Neutron stars with a stable, light supersymmetric baryon

Shmuel Balberg; Glennys R. Farrar; Tsvi Piran

doi:10.1086/319101

Neutron stars with a stable, light supersymmetric baryon

Shmuel Balberg, Glennys R. Farrar, Tsvi Piran

Research output: Contribution to journal › Article › peer-review

Abstract

If a light gluino exists, the lightest gluino-containing baryon, S⁰, is a possible candidate for self-interacting dark matter. In this scenario, the simplest explanation for the observed ratio Ω_DM/Ω_b ≈ 6 - 10 is that m_S0 ≃ 900 MeV c^-2; at present, this is not excluded by particle physics. Such an S⁰ could be present in neutron stars, with the hyperon formation serving as an intermediate stage. We calculate equilibrium compositions and the equation of state for high-density matter with S⁰, and we find that for a wide range of parameters, the properties of neutron stars with S⁰ are consistent with observations. In particular, the maximum mass of a nonrotating star is 1.7 - 1.8 M⊙, and the presence of S⁰ is helpful in reconciling observed cooling rates with hyperon formation.

Original language	English (US)
Pages (from-to)	L179-L182
Journal	Astrophysical Journal
Volume	548
Issue number	2 PART 2
DOIs	https://doi.org/10.1086/319101
State	Published - Feb 20 2001

Keywords

Dark matter
Dense matter
Elementary particles
Equation of state
Stars: neutron

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/319101

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title = "Neutron stars with a stable, light supersymmetric baryon",

abstract = "If a light gluino exists, the lightest gluino-containing baryon, S0, is a possible candidate for self-interacting dark matter. In this scenario, the simplest explanation for the observed ratio ΩDM/Ωb ≈ 6 - 10 is that mS0 ≃ 900 MeV c-2; at present, this is not excluded by particle physics. Such an S0 could be present in neutron stars, with the hyperon formation serving as an intermediate stage. We calculate equilibrium compositions and the equation of state for high-density matter with S0, and we find that for a wide range of parameters, the properties of neutron stars with S0 are consistent with observations. In particular, the maximum mass of a nonrotating star is 1.7 - 1.8 M⊙, and the presence of S0 is helpful in reconciling observed cooling rates with hyperon formation.",

keywords = "Dark matter, Dense matter, Elementary particles, Equation of state, Stars: neutron",

author = "Shmuel Balberg and Farrar, {Glennys R.} and Tsvi Piran",

note = "Funding Information: The research of G. R. F. is supported in part by NSF grant PHY 99-96173. The idea that S0 could be a DM candidate and the constraints on such a scenario were developed by G. R. F. in collaboration with D. Spergel and P. Steinhardt. That work will be reported in greater depth elsewhere (G. R. Farrar, D. N. Spergel, & P. J. Steinhardt 2001, in preparation), but a brief description can be found in Wandelt et al. (2000). S. B. and T. P. thank NYU for the hospitality that facilitated this research.",

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AU - Farrar, Glennys R.

AU - Piran, Tsvi

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PY - 2001/2/20

Y1 - 2001/2/20

N2 - If a light gluino exists, the lightest gluino-containing baryon, S0, is a possible candidate for self-interacting dark matter. In this scenario, the simplest explanation for the observed ratio ΩDM/Ωb ≈ 6 - 10 is that mS0 ≃ 900 MeV c-2; at present, this is not excluded by particle physics. Such an S0 could be present in neutron stars, with the hyperon formation serving as an intermediate stage. We calculate equilibrium compositions and the equation of state for high-density matter with S0, and we find that for a wide range of parameters, the properties of neutron stars with S0 are consistent with observations. In particular, the maximum mass of a nonrotating star is 1.7 - 1.8 M⊙, and the presence of S0 is helpful in reconciling observed cooling rates with hyperon formation.

AB - If a light gluino exists, the lightest gluino-containing baryon, S0, is a possible candidate for self-interacting dark matter. In this scenario, the simplest explanation for the observed ratio ΩDM/Ωb ≈ 6 - 10 is that mS0 ≃ 900 MeV c-2; at present, this is not excluded by particle physics. Such an S0 could be present in neutron stars, with the hyperon formation serving as an intermediate stage. We calculate equilibrium compositions and the equation of state for high-density matter with S0, and we find that for a wide range of parameters, the properties of neutron stars with S0 are consistent with observations. In particular, the maximum mass of a nonrotating star is 1.7 - 1.8 M⊙, and the presence of S0 is helpful in reconciling observed cooling rates with hyperon formation.

KW - Dark matter

KW - Dense matter

KW - Elementary particles

KW - Equation of state

KW - Stars: neutron

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Neutron stars with a stable, light supersymmetric baryon

Abstract

Keywords

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