Speaker
Description
Quantum chromodynamics (QCD) axions might solve the mystery of an exact candidate for dark
matter (DM). Axions are weakly interacting particles, motivated by the solutions to the strong CP
problem physics. The cooling process of neutron stars (NS) occurs through the emission of particles,
including neutrinos and axions.
By employing the SLY equation of state (EoS), we solve the modified Tolman-Oppenheimer-Volkoff
(TOV) set of equations. We take into account the Bremsstrahlung process that occurs in both the core
and crust of the NS. Additionally, we analyze the influence of strong magnetic fields on the luminosity
versus the ages of NSs for different masses of axions.
We utilize the maximum permissible limit for the central magnetic field and a radially distance-
dependent expression for the magnetic field while generating profiles using the TOV equations. The
luminosity of axions produced through the Bremsstrahlung process is significantly higher in the
presence of a magnetic field compared to without magnetic field, particularly during the early stages
of the NS, within the possible range of axion masses. When a magnetic field is included, we observe a
notable difference in the luminosity of axions for all characteristic ages of NSs. Our analysis indicates
that the luminosity of particles, such as axions and neutrinos, in the cooling of NSs is largely affected
by the presence of an intense magnetic field. With the inclusion of magnetic fields in the EoS and
various processes related to the cooling of NSs, we can achieve a better understanding of the
underlying physics of the universe. The current results address fundamental questions regarding the
formation of stars and galaxies by observing their gravitational effects and electromagnetic radiation.