Classical corrections to black hole entropy in d dimensions: A rear window to quantum gravity?

Abstract

We provide a simple derivation of the corrections for Schwarzschild and Schwarzschild-Tangherlini black hole entropy without knowing the details of quantum gravity. We will follow Bekenstein, Wheeler and Jaynes ideas, using summations techniques without calculus approximations, to directly find logarithmic corrections to well-known entropy formula for black holes. Our approach is free from pathological behaviour giving negative entropy for small values of black hole mass M . With the aid of "Universality" principle we will argue that this purely classical approach could open a window for exploring properties of quantum gravity.

The QCD Equation of State and Quark Star Properties

“…Similar values for the maximal mass and radius were found in a perturbative approach with a physically motivated choice of the renormalization scale [17]. In a Schwinger-Dyson approach [18], M ≈ 0.7M sun and R ≈ 9 km were obtained. It is interesting to compare these values with the mass and the radius of the object RX J1856: M ≈ 0.9M sun and R ≈ 6 km [19], which are not compatible with any hadronic equation of state.…”

Effect of the chiral chemical potential on the position of the critical endpoint

“…It overcomes the difficulty in the summation of the frequency spectrum at finite temperature confronted in many other more sophisticated gluon propagator models [29][30][31], but it can be used to highlight many underlying mechanisms. In the literature, it has been used to study the chiral phase transition without considering the chiral imbalance and gives reasonable results compared to that obtained with other nonperturbative methods [9,10,32,33], At finite temperature, chemical potential, and chiral chemi cal potential, this model gluon propagator can be written as (9) in which qn -{q,ojn), with mn = {2n+\)7iT+ip [28,34,35], As it is noted in Ref. [28], the UV cutoff of this model is much stronger than general asymptotic behavior, so it is not suitable to study the physics in which the asymptotic behavior becomes apparent but can be used in the study that centers on physics in the chiral symmetry broken phase and in the vicinity of the chiral phase transition.…”

Short introduction to the physics of neutron stars

“…The interested reader is referred to Ref. [14] for a recent review on this hot and exciting topic. Neutron stars can be observed either as isolated objects or forming binary systems together with other neutron stars, white dwarfs or ordinary (main-sequence and red giant) stars.…”