Super-Eddington accretion as a possible scenario to form GW190425

Author:

Zhang W T1,Wang Z H T2ORCID,Zhu J-P34ORCID,Hu R-C5ORCID,Shu X W1,Tang Q W6ORCID,Yi S X7ORCID,Lyu F8ORCID,Liang E W2ORCID,Qin Y12ORCID

Affiliation:

1. Department of Physics, Anhui Normal University , Wuhu, Anhui 241002 , China

2. Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University , Nanning 530004 , China

3. School of Physics and Astronomy, Monash University , Clayton Victoria 3800 , Australia

4. OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery , Clayton Victoria 3800 , Australia

5. Department of Physics and Astronomy, University of Nevada , Las Vegas, NV 89154 , USA

6. Department of Physics, School of Physics and Materials Science, Nanchang University , Nanchang 330031 , China

7. School of Physics and Physical Engineering, Qufu Normal University , Qufu, Shandong 273165 , China

8. Astronomical Research Center, Shanghai Science & Technology Museum , Shanghai 201306 , China

Abstract

ABSTRACT 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 $3.4^{+0.3}_{-0.1}\, \mathrm{M}_\odot$ 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 modelling, we find that in order to reproduce GW190425-like events, super-Eddington accretion (e.g. $1,000\, \dot{M}_{\rm Edd}$) from a He-rich star onto the first-born NS with a typical mass of 1.33 M⊙ via stable Case BB mass transfer (MT) is necessarily required. Furthermore, the immediate progenitors should potentially have an initial mass of MZamsHe in a range of 3.0–3.5 M⊙ and an initial orbital period of Pinit from 0.08 d to 0.12 d, respectively. The corresponding mass accreted onto NSs via stable Case BB MT phase varies from $0.70\, \mathrm{M}_\odot$ to $0.77\, \mathrm{M}_\odot$. After the formation of the second-born NS, the BNSs are expected to be merged due to gravitational wave emission from ∼11 Myr to ∼190 Myr.

Funder

Anhui Normal University

National Natural Science Foundation of China

Natural Science Foundation of Anhui Province

Natural Science Foundation of Jiangxi Province

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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