2022A&A...657L...6A


Query : 2022A&A...657L...6A

2022A&A...657L...6A - Astronomy and Astrophysics, volume 657, L6-6 (2022/1-1)

Explodability fluctuations of massive stellar cores enable asymmetric compact object mergers such as GW190814.

ANTONIADIS J., AGUILERA-DENA D.R., VIGNA-GOMEZ A., KRAMER M., LANGER N., MULLER B., TAURIS T.M., WANG C. and XU X.-T.

Abstract (from CDS):

The first three observing runs with Advanced LIGO and Virgo have resulted in the detection of binary black hole (BBH) mergers with highly unequal mass components, which are difficult to reconcile with standard formation paradigms. The most representative of these is GW190814, a highly asymmetric merger between a 23 M black hole (BH) and a 2.6 M compact object. Here, we explore recent results, suggesting that a sizable fraction of stars with pre-collapse carbon-oxygen core masses above 10 M, and extending up to at least 30 M, may produce objects inside the so-called lower mass gap that bridges the division between massive pulsars and BHs in Galactic X-ray binaries. We demonstrate that such an explosion landscape would naturally cause a fraction of massive binaries to produce GW190814-like systems instead of symmetric-mass BBHs. We present examples of specific evolutionary channels leading to the formation of GW190814 and GW200210, a 24 + 2.8 M merger discovered during the O3b observing run. We estimate the merger-rate density of these events in our scenario to be O(5%) of the total BBH merger rate. Finally, we discuss the broader implications of this formation channel for compact object populations, and its possible relevance to less asymmetric merger events such as GW200105 and GW200115.

Abstract Copyright: © J. Antoniadis et al. 2022

Journal keyword(s): gravitational waves - stars: massive - stars: black holes - stars: neutron - binaries: close - supernovae: general

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10530 1
2 V* BP Cru HXB 12 26 37.5605188992 -62 46 13.261044684   12.70 10.66     B1.5Iaeq 657 0
3 GrW 150914 GWE ~ ~           ~ 518 1
4 GrW 200115 GWE ~ ~           ~ 61 0
5 GrW 200210 092254 GWE ~ ~           ~ 11 0
6 GrW 190814 GWE ~ ~           ~ 240 0
7 GrW 200105 GWE ~ ~           ~ 53 0

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2023.01.30-21:51:40

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