Astrophysical Aspects of Neutrino Dynamics in Ultradegenerate Quark Gluon Plasma

Souvik Priyam Adhya

doi:10.1155/2017/1273931

Abstract

The cardinal focus of the present review is to explore the role of neutrinos originating from the ultradense core of neutron stars composed of quark gluon plasma in the astrophysical scenario. The collective excitations of the quarks involving the neutrinos through the different kinematical processes have been studied. The cooling of the neutron stars as well as pulsar kicks due to asymmetric neutrino emission has been discussed in detail. Results involving calculation of relevant physical quantities like neutrino mean free path and emissivity have been presented in the framework of non-Fermi liquid behavior as applicable to ultradegenerate plasma.

Highlights

Compact stars, in minutes or hours after their birth, rapidly cool down to temperatures (T) of the order of 109 K from upper bounds of T ≿ 1011 K
It has been shown that the non-Fermi liquid (NFL) corrections to the quark selfenergy enhance the neutrino emissivity of ungapped quark matter which may exist at the core of neutron stars [19]
We have found the mean free path (MFP) for both the degenerate and the nondegenerate neutrinos involving terms which have fractional powers in (T/μ) at higher orders using the perturbation theory and the NFL phenomenon as discussed above

Summary

Introduction

In minutes or hours after their birth, rapidly cool down to temperatures (T) of the order of 109 K from upper bounds of T ≿ 1011 K. In dense quark matter, the neutrino mean free path (MFP) receives significant NFL corrections as has been demonstrated in [20] In many calculations, such corrections appear in the modification of the phase space giving rise to appreciable contributions to the well known FL terms. We will present the specific heat of degenerate quark matter which receives significant correction due to the presence of the high external magnetic field while including the NFL corrections. This quantity directly influences the kick velocity of pulsars (i.e., rapidly rotating neutron stars) which arises due to asymmetric neutrino emission.

Neutrino Mean Free Path

Neutrino Emissivity

Cooling Behavior of Neutron Star with Dense Quark Core

Pulsar Kick Velocity through Asymmetric Neutrino Emission

Conclusions