Analytical expression for a class of spherically symmetric solutions in Lorentz-breaking massive gravity. (27th April 2016)

• Record Type: Journal Article
• Authors: Li, Ping; Li, Xin-zhou; Xi, Ping
• Is Part Of: Classical and quantum gravity. Volume 33:Number 11(2016:Jun.)
• Publication Date: 2016-04-27
• Subjects: massive gravity -- spherically symmetric solution -- commutative ring -- stability; 0450 Kd -- 0420 -q; Quantum gravity -- Periodicals; Gravitation -- Periodicals; Relativity (Physics) -- Periodicals; Space and time -- Periodicals; Periodicals; 521.1
• DOI: 10.1088/0264-9381/33/11/115004
• Languages: English
• ISSNs: 0264-9381

Abstract

Abstract: We present a detailed study of the spherically symmetric solutions in Lorentz-breaking massive gravity. There is an undetermined function  ( X, w 1, w 2, w 3 ) in the action of Stückelberg fields S ϕ = Λ 4 ∫ d 4 x − g , which should be resolved through physical means. In general relativity, the spherically symmetric solution to the Einstein equation is a benchmark and its massive deformation also plays a crucial role in Lorentz-breaking massive gravity.  will satisfy the constraint equation T 0 1 = 0 from the spherically symmetric Einstein tensor G 0 1 = 0, if we maintain that any reasonable physical theory should possess the spherically symmetric solutions. The Stückelberg field ϕ i is taken as a 'hedgehog' configuration ϕ i = ϕ ( r ) x i / r, whose stability is guaranteed by the topological one. Under this ansätz, T 0 1 = 0 is reduced to d  = 0 . The functions  for d  = 0 form a commutative ring R  . We obtain an expression of the solution to the functional differential equation with spherical symmetry if  ∈ R  . If  ∈ R  and ∂  / ∂ X = 0, the functions  form a subring S  ⊂ R  . We show that the metric is Schwarzschild, Schwarzschild-AdS or Schwarzschild-dS if  ∈ S  . When  ∈ R  but  ∉ S , we will obtain some new metric solutions, including the furry black hole and beyond. Using the general formula and the basic property of function ring R , we give some analytical examples and their phenomenological applications. Furthermore, we discuss the stability of the gravitational field by the analysis of the Komar integral and the results of quasinormal modes (QNMs).