Asymmetric dark matter stars

Kouvaris, Chris; Nielsen, Niklas Grønlund

doi:10.1103/physrevd.92.063526

Cited by 90 publications

(104 citation statements)

References 150 publications

(169 reference statements)

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“…[59]. The DM particles are non-self annihilating [60][61][62][63][64], and selfinteracting [65]. Differently from [58], where the only DM mass considered was 100 GeV, in this paper we take into account DM particle masses equal to 1, 5, 10, 50, 100, 200, 500 GeV.…”

Section: Theoretical Modelmentioning

confidence: 99%

Dark compact objects: An extensive overview

et al. 2019

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We study the structure of compact objects that contain non-self annihilating, self-interacting dark matter admixed with ordinary matter made of neutron star and white dwarf materials. We extend the previous work Phys. Rev. D 92 123002 (2015) on these dark compact objects by analyzing the effect of weak and strongly interacting dark matter with particle masses in the range of 1-500 GeV, so as to set some constraints in the strength of the interaction and the mass of the dark matter particle. We find that the total mass of the compact objects increases with decreasing dark matter particle mass. In the strong interacting case and for dark matter particle masses in the range 1-10 GeV, the total mass of the compact objects largely exceeds the 2M constraint for neutron star masses and the nominal 1M for white dwarfs, while for larger dark matter particle masses or in the weakly interacting case the compact objects show masses in agreement or smaller than these constraints, thus hinting at the exclusion of strongly self-interacting dark matter of masses 1-10 GeV in the interior of these compact objects. Moreover, we observe that the smaller the dark matter particle mass, the larger the quantity of dark matter captured is, putting constraints on the dark matter mass trapped in the compact objects so as to fullfill 2M observations. Finally, the inhomogeneity of distribution of dark matter in the Galaxy implies a mass dependence of compact objects from the environment which can be used to put constraints on the characteristics of the Galaxy halo DM profile and on particle mass. In view of the these results, we discuss the formation of the dark compact objects in an homogeneous and non-homogeneous dark matter environment. In the ΛCDM model, a parameterization of the big-bang cosmology with six parameters, the DE is associated with the cosmological constant Λ, and the material components of the Universe are the ones indicated previously. The quoted ΛCDM paradigm, describes correctly many of the observations[2, 6-9], but has some drawbacks. On large scale CMB shows some anomalies, such as that the Planck 2015 data are in tension with the CFHTLenS weak lensing [10], and σ 8 [11]. There is also another tension with the value of the Hubble parameter measured by SNIa 1 . Another big issue of the paradigm is the nature of DM. A "zoo" of candidates have been proposed, with masses in the range of 10 −33 GeV (Fuzzy DM) to 10 15 GeV (Wimpzillas). In that large "zoo", 1 The ΛCDM paradigm has some other drawbacks, as the cosmological constant problem [12,13], the unknown nature of DE [14-16] and the so called "small scale problems" [17].

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Section: Theoretical Modelmentioning

confidence: 99%

Dark compact objects: An extensive overview

et al. 2019

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“…Eq. (35). We also analyse the parameter space region in which the black hole formed does not evaporate, but rather grows by accretion of both dark matter and stellar material, eventually consuming the white dwarf.…”

Section: Dark Matter Collapse and Heating To Critical Temperaturementioning

confidence: 99%

“…The mass of dark matter required to form a black hole will depend on the spin of the dark matter field and its self-couplings [35,36,67]. In the case of a Higgs portal dark matter model examined in Section 5, the dark matter self-interactions are attractive and do not preclude the black hole formation.…”

Section: Black Hole Formation From Collapsing Dark Mattermentioning

confidence: 99%

Supernovae sparked by dark matter in white dwarfs

Acevedo

Bramante

2019

Phys. Rev. D

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It was recently demonstrated that asymmetric dark matter can ignite supernovae by collecting and collapsing inside lone sub-Chandrasekhar mass white dwarfs, and that this may be the cause of Type Ia supernovae. A ball of asymmetric dark matter accumulated inside a white dwarf and collapsing under its own weight, sheds enough gravitational potential energy through scattering with nuclei, to spark the fusion reactions that precede a Type Ia supernova explosion. In this article we elaborate on this mechanism and use it to place new bounds on interactions between nucleons and asymmetric dark matter for masses m X = 10 6 − 10 16 GeV. Interestingly, we find that for dark matter more massive than 10 11 GeV, Type Ia supernova ignition can proceed through the Hawking evaporation of a small black hole formed by the collapsed dark matter. We also identify how a cold white dwarf's Coulomb crystal structure substantially suppresses dark matter-nuclear scattering at low momentum transfers, which is crucial for calculating the time it takes dark matter to form a black hole. Higgs and vector portal dark matter models that ignite Type Ia supernovae are explored.

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“…Constraints on the properties of dark matter candidates can be obtained from stars which can accrete asymmetric dark matter in its lifetime and then collapse into a neutron star [14]. Constraints on the mass of dark matter candidates can also be obtained by the possible collapse of compact stars due to dark matter accretion [15,16]. The cooling process of com-pact objects can be affected by the capture of dark matter which can annihilate the star [17].…”

Section: Introductionmentioning

confidence: 99%

Quark stars admixed with dark matter

Mukhopadhyay

Schaffner-Bielich

2016

Phys. Rev. D

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Compact stars consisting of massless quark matter and fermionic dark matter are studied by solving the Tolman-Oppenheimer-Volkoff equations for two fluids separately. Dark matter is further investigated by incorporating inter-fermionic interactions among the dark matter particles. The properties of stars made of quark matter particles and self-interacting and free dark matter particles are explored by obtaining their mass-radius relations. The regions of stability for such a compact star are determined and it is demonstrated that the maximum stable total mass of such a star decreases approximately linearly with increasing dark matter fraction.

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Asymmetric dark matter stars

Cited by 90 publications

References 150 publications

Dark compact objects: An extensive overview

Dark compact objects: An extensive overview

Supernovae sparked by dark matter in white dwarfs

Quark stars admixed with dark matter

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