TY - JOUR
T1 - Constraining properties of asymmetric dark matter candidates from gravitational-wave observations
AU - Singh, Divya
AU - Gupta, Anuradha
AU - Berti, Emanuele
AU - Reddy, Sanjay
AU - Sathyaprakash, B. S.
N1 - Funding Information:
We thank K. Belczynski for useful discussions on BNS delay times, as well as M. Baryakhtar and T. Slatyer for discussions on the DM scenarios considered in this paper. D. S. and B. S. S. were supported in part by NSF Grants No. PHY-1836779, No. PHY-2012083, No. AST-2006384, and No. PHY-2207638. A. G. is supported by NSF Grant No. AST-2205920. E. B. is supported by NSF Grants No. AST-2006538, No. PHY-2207502, No. PHY-090003, and No. PHY20043, and NASA Grants No. 19-ATP19-0051, No. 20-LPS20-0011, and No. 21-ATP21-0010. This research project was conducted using computational resources at the Maryland Advanced Research Computing Center (MARCC). S. R. is supported by the U.S. Department of Energy under Award No. DE-FG02- 00ER41132 and National Science Foundation’s Physics Frontier Center: The Network for Neutrinos, Nuclear Astrophysics, and Symmetries. Part of the work by E. B. and B. S. S. was performed at the Aspen Center for Physics, which is supported by National Science Foundation Grant No. PHY-1607611. This research was also supported in part by the National Science Foundation under Grant No. NSF PHY-1748958.
Publisher Copyright:
© 2023 American Physical Society.
PY - 2023/4/15
Y1 - 2023/4/15
N2 - 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 ∼1-2M⊙, 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.
AB - 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 ∼1-2M⊙, 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.
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U2 - 10.1103/PhysRevD.107.083037
DO - 10.1103/PhysRevD.107.083037
M3 - Article
AN - SCOPUS:85158818795
SN - 2470-0010
VL - 107
JO - Physical Review D
JF - Physical Review D
IS - 8
M1 - 083037
ER -