Constraints on tidal charge of the supermassive black hole at the Galactic Center with trajectories of bright stars

Abstract

As it was pointed out recently in Hees et al. (Phys Rev Lett 118:211101, 2017), observations of stars near the Galactic Center with current and future facilities provide an unique tool to test general relativity (GR) and alternative theories of gravity in a strong gravitational field regime. In particular, the authors showed that the Yukawa gravity could be constrained with Keck and TMT observations. Some time ago, Dadhich et al. (Phys Lett B 487:1, 2001) showed that the Reissner–Nordström metric with a tidal charge is naturally appeared in the framework of Randall–Sundrum model with an extra dimension ( is called tidal charge and it could be negative in such an approach). Astrophysical consequences of presence of black holes with a tidal charge are considerered, in particular, geodesics and shadows in Kerr–Newman braneworld metric are analyzed in Schee and Stuchlík (Intern J Mod Phys D 18:983, 2009), while profiles of emission lines generated by rings orbiting braneworld Kerr black hole are considered in Schee and Stuchlík (Gen Relat Grav 52:1795, 2009). Possible observational signatures of gravitational lensing in a presence of the Reissner–Nordström black hole with a tidal charge at the Galactic Center are discussed in papers (Bin-Nun in Phys Rev D 81:123011, 2010; Bin-Nun in Phys Rev D 82:064009, 2010; Bin-Nun in Class Quant Grav 28:114003, 2011). Here we are following such an approach and we obtain analytical expressions for orbital precession for Reissner–Nordström–de-Sitter solution in post-Newtonian approximation and discuss opportunities to constrain parameters of the metric from observations of bright stars with current and future astrometric observational facilities such as VLT, Keck, GRAVITY, E-ELT and TMT.

Phenomenological Extension for Tidal Charge Black Hole

“…In this paper we studied a generalization of the Reissner-Nordstrom metric performed by an introduction of a term proportional to r −3 . Such a generalization allows one to account for beyond GR effects that cannot be described by the pure Reissner-Nordstrom metric [12,19,21]. We treat this metric as a phenomenological ansatz which allows us to relate metric parameters with observational data.…”

“…So we propose a generalization of the Reissner-Nordstrom metric that accounts for more fine modified gravity effects which fall faster that r −2 . The corresponding effects will be detected in the nearest future via projects aimed on measuring black hole shadow properties [18,19]. So the main scope of this paper is to provide an additional way to connect observational data with new metric parameters.…”

Bound orbits near scalar field naked singularities

“…Thus, a bound orbit of the general type oscillates near a stable circular orbit (an oscillation is the motion from pericentre to apocentre and back) and ϕ osc is the angle between any two successive pericentre points of the orbit. The relativistic precession of pericentres of bound orbits is considered in [1,5,11,[40][41][42][43][44] both from a purely theoretical point of view and in the context of observations of S-stars in the Galactic Centre. If a massive test particle moves radially in some nonstatic degenerate orbit, which will be the case if J = 0 and A(r 0 ) < E 2 < 1, then ∆ ϕ = −2π.…”

Investigation of Particle Distributions in Xe-Xe Collision at sNN=5.44 TeV with the Tsallis Statistics

“…The Large Hadron Collider (LHC) has performed different species of collisions at one or more energies, such as lead-lead, proton-lead and proton-proton collisions. The Xe-Xe ion collision [1,2] Since the mass number value of the xenon is between the proton and the lead, it helps us to understand the system-scale effect of the final-state particle properties in ion collisions at high energy [3][4][5][6]. Many charged particles are produced and measured in the AA collisions.…”