Thermal Evolution and Axion Emission Properties of Strongly Magnetized Neutron Stars

Emission properties of compact astrophysical objects such as Neutron stars(NSs) are associated with crucial astronomical observables. In the currentwork, we obtain the mass, pressure profiles of the non-rotating NSs using themodified Tolman Oppenheimer Volkoff (TOV) system of equations in the presenceof intense magnetic field. We obtain the profiles by using a specificdistance-dependent magnetic field in the modified TOV equations. We employthree different equations of states (EoS) to solve the TOV equations byassuming the core of NSs comprises a hadronic matter. Employing the aboveprofiles, we determine the cooling rates of spherically symmetric NSs as afunction of time with and without including the magnetic field using the NSCoolcode. We have also determined the cooling rates as a function of radius forthree different NSs. Furthermore, we determine the luminosity of neutrinos,axions, and photons emitting from the NSs in the presence and absence of amagnetic field for an axion mass 16 meV and three different EoS. Ourcomparative study indicates that the cooling rate and luminosities ofneutrinos, axions, and photons change significantly due to the impact of thestrong magnetic field. We also find that due to the magnetic field, the axionmass bound increases slightly compared to without a magnetic field..