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On 2019 April 25, the LIGO/Virgo Scientific Collaboration detected a compactbinary coalescence, GW190425. Under the assumption of the binary neutron star(BNS), the total mass of $3.4^{+0.3}_{-0.1}\, M_\odot$ lies five standarddeviations away from the known Galactic population mean. In the standard commonenvelope scenario, the immediate progenitor of GW190425 is a close binarysystem composed of an NS and a He-rich star. With the detailed binaryevolutionary modeling, we find that in order to reproduce GW190425-like events,super-Eddington accretion (e.g., $1,000\,\dot{M}_{\rm Edd}$) from a He-richstar onto the first-born NS with a typical mass of 1.33 $M_\odot$ via stableCase BB mass transfer (MT) is necessarily required. Furthermore, the immediateprogenitors should potentially have an initial mass of $M_{\rm ZamsHe}$ in arange of $3.0-3.5$ $M_\odot$ and an initial orbital period of $P_{\rm init}$from 0.08 days to 0.12 days, respectively. The corresponding mass accreted ontoNSs via stable Case BB MT phase varies from $0.70\, M_\odot$ to $0.77\,M_\odot$. After the formation of the second-born NS, the BNSs are expected tobe merged due to gravitational wave emission from $\sim$ 11 Myr to $\sim$ 190Myr.

Super-Eddington Accretion as a Possible Scenario to Form GW190425