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Does GW190425 require an alternative formation pathway than a fast-merging channel? by Safarzadeh, Mohammadtaher; Ramirez-Ruiz, Enrico; Berger, Edo is a scholarly article available to read on EtoBox.

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The LIGO/Virgo Scientific Collaboration (LVC) recently announced the detection of a compact object binary merger, GW190425, with a total mass of $3.4^{+0.3}_{-0.1}$ M$_{\odot}$, and individual component masses in the range of about 1.1 to 2.5 $M_{\odot}$. If the constituent compact objects are neutron stars, then the total mass is five standard deviations higher than the mean of $2.66\pm 0.12$ M$_{\odot}$ for Galactic binary neutron stars (BNSs). LVC suggests such massive BNS systems are born from a fast-merging channel, and therefore, their non-detection in the Galaxy to be due to a selection effect. However, we are unable to reconcile the inferred formation efficiency from the reported merger rate, $\mathcal{R}_{\rm GW190425}=460^{+1050}_{-390}$ yr$^{-1}$ Gpc$^{-3}$, with predictions from our own study for fast-merging BNS systems. Moreover, the comparable merger rates of GW190425, and GW170817 are possibly in tension with our results for two reasons: (i) more massive systems are expected to have a lower formation rate, and (ii) fast merging channels should constitute $\lesssim 10\%$ of the total BNS systems if case BB unstable mass transfer is permitted to take place as a format

Author

Safarzadeh, Mohammadtaher; Ramirez-Ruiz, Enrico; Berger, Edo

Published

2020

Language

EN