Spacetime structure of static solutions in GaussBonnet gravity: Charged case
Abstract
We have studied spacetime structures of static solutions in the ndimensional EinsteinGaussBonnetMaxwell{lambda} system. Especially we focus on effects of the Maxwell charge. We assume that the GaussBonnet coefficient {alpha} is nonnegative and 4{alpha}tilde/l{sup 2}{<=}1 in order to define the relevant vacuum state. Solutions have the (n2)dimensional Euclidean submanifold whose curvature is k=1, 0, or 1. In GaussBonnet gravity, solutions are classified into plus and minus branches. In the plus branch all solutions have the same asymptotic structure as those in general relativity with a negative cosmological constant. The charge affects a central region of a spacetime. A branch singularity appears at the finite radius r=r{sub b}>0 for any mass parameter. There the Kretschmann invariant behaves as O((rr{sub b}){sup 3}), which is much milder than the divergent behavior of the central singularity in general relativity O(r{sup 4(n2)}). In the k=1 and 0 cases plusbranch solutions have no horizon. In the k=1 case, the radius of a horizon is restricted as r{sub h}<{radical}(2{alpha}tilde) (r{sub h}>{radical}(2{alpha}tilde) in the plus (minus) branch. Some charged black hole solutions have no inner horizon in GaussBonnet gravity. There are topological black hole solutions with zero and negative mass in the plus branch regardless of the sign ofmore »
 Authors:

 Graduate School of Science, Waseda University, Shinjukuku, Tokyo 1698555 (Japan)
 Advanced Research Institute for Science and Engineering, Waseda University, Shinjukuku, Tokyo 1698555 (Japan)
 Publication Date:
 OSTI Identifier:
 20713540
 Resource Type:
 Journal Article
 Journal Name:
 Physical Review. D, Particles Fields
 Additional Journal Information:
 Journal Volume: 72; Journal Issue: 6; Other Information: DOI: 10.1103/PhysRevD.72.064007; (c) 2005 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 05562821
 Country of Publication:
 United States
 Language:
 English
 Subject:
 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; BLACK HOLES; COSMOLOGICAL CONSTANT; COSMOLOGY; EUCLIDEAN SPACE; GENERAL RELATIVITY THEORY; GRAVITATION; MATHEMATICAL SOLUTIONS; NEGATIVE MASS; SINGULARITY; SPACETIME; TOPOLOGY; VACUUM STATES
Citation Formats
Torii, Takashi, Advanced Research Institute for Science and Engineering, Waseda University, Shinjukuku, Tokyo 1698555, and Maeda, Hideki. Spacetime structure of static solutions in GaussBonnet gravity: Charged case. United States: N. p., 2005.
Web. doi:10.1103/PhysRevD.72.064007.
Torii, Takashi, Advanced Research Institute for Science and Engineering, Waseda University, Shinjukuku, Tokyo 1698555, & Maeda, Hideki. Spacetime structure of static solutions in GaussBonnet gravity: Charged case. United States. doi:10.1103/PhysRevD.72.064007.
Torii, Takashi, Advanced Research Institute for Science and Engineering, Waseda University, Shinjukuku, Tokyo 1698555, and Maeda, Hideki. Thu .
"Spacetime structure of static solutions in GaussBonnet gravity: Charged case". United States. doi:10.1103/PhysRevD.72.064007.
@article{osti_20713540,
title = {Spacetime structure of static solutions in GaussBonnet gravity: Charged case},
author = {Torii, Takashi and Advanced Research Institute for Science and Engineering, Waseda University, Shinjukuku, Tokyo 1698555 and Maeda, Hideki},
abstractNote = {We have studied spacetime structures of static solutions in the ndimensional EinsteinGaussBonnetMaxwell{lambda} system. Especially we focus on effects of the Maxwell charge. We assume that the GaussBonnet coefficient {alpha} is nonnegative and 4{alpha}tilde/l{sup 2}{<=}1 in order to define the relevant vacuum state. Solutions have the (n2)dimensional Euclidean submanifold whose curvature is k=1, 0, or 1. In GaussBonnet gravity, solutions are classified into plus and minus branches. In the plus branch all solutions have the same asymptotic structure as those in general relativity with a negative cosmological constant. The charge affects a central region of a spacetime. A branch singularity appears at the finite radius r=r{sub b}>0 for any mass parameter. There the Kretschmann invariant behaves as O((rr{sub b}){sup 3}), which is much milder than the divergent behavior of the central singularity in general relativity O(r{sup 4(n2)}). In the k=1 and 0 cases plusbranch solutions have no horizon. In the k=1 case, the radius of a horizon is restricted as r{sub h}<{radical}(2{alpha}tilde) (r{sub h}>{radical}(2{alpha}tilde) in the plus (minus) branch. Some charged black hole solutions have no inner horizon in GaussBonnet gravity. There are topological black hole solutions with zero and negative mass in the plus branch regardless of the sign of the cosmological constant. Although there is a maximum mass for black hole solutions in the plus branch for k=1 in the neutral case, no such maximum exists in the charged case. The solutions in the plus branch with k=1 and n{>=}6 have an inner black hole and inner and outer black hole horizons. In the 4{alpha}tilde/l{sup 2}=1 case, only a positive mass solution is allowed, otherwise the metric function takes a complex value. Considering the evolution of black holes, we briefly discuss a classical discontinuous transition from one black hole spacetime to another.},
doi = {10.1103/PhysRevD.72.064007},
journal = {Physical Review. D, Particles Fields},
issn = {05562821},
number = 6,
volume = 72,
place = {United States},
year = {2005},
month = {9}
}