Observational constraints on spinning, relativistic Bose-Einstein condensate stars

Abstract

Bose-Einstein condensates (BECs) have been proposed as candidate states of matter for the interior of neutron stars. Specifically, Chavanis and Harko obtained the mass-radius relation for a BEC star and proposed that the recently discovered neutron stars with masses around 2$M_{\odot }$ are BEC stars. They employed a barotropic equation of state (EOS), with one free parameter, that was first found by Colpi, Wasserman, and Shapiro (CSW), to describe them and derive stable equilibrium configurations of spinning BEC stars in General Relativity. In this work we show that while it is true that BECs allow for compact object masses as heavy as the heaviest observed ones, such stars cannot simultaneously have radii that are small enough to be consistent with the latest observations, in spite of the flexibility available in the EOS in the form of the free parameter. In fact, our conclusion applies to any spinning relativistic boson star that obeys the CSW EOS.

10 pages, 5 figures, significantly added materials; to be published in PRD; AM and SB dedicate this paper to our co-author, late Shreya Shah

References in corpus (7)

• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• Astrophysical Measurement of the Equation of State of Neutron Star Matter
• The Mass and Radius of the Neutron Star in 4U 1820-30
• Accretion disk onto boson stars: a way to supplant black holes candidates
• The Spin Distribution of Millisecond X-ray Pulsars
• Double Neutron Stars: Evidence For Two Different Neutron-Star Formation Mechanisms

Cited by in corpus (3)

• Testing Bose-Einstein Condensate dark matter models with the SPARC galactic rotation curves data
• Compact stars admitting Finch-Skea symmetry in the presence of various matter fields
• Bose-Einstein Condensate dark matter models in the presence of baryonic matter and random confining potentials