Speaker
Description
The configuration of the magnetic field is a crucial factor in determining its effects on the internal
composition and structure of neutron stars (NS). In this study, we enhance our understanding of the
emission rate of observable axions-hypothetical particles that may provide insight into viable dark
matter (DM) candidates resulting from the cooling of NS. We analyze the influence of the magnetic
field by solving the Tolman-Oppenheimer-Volkoff equations. Our approach incorporates a radially
distance-dependent magnetic field and the maximum possible strength of the central magnetic field.
We assume that the nucleon–nucleon bremsstrahlung process occurs within the core of a spherically
symmetric, strongly magnetized NS. The presence of a strong magnetic field significantly alters
both the energy spectrum of axions and the flux of photons originating from axion-photon
conversion. Notably, our results exhibit distinct features when the spectrum produced through the
Bremsstrahlung process is far more pronounced when magnetic field is present, exceeding the
corresponding emission in the non-magnetized configuration across the possible axion masses. We
conclude that incorporating magnetic fields into the various axion production processes is essential
for a comprehensive understanding of the physics underlying axionic DM, as modeled with the NS
Cooling code.