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 3.4β0.1+0.3βMββ 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., 1,000MΛEddβ) from a He-rich
star onto the first-born NS with a typical mass of 1.33 Mββ via stable
Case BB mass transfer (MT) is necessarily required. Furthermore, the immediate
progenitors should potentially have an initial mass of MZamsHeβ in a
range of 3.0β3.5Mββ and an initial orbital period of Pinitβ
from 0.08 days to 0.12 days, respectively. The corresponding mass accreted onto
NSs via stable Case BB MT phase varies from 0.70Mββ to 0.77Mββ. After the formation of the second-born NS, the BNSs are expected to
be merged due to gravitational wave emission from βΌ 11 Myr to βΌ 190
Myr.Comment: 8 pages, 10 figures, updated to add one referenc