Discrepancy in the Upper Bound Mass of Neutron Stars
Sandeep Kumar S (1), Kenath Arun (1, 2), C Sivaram (3) ((1) Department, of Physics, Electronics, Christ (Deemed to be University), Bengaluru (2), Department of Physics, Christ Junior College, Bengaluru (3) Indian Institute, of Astrophysics, Bengaluru)
TL;DR
This paper explores how dark matter particles influence the maximum mass of neutron stars, potentially explaining why observed neutron stars are often less massive than theoretical predictions.
Contribution
It introduces the role of dark matter in softening the neutron star equation of state, affecting the upper mass limit and offering a new perspective on neutron star mass discrepancies.
Findings
Dark matter capture by stars reduces neutron star mass limits.
Higher dark matter admixture at earlier cosmic epochs.
Dark matter softens the neutron star equation of state.
Abstract
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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Taxonomy
TopicsDark Matter and Cosmic Phenomena · Cosmology and Gravitation Theories · Pulsars and Gravitational Waves Research