Constraints on the fermionic dark matter from observations of neutron stars

Sagun, V. V.; Giangrandi, Edoardo; Ivanytskyi, O.; Lopes, Ilídio; Bugaev, K. A.

doi:10.22323/1.380.0313

Cited by 10 publications

(12 citation statements)

References 11 publications

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“…Numerous studies suggest that dark matter can cluster around and inside compact objects such as neutron stars, e.g., [10][11][12][13][14][15][16][17][18][19][20][21]. As a result, dark matter may increase the total gravitational mass of a neutron star due to an extended halo formation or, on the contrary, reduce it, due to the formation of a dense core, e.g., [9,[22][23][24].…”

Section: Introductionmentioning

confidence: 99%

Numerical Simulations of Dark Matter Admixed Neutron Star Binaries

et al. 2022

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Multi-messenger observations of compact binary mergers provide a new way to constrain the nature of dark matter that may accumulate in and around neutron stars. In this article, we extend the infrastructure of our numerical-relativity code BAM to enable the simulation of neutron stars that contain an additional mirror dark matter component. We perform single star tests to verify our code and the first binary neutron star simulations of this kind. We find that the presence of dark matter reduces the lifetime of the merger remnant and favors a prompt collapse to a black hole. Furthermore, we find differences in the merger time for systems with the same total mass and mass ratio, but different amounts of dark matter. Finally, we find that electromagnetic signals produced by the merger of binary neutron stars admixed with dark matter are very unlikely to be as bright as their dark matter-free counterparts. Given the increased sensitivity of multi-messenger facilities, our analysis gives a new perspective on how to probe the presence of dark matter.

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Section: Introductionmentioning

confidence: 99%

Numerical Simulations of Dark Matter Admixed Neutron Star Binaries

et al. 2022

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“…A more detailed investigation on the size of the DM inside the star can be easily performed by adopting the two-fluid approach, in which profiles of each component can be obtained separately and, consequently, precise information regarding DM halos or DM concentrated in the CS core can be extracted. In a recent study performed in Sagun et al (2022); Giangrandi et al (2022), for instance, the authors shown that accumulated DM inside the star favor the compatibility with the GW170817 data.…”

Section: Mass-radius Diagrams and Tidal Deformabilitymentioning

confidence: 96%

Dark particle mass effects on neutron star properties from a short-range correlated hadronic model

Dutra

Lenzi

Lourenço

2022

Monthly Notices of the Royal Astronomical Society

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In this work we study a relativistic mean-field (RMF) hadronic model, with nucleonic short-range correlations (SRC) included, coupled to dark matter (DM) through the Higgs boson. We study different parametrizations of this model by running the dark particle Fermi momentum, and its mass in the range of 50GeV ≤ Mχ ≤ 500GeV, compatible with experimental spin-independent scattering cross-sections. By using this RMF-SRC-DM model, we calculate some neutron star quantities, namely, mass-radius profiles, dimensionless tidal deformabilities, and crustal properties. Our findings show that is possible to construct RMF-SRC-DM parametrizations in agreement with constraints provided by LIGO and Virgo collaboration (LVC) on the GW170817 event, and recent observational data from the NICER mission. Furthermore, we show that the increase of Mχ favors the model to attain data from LVC regarding the tidal deformabilities. Higher values of Mχ also induce a reduction of the neutron star crust (mass and thickness), and cause a decrease of the crustal fraction of the moment of inertia (Icrust/I). Nevertheless, we show that some RMF-SRC-DM parametrizations still exhibit $I_{\mbox{crust}}/I>7\%$, a condition that explains the glitch activity in rotation-powered pulsars such as the Vela one. Therefore, dark matter content can also be used for describing such a phenomenon.

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“…Due to their high compactness, NSs can trap and accumulate DM in their interior throughout the star's evolution. DM alters the compact star's properties, e. g., its mass, its radius, its tidal deformability, its energy density and speed of sound profiles [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15]. Its effect depends on the relative fraction of DM and on the exact equation of state (EoS) for the DM and baryonic matter (BM).…”

Section: Introductionmentioning

confidence: 99%

“…This assumption is in very good agreement with the observations of the Bullet Cluster [55,56] and direct DM searches [57], which show that the DM-BM cross section to be many orders of magnitude lower than the typical nuclear one, σ DM −BM ≈ 10 −45 cm 2 σ BM ∼ 10 −24 cm 2 . By varying the particle mass and relative fraction of DM, we obtain either a core configuration with a radius of the DM component less or equal to the baryonic one, R D ≤ R B , or a halo with R D > R B [58]. For both scenarios, we construct initial configurations employing SGRID [59,60].…”

Section: Introductionmentioning

confidence: 99%

Quasi-equilibrium configurations of binary systems of dark matter admixed neutron stars

Rüter¹,

Sagun²,

Tichy³

et al. 2023

Preprint

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Using an adapted version of the SGRID code, we construct for the first time consistent quasiequilibrium configurations for a binary system consisting of two neutron stars in which each is admixed with dark matter. The stars are modelled as a system of two non-interacting fluids minimally coupled to gravity. For the fluid representing baryonic matter the SLy equation of state is used, whereas the second fluid, which corresponds to dark matter, is described using the equation of state of a degenerate Fermi gas. We consider two different scenarios for the distribution of the dark matter. In the first scenario the dark matter is confined to the core of the star, whereas in the second scenario the dark matter extends beyond the surface of the baryonic matter, forming a halo around the baryonic star. The presence of dark matter alters the star's reaction to the companion's tidal forces, which we investigate in terms of the coordinate deformation and mass shedding parameters. The constructed quasi-equilibrium configurations mark the first step towards consistent numerical-relativity simulations of dark matter admixed neutron star binaries.

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Constraints on the fermionic dark matter from observations of neutron stars

Cited by 10 publications

References 11 publications

Numerical Simulations of Dark Matter Admixed Neutron Star Binaries

Numerical Simulations of Dark Matter Admixed Neutron Star Binaries

Dark particle mass effects on neutron star properties from a short-range correlated hadronic model

Quasi-equilibrium configurations of binary systems of dark matter admixed neutron stars

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