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
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
收藏
页码:L82 / L86
页数:5
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