$R$-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar

Abstract

The nature of GW190814's secondary component $m_2$ of mass $(2.50-2.67){\text{M}}_{\odot }$ in the mass gap between the currently known maximum mass of neutron stars and the minimum mass of black holes is currently under hot debate. Among the many possibilities proposed in the literature, the $m_2$ was suggested as a superfast pulsar while its r-mode stability against the run-away gravitational radiation through the Chandrasekhar-Friedman-Schutz mechanism is still unknown. Using those fulfilling all currently known astrophysical and nuclear physics constraints among a sample of 33 unified equation of states (EOSs) constructed previously by Fortin {\it et al.} (2016) using the same nuclear interactions from the crust to the core consistently, we compare the minimum frequency required for the $m_2$ to rotationally sustain a mass higher than $2.50{\text{M}}_{\odot }$ with the critical frequency above which the r-mode instability occurs. We use two extreme damping models assuming the crust is either perfectly rigid or elastic. Using the stability of 19 observed low-mass x-ray binaries as an indication that the rigid crust damping of the r-mode dominates within the models studied, we find that the $m_2$ is r-mode stable while rotating with a frequency higher than 870.2 Hz (0.744 times its Kepler frequency of 1169.6 Hz) as long as its temperate is lower than about $3.9\times 10^{7}K$, further supporting the proposal that GW190814's secondary component is a supermassive and superfast pulsar.

arXiv comment9 pages, 5 figures, 1 table, version accepted for publication in ApJ

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