Discrepancy in the Upper Bound Mass of Neutron Stars. (arXiv:1902.08618v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+S_S/0/1/0/all/0/1">Sandeep Kumar S</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Arun_K/0/1/0/all/0/1">Kenath Arun</a> (1, 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Sivaram_C/0/1/0/all/0/1">C Sivaram</a> (3) ((1) Department of Physics and Electronics, Christ (Deemed to be University), Bengaluru (2) Department of Physics, Christ Junior College, Bengaluru (3) Indian Institute of Astrophysics, Bengaluru)
Observations have indicated that we do not see neutron stars (NS) of mass
near the theoretical upper limit as predicted. Here we invoke the role of dark
matter (DM) particles in star formation, and their role in lowering the mass of
remnants eventually formed from these stars. Massive stars can capture DM
particles more effectively than the lower mass stars, thus further softening
the equation of state of neutron star. We also look at the capture of DM
particles by the NS, which could further soften the upper mass limit of NS. The
admixture of DM particles would be higher at earlier epochs (high z).
Observations have indicated that we do not see neutron stars (NS) of mass
near the theoretical upper limit as predicted. Here we invoke the role of dark
matter (DM) particles in star formation, and their role in lowering the mass of
remnants eventually formed from these stars. Massive stars can capture DM
particles more effectively than the lower mass stars, thus further softening
the equation of state of neutron star. We also look at the capture of DM
particles by the NS, which could further soften the upper mass limit of NS. The
admixture of DM particles would be higher at earlier epochs (high z).
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