Open AccessR-mode stabilization in neutron stars with hyperon cores
Author(s) -
D. D. Ofengeim,
M. E. Gusakov,
P. Haensel,
M. Fortin
Publication year - 2019
Publication title -
journal of physics. conference series
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.21
H-Index - 85
eISSN - 1742-6596
pISSN - 1742-6588
DOI - 10.1088/1742-6596/1400/2/022029
Subject(s) - hyperon , neutron star , physics , superfluidity , dissipative system , instability , gravitational wave , stars , baryon , neutron , nuclear physics , volume viscosity , astrophysics , viscosity , condensed matter physics , quantum mechanics
R-mode oscillations of neutron stars are known to be generally unstable with respect to the emission of gravitational waves. This instability can be suppressed by dissipative processes in the neutron star core. The standard minimal nucleonic model of the core cannot stabilize r-modes for many observed neutron stars, at the same time the probability to observe them unstable should be very low. One of the solutions to this problem is to account for possible presence of hyperons in the stellar core. Hyperons strongly enhance bulk viscosity in the core, which effectively suppresses the r-mode instability. We revisit the bulk viscosity calculations in the non-superfluid hyperon matter and briefly discuss the effect of baryon superfluidity. Our results suggest that the hyperon solution to the r-mode problem is more promising than it was thought before.