A lower bound on the maximum mass if the secondary in GW190814 was once a rapidly spinning neutron star

被引：130

作者：

Most, Elias R. ^{[1
]}

Papenfort, L. Jens ^{[1
]}

Weih, Lukas R. ^{[1
]}

Rezzolla, Luciano ^{[1
,2
,3
]}

机构：

[1] Goethe Univ, Inst Theoret Phys, Max Von Laue Str 1, D-60438 Frankfurt, Germany

[2] Trinity Coll Dublin, Sch Math, Dublin 2, Ireland

[3] Helmholtz Res Acad Hesse FAIR, Max Von Laue Str 12, D-60438 Frankfurt, Germany

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 499卷 / 01期

关键词：

gravitational waves; stars: neutron; black hole; neutron star mergers; STABILITY;

D O I：

10.1093/mnrasl/slaa168

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The recent detection of GW190814 featured the merger of a binary with a primary having a mass of similar to 23 M-circle dot and a secondary with a mass of similar to 2.6 M-circle dot. While the primary was most likely a black hole, the secondary could be interpreted as either the lightest black hole or the most massive neutron star ever observed, but also as the indication of a novel class of exotic compact objects. We here argue that although the secondary in GW190814 is most likely a black hole at merger, it needs not be an ab-initio black hole nor an exotic object. Rather, based on our current understanding of the nuclear-matter equation of state, it can be a rapidly rotating neutron star that collapsed to a rotating black hole at some point before merger. Using universal relations connecting the masses and spins of uniformly rotating neutron stars, we estimate the spin, 0.49(-0.05)(+0.08) less than or similar to chi less than or similar to 0.68(-0.05)(+0.11), of the secondary - a quantity not constrained so far by the detection - and a novel strict lower bound on the maximum mass, M-TOV > 2.08(-0.04)(+0.04) M-circle dot and an optimal bound of M-TOV > 2.15(-0.04)(+0.04) M-circle dot, of non-rotating neutron stars, consistent with recent observations of a very massive pulsar. The new lower bound also remains valid even in the less likely scenario in which the secondary neutron star never collapsed to a black hole.

引用

页码：L82 / L86

页数：5

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