Spherically symmetric solutions in covariant HoravaLifshitz gravity
Abstract
We study the most general case of spherically symmetric vacuum solutions in the framework of the covariant HoravaLifshitz gravity, for an action that includes all possible higher order terms in curvature which are compatible with powercounting normalizability requirement. We find that solutions can be separated into two main classes: (i) solutions with nonzero radial shift function, and (ii) solutions with zero radial shift function. In the case (ii), spherically symmetric solutions are consistent with observations if we adopt the view of Horava and MelbyTomson [P. Horava and C. M. MelbyThompson, Phys. Rev. D 82, 064027 (2010).], according to which the auxiliary field A can be considered as a part of an effective general relativistic metric, which is valid only in the IR limit. On the other hand, in the case (i), consistency with observations implies that the field A should be independent of the spacetime geometry, as the Newtonian potential arises from the nonzero radial shift function. Also, our aim in this paper is to discuss and compare these two alternative but different assumptions for the auxiliary field A.
 Authors:

 King's College London, Department of Physics, London WC2R 2LS (United Kingdom)
 Department of Physics, National Technical University of Athens, Zografou Campus GR 157 73, Athens (Greece)
 Publication Date:
 OSTI Identifier:
 21541496
 Resource Type:
 Journal Article
 Journal Name:
 Physical Review. D, Particles Fields
 Additional Journal Information:
 Journal Volume: 83; Journal Issue: 8; Other Information: DOI: 10.1103/PhysRevD.83.084030; (c) 2011 American Institute of Physics; Journal ID: ISSN 05562821
 Country of Publication:
 United States
 Language:
 English
 Subject:
 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; COMPARATIVE EVALUATIONS; GRAVITATION; MATHEMATICAL SOLUTIONS; METRICS; RELATIVISTIC RANGE; SPACETIME; SPHERICAL CONFIGURATION; SYMMETRY; CONFIGURATION; ENERGY RANGE; EVALUATION
Citation Formats
Alexandre, Jean, and Pasipoularides, Pavlos. Spherically symmetric solutions in covariant HoravaLifshitz gravity. United States: N. p., 2011.
Web. doi:10.1103/PHYSREVD.83.084030.
Alexandre, Jean, & Pasipoularides, Pavlos. Spherically symmetric solutions in covariant HoravaLifshitz gravity. United States. https://doi.org/10.1103/PHYSREVD.83.084030
Alexandre, Jean, and Pasipoularides, Pavlos. Fri .
"Spherically symmetric solutions in covariant HoravaLifshitz gravity". United States. https://doi.org/10.1103/PHYSREVD.83.084030.
@article{osti_21541496,
title = {Spherically symmetric solutions in covariant HoravaLifshitz gravity},
author = {Alexandre, Jean and Pasipoularides, Pavlos},
abstractNote = {We study the most general case of spherically symmetric vacuum solutions in the framework of the covariant HoravaLifshitz gravity, for an action that includes all possible higher order terms in curvature which are compatible with powercounting normalizability requirement. We find that solutions can be separated into two main classes: (i) solutions with nonzero radial shift function, and (ii) solutions with zero radial shift function. In the case (ii), spherically symmetric solutions are consistent with observations if we adopt the view of Horava and MelbyTomson [P. Horava and C. M. MelbyThompson, Phys. Rev. D 82, 064027 (2010).], according to which the auxiliary field A can be considered as a part of an effective general relativistic metric, which is valid only in the IR limit. On the other hand, in the case (i), consistency with observations implies that the field A should be independent of the spacetime geometry, as the Newtonian potential arises from the nonzero radial shift function. Also, our aim in this paper is to discuss and compare these two alternative but different assumptions for the auxiliary field A.},
doi = {10.1103/PHYSREVD.83.084030},
url = {https://www.osti.gov/biblio/21541496},
journal = {Physical Review. D, Particles Fields},
issn = {05562821},
number = 8,
volume = 83,
place = {United States},
year = {2011},
month = {4}
}