Constraining properties of asymmetric dark matter candidates from gravitational-wave observations
Constraining properties of asymmetric dark matter candidates from gravitational-wave observations
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DOI：
10.1103/physrevd.107.083037
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发表时间：
2022-10
影响因子：
5
通讯作者：
Divya Singh;Anuradha Gupta;E. Berti;S. Reddy;B. Sathyaprakash
中科院分区：
文献类型：
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作者：
Divya Singh;Anuradha Gupta;E. Berti;S. Reddy;B. Sathyaprakash
中子星星核中某些类型的暗物质粒子由于长时间的吸积而积累，可能导致迷你黑洞的形成。在这种情况下，中子星星不稳定并坍缩形成黑洞，而不会显着增加其质量。当这一过程发生在合并双星中的中子星时，一颗或两颗恒星可能在合并前转化为黑洞。因此，在质量范围为$\sim \mbox{1- 2}\，M_\odot，$的宇宙可能包含三个不同的致密双星群体：一个只包含中子星，第二个群体只有黑洞，第三个，由中子星星和黑洞组成的混合群体。然而，它不太可能有混合的种群，因为不同的时间尺度允许两颗中子星在短时间尺度内保留或坍缩。在本文中，我们探讨了未来的引力波探测器网络的能力，包括升级先进的LIGO和处女座，以及新的设施，如宇宙探测器和爱因斯坦望远镜（XG网络），通过测量有效的潮汐变形的二进制，这是零的二元黑洞，但非零的二元中子星区分不同的人群。此外，我们表明，观察不同种群的相对丰度可以用来推断中子星内爆成黑洞的时间尺度，反过来，提供对暗物质粒子性质的约束。XG网络将在90%的可信区间内推断出内爆时间尺度在0.01 Gyr的精度内，并确定暗物质质量和相互作用截面分别在2 GeV和10 cm$^{-2}$的因子内。
The accumulation of certain types of dark matter particles in neutron star cores due to accretion over long timescales can lead to the formation of a mini black hole. In this scenario, the neutron star is destabilized and implodes to form a black hole without significantly increasing its mass. When this process occurs in neutron stars in coalescing binaries, one or both stars might be converted to a black hole before they merge. Thus, in the mass range of $\sim \mbox{1--2}\, M_\odot,$ the Universe might contain three distinct populations of compact binaries: one containing only neutron stars, the second population of only black holes, and a third, mixed population consisting of a neutron star and a black hole. However, it is unlikely to have a mixed population as the various timescales allow for both neutron stars to remain or collapse within a short timescale. In this paper, we explore the capability of future gravitational-wave detector networks, including upgrades of Advanced LIGO and Virgo, and new facilities such as the Cosmic Explorer and Einstein Telescope (XG network), to discriminate between different populations by measuring the effective tidal deformability of the binary, which is zero for binary black holes but nonzero for binary neutron stars. Furthermore, we show that observing the relative abundances of the different populations can be used to infer the timescale for neutron stars to implode into black holes, and in turn, provide constraints on the particle nature of dark matter. The XG network will infer the implosion timescale to within an accuracy of 0.01 Gyr at 90% credible interval and determine the dark matter mass and interaction cross section to within a factor of 2 GeV and 10 cm$^{-2}$, respectively.