Does GW190425 Require an Alternative Formation Pathway than a Fast-merging Channel?

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Does GW190425 Require an Alternative Formation Pathway than a Fast-merging Channel? / Safarzadeh, Mohammadtaher; Ramirez-Ruiz, Enrico; Berger, Edo.

In: Astrophysical Journal, Vol. 900, No. 1, 13, 27.08.2020.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Safarzadeh, M, Ramirez-Ruiz, E & Berger, E 2020, 'Does GW190425 Require an Alternative Formation Pathway than a Fast-merging Channel?', Astrophysical Journal, vol. 900, no. 1, 13. https://doi.org/10.3847/1538-4357/aba596

APA

Safarzadeh, M., Ramirez-Ruiz, E., & Berger, E. (2020). Does GW190425 Require an Alternative Formation Pathway than a Fast-merging Channel? Astrophysical Journal, 900(1), [13]. https://doi.org/10.3847/1538-4357/aba596

Vancouver

Safarzadeh M, Ramirez-Ruiz E, Berger E. Does GW190425 Require an Alternative Formation Pathway than a Fast-merging Channel? Astrophysical Journal. 2020 Aug 27;900(1). 13. https://doi.org/10.3847/1538-4357/aba596

Author

Safarzadeh, Mohammadtaher ; Ramirez-Ruiz, Enrico ; Berger, Edo. / Does GW190425 Require an Alternative Formation Pathway than a Fast-merging Channel?. In: Astrophysical Journal. 2020 ; Vol. 900, No. 1.

Bibtex

@article{c298519bc95e4316bcb2d036804020fb,

title = "Does GW190425 Require an Alternative Formation Pathway than a Fast-merging Channel?",

abstract = "The LIGO/Virgo Scientific Collaboration (LVC) recently announced the detection of a compact object binary merger, GW190425, with a total mass of 3.4(-0.1)(+0..3) M-circle dot and individual component masses in the range of about 1.1-2.5 M-circle dot. If the constituent compact objects are neutron stars, then the total mass is five standard deviations higher than the mean of 2.66 +/- 0.12 M-circle dot for Galactic binary neutron stars. LVC suggests that the nondetection of such massive binary neutron star (BNS) systems in the Galaxy is due to a selection effect. However, we are unable to reconcile the inferred formation efficiency from the reported merger rate, R-GW190425 = 40(-390)(+1050) 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 lower formation rates, and (ii) fast-merging channels should constitute less than or similar to 10% of the total BNS systems if case BB unstable mass transfer is permitted to take place as a formation pathway. We argue that, to account for the high merger rate of GW190425 as a BNS system, (i) our understanding of NS formation in supernova explosions must be revisited, or (ii) more massive NSs must be preferentially born with either very weak or very high magnetic fields so that they would be undetectable in the radio surveys. Perhaps the detected massive NSs in NS-white dwarf binaries are our clues to the formation path of GW190425 systems.",

keywords = "Binary stars, LIGO, Neutron stars, Common envelope binary stars, NEUTRON-STAR, MAGNETIC-FIELD, GRAVITATIONAL-WAVE, COMMON ENVELOPE, EVOLUTION, BINARIES, RATES",

author = "Mohammadtaher Safarzadeh and Enrico Ramirez-Ruiz and Edo Berger",

year = "2020",

month = aug,

day = "27",

doi = "10.3847/1538-4357/aba596",

language = "English",

volume = "900",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "Institute of Physics Publishing, Inc",

number = "1",