage Rings ◽  
Thermal Spectrum ◽  
Experimental Detection ◽  
Physical Picture

We present a simple and general procedure for calculating the thermal radiation coming from any stationary metric. The physical picture is that the radiation arises as the quasiclassical tunneling of particles through a gravitational barrier. We study three cases in detail: the linear accelerating observer (Unruh radiation), the nonrotating black hole (Hawking radiation), and the rotating/orbiting observer (circular Unruh radiation). For the linear accelerating observer we obtain a thermal spectrum with the usual Unruh temperature. For the nonrotating black hole we obtain a thermal spectrum, but with a temperature twice that given by the original Hawking calculations. We discuss possible reasons for the discrepancies in temperatures as given by the two different methods. For the rotating/orbiting case the quasiclassical tunneling approach indicates that there is no thermal radiation. This result for the rotating/orbiting case has experimental implications for the experimental detection of this effect via the polarization of particles in storage rings.

Non-thermal radiation from a non-Kerr-Newman black hole

2001 ◽  
Vol 10 (10) ◽  
pp. 979-982 ◽  
Author(s):  
Xie Shi-chong ◽  
Yang Xue-te ◽  
Yang Shu-zheng ◽  
Lin Li-bin
Keyword(s):  
Black Hole ◽  
Thermal Radiation ◽  
Newman Black Hole

QUANTUM ERGOSPHERE AND HAWKING PROCESS

1999 ◽  
Vol 14 (28) ◽  
pp. 1951-1960 ◽  
Author(s):  
ZHONG-HENG LI
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Thermal Radiation ◽  
Radiation Spectrum ◽  
Spherically Symmetric ◽  
Field Equations ◽  
Stationary Black Hole ◽  
Symmetric Black Hole ◽  
Hawking Process ◽  
Nonstationary Black Hole

We study both spherically symmetric and rotating (Kerr) nonstationary black holes and discuss the radiation of these black holes via the Hawking process. We find that the thermal radiation spectrum of a nonstationary black hole is obviously dependent on the spin state of a particle and is different from the case of a stationary black hole. This effect originates from the quantum ergosphere. We also find that the field equations of spin s=0,1/2,1 and 2 can combine into a generalized Teukolsky-type master equation with sources for any spherically symmetric black hole.

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