Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 500, Issue 2, Pages 1817-1832Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa3372
Keywords
gravitational waves; black holes; stars: neutron
Categories
Funding
- David and Ellen Lee Fellowship at Caltech - Gordon and Betty Moore Foundation [GBMF5076]
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The researchers propose that the GW190814 event may be a second-generation merger from a hierarchical triple system based on the component masses and rates of coalescence. Their model provides several predictions and areas for further research in understanding these types of systems in the universe.
The LIGO-Virgo collaboration recently reported a puzzling event, GW190814, with component masses of 23 and 2.6 M-circle dot. Motivated by the relatively small rate of such a coalescence (1-23 Gpc(-3) yr(-1)) and the fact that the mass of the secondary is close to the total mass of known binary neutron star (bNS) systems, we propose that GW190814 was a second-generation merger from a hierarchical triple system; i.e. the remnant from the bNS coalescence was able to merge again with the 23 M-circle dot black hole (BH) tertiary. We show that this occurs at a sufficiently high probability provided that the semimajor axis of the outer orbit is less than a few au at the time of bNS coalescence. It remains to be explored whether the conditions for the formation of such tight triple systems are commonly realized in the Universe, especially in low-metallicity (less than or similar to 0.1 Z(circle dot)) environments. Our model provides a number of predictions. (1) The spin of the secondary in GW190814-like systems is 0.6-0.7. (2) The component mass distribution from a large sample of LIGO sources should have a narrow peak between 2.5 and similar to 3.5 M-circle dot, whereas the range between similar to 3.5 and similar to 5 M-circle dot stays empty (provided that stellar evolution does not generate such BHs in the 'mass gap'). (3) About 90 per cent (10 per cent) of GW190814-like events have an eccentricity of e greater than or similar to 2 x 10(-3) (greater than or similar to 0.1) near gravitational wave frequency of 10 mHz. (4) A significant fraction (greater than or similar to 10 per cent) of bNS mergers should have signatures of a massive tertiary at a distance of a few au in the gravitational waveform. (5) There are 10(5) undetected radio-quiet bNS systems with a massive BH tertiary in the Milky Way.
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