Gravitational phase transition mediated by thermalon in Einstein-Gauss-Bonnet-Maxwell-Kalb-Ramond gravity

Daris Samart,Phongpichit Channuie

doi:10.1007/jhep08(2020)100

Abstract

In this work, we study the possible existence of gravitational phase transition from AdS to dS asymptotic geometries in Einstein-Gauss-Bonnet gravity by adding the Maxwell one-form field (Aμ) and the Kalb-Ramond two-form field (Bμν) as impurity substitutions. The phase transitions proceed via the bubble nucleation of spherical thin-shells described by different branches of the solutions which host a dS black hole in the interior and asymptotic thermal AdS state in the exterior. We analyze the phase diagrams of the free energy and temperature to demonstrate the existence of the phase transitions in the grand canonical ensemble (fixed electrical potential). The phase transitions of having the one-form and two-form charges are possible in which the critical temperature is lower than that of the neutral case. Comparing results with existing literature, more importantly, our analyses show that the critical temperature and the Gauss-Bonnet coupling λ of the phase transitions get decreased by adding more types of the charges.

Highlights

JHEP08(2020)100 thermalon mediated phase transitions [19,20,21,22,23] in many cases of Lovelock gravity with a vacuum solution
In this work, we study the possible existence of gravitational phase transition from anti-de Sitter (AdS) to de Sitter (dS) asymptotic geometries in Einstein-Gauss-Bonnet gravity by adding the Maxwell one-form field (Aμ) and the Kalb-Ramond two-form field (Bμν) as impurity substitutions
This is a so-called the generalize HP phase transition which is different from original HP phase transition for the fact that the thermal AdS vacuum decays into a black hole belonging to a different branch solution

Summary

The Einstein-Gauss-Bonnet gravity with Maxwell and Kalb-Ramond fields

The standard definition of the Maxwell field in the five-dimensional spherical symmetric spacetime and its equation of motions in the vacuum are given by. The field strength tensor F in terms of differential form is given by,. We note that the KR strength field has the same properties and solution as the Maxwell gauge field under dual transformations and in fivedimensional spacetime. We note that there are two branches of the spherical symmetric solutions of the EGBM theory with KR fields. The effective cosmological constants of these branch solutions are obtained by setting, M = QA = QB = 0 in eq (2.18). We call f+(r) and f−(r) braches as the outer and inner manifold in the latter when we will consider and study the gravitational phase transition between two branches solution of the theory

Junction condition: thermalon dynamics and its stability

AdS to dS phase transition

Conclusion