scholarly journals Evolution of massive scalar fields in the spacetime of a tense brane black hole

2008 ◽  
Vol 41 (7) ◽  
pp. 1611-1623 ◽  
Author(s):  
Marek Rogatko ◽  
Agnieszka Szypłowska
Keyword(s):  
Black Hole ◽  
Scalar Fields ◽  
Massive Scalar

scholarly journals HAWKING RADIATION FOR SCALAR AND DIRAC FIELDS IN FIVE-DIMENSIONAL DILATONIC BLACK HOLE VIA ANOMALIES

2012 ◽  
Vol 21 (03) ◽  
pp. 1250030 ◽  
Author(s):  
RAMÓN BECAR ◽  
P. A. GONZÁLEZ
Keyword(s):  
Black Hole ◽  
Gauge Invariance ◽  
Scalar Fields ◽  
Two Dimensional ◽  
Massive Scalar ◽  
Dimensional Theory ◽  
Dirac Fields ◽  
Black Hole Background ◽  
Planck Distribution ◽  
Dilatonic Black Hole

We study massive scalar fields and Dirac fields propagating in a five-dimensional dilatonic black hole background. We expose that for both fields the physics can be described by a two-dimensional theory, near the horizon. Then, in this limit, by applying the covariant anomalies method we find the Hawking flux by restoring the gauge invariance and the general coordinate covariance, which coincides with the flux obtained from integrating the Planck distribution for fermions.

Stationary configurations around charged rotating black holes

2016 ◽  
Vol 25 (09) ◽  
pp. 1641012
Author(s):  
Carolina L. Benone
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Bound States ◽  
Scalar Fields ◽  
Analytic Solutions ◽  
Massive Scalar ◽  
Massive Scalar Field ◽  
Rotating Black Holes ◽  
Specific Frequency

Scalar fields can form real bound states around black holes for a specific frequency. In this work, we review the case of a charged and massive scalar field around a charged rotating black hole, in order to find these bound states. We analyze the behavior of these solutions for different parameters and also comment on analytic solutions for certain regimes.

Dynamics of scalar shell for rotating and charged rotating BTZ black holes

2019 ◽  
Vol 35 (02) ◽  
pp. 1950350 ◽  
Author(s):  
M. Sharif ◽  
Faisal Javed
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Thin Shell ◽  
Equations Of Motion ◽  
Scalar Fields ◽  
Massless Scalar ◽  
Massive Scalar ◽  
Matter Distribution ◽  
Dynamical Equations

This paper studies the dynamics of thin-shell for (2 + 1)-dimensional rotating and charged rotating Bañados–Teitelboim–Zanelli black holes by using Israel thin-shell formalism. We consider the matter distribution located at thin-shell associated with a scalar field and analyze its effects on the dynamics of thin-shell through equations of motion and effective potential. The corresponding dynamical equations are numerically studied for both massless as well as massive scalar fields. For rotating case, the rate of expansion and collapse increases with massless scalar shell but decreases for massive case. For charged rotating, the rate of expansion and collapse decreases by increasing angular momentum for both massless as well as massive case. We conclude that the rate of expansion and collapse of the rotating case is greater than charged rotating black hole.

scholarly journals VACUUM POLARIZATION OF MASSIVE SCALAR FIELDS ON THE BLACK HOLE HORIZON

2000 ◽  
Vol 15 (11n12) ◽  
pp. 815-824 ◽  
Author(s):  
HIROKO KOYAMA ◽  
YASUSADA NAMBU ◽  
AKIRA TOMIMATSU
Keyword(s):  
Black Hole ◽  
Vacuum Polarization ◽  
Thermal State ◽  
Power Series Expansion ◽  
Analytic Form ◽  
Scalar Fields ◽  
Large Mass ◽  
Black Hole Horizon ◽  
Massive Scalar ◽  
Mode Function

Vacuum polarization of massive scalar fields in a thermal state at arbitrary temperature is studied near the horizon of a Reissner–Nordström black hole. We derived an analytic form of <ϕ2> approximately in the large mass limit near the black hole horizon. We uses the zeroth order WKB approximation and power series expansion near the horizon for the Euclideanized mode function. Our formula for the vacuum polarization shows regular behavior on the horizon if the temperature of the scalar field is equal to the Hawking temperature of the black hole. The finite part of the vacuum polarization agrees with the result of the DeWitt–Schwinger approximation up to O(m-4) which is the next-to-leading order of the expansion.

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