| dc.description.abstract |
Emission properties of compact astrophysical objects such as Neutron Stars have been found to be associated with crucial astronomical observables. In the current work, we obtain the mass, pressure and baryon number density profiles of the non-rotating neutron stars using the modified Tolman Oppenheimer Volkoff (TOV) system of equations in the presence of an intense radially distributed magnetic field. Employing the above profiles, we have determined the cooling rates of spherically symmetric neutron stars as a function of time with and without including the magnetic field using the NSCool code. We used a specific distance-dependent magnetic field in the modified TOV equations to obtain the profiles. We employ three different equation of states to solve the TOV equations by assuming the core of Neutron Stars to be made up of a hadronic matter. Using the above profiles, the cooling rate of neutron stars is obtained by employing NSCool code. Furthermore, based on the cooling rate, we determine the luminosity of Neutrinos, Axions and Photons emitting from the neutron stars in the presence and absence of a magnetic field for different axion masses and three equations of states. Our comparative study indicates that the colling rate and luminosities of axions, photons and neutrinos changes significantly due to the impact of magnetic field |
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