Super-Eddington Accretion as a Possible Scenario to Form GW190425

On 2019 April 25, the LIGO/Virgo Scientific Collaboration detected a compact binary coalescence, GW190425. Under the assumption of the binary neutron star (BNS), the total mass of $3.4_{-0.1}^{+0.3}{M}_{\odot }$ lies five standard deviations away from the known Galactic population mean. In the standard common envelope scenario, the immediate progenitor of GW190425 is a close binary system composed of an NS and a He-rich star. With the detailed binary evolutionary modeling, we find that in order to reproduce GW190425-like events, super-Eddington accretion (e.g., $1,000{\dot{M}}_{\mathrm{E}\mathrm{d}\mathrm{d}}$) from a He-rich star onto the first-born NS with a typical mass of 1.33 $M_{\odot }$ via stable Case BB mass transfer (MT) is necessarily required. Furthermore, the immediate progenitors should potentially have an initial mass of $M_{\mathrm{Z}\mathrm{a}\mathrm{m}\mathrm{s}\mathrm{H}\mathrm{e}}$ in a range of $3.0-3.5$ $M_{\odot }$ and an initial orbital period of $P_{\mathrm{i}\mathrm{n}\mathrm{i}\mathrm{t}}$ from 0.08 days to 0.12 days, respectively. The corresponding mass accreted onto NSs via stable Case BB MT phase varies from $0.70M_{\odot }$ to $0.77M_{\odot }$. After the formation of the second-born NS, the BNSs are expected to be merged due to gravitational wave emission from $\sim$ 11 Myr to $\sim$ 190 Myr.