Author:
Shirke Swarnim,Ghosh Suprovo,Chatterjee Debarati,Sagunski Laura,Schaffner-Bielich Jürgen
Abstract
Abstract
In this work, we perform the first systematic investigation of effects of the presence of
dark matter on r-mode oscillations in neutron stars (NSs). Using a self-interacting dark matter (DM) model based on the neutron decay anomaly and a hadronic model obtained from the posterior
distribution of a recent Bayesian analysis, we impose constraints on the DM self-interaction
strength using recent multimessenger astrophysical observations. We also put new constraints on
the DM fraction for this model of DM. The constrained DM interaction strength is then used to
estimate DM self-interaction cross section and shear viscosity resulting from DM, which is found
to be several orders of magnitude smaller than shear viscosity due to hadronic matter. Assuming
chemical equilibrium among DM fermions and neutrons, we estimate the bulk viscosity resulting from
the dark decay of neutrons considering different scenarios for the temperature dependence of the
reaction rate and investigate the effect on the r-mode instability window. We conclude that DM
shear and bulk viscosity may significantly modify the r-mode instability window compared with
the minimal hadronic viscosities, depending on the temperature dependence of the process. We also
found that for the window to be compatible with the X-ray and pulsar observational data, the rate
for the dark decay process must be fast.
Subject
Astronomy and Astrophysics
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