Numerical Simulations of Dark Matter Admixed Neutron Star Binaries

Emma, Mattia; Schianchi, Federico; Pannarale, F.; Sagun, V. V.; Dietrich, Tim

doi:10.3390/particles5030024

Cited by 24 publications

(13 citation statements)

References 79 publications

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“…We have shown that the presence of DM can delay the point of mass-shedding to a later stage of the inspiral, i. e., towards closer separations. This is in accordance with the findings in numerical evolutions of two-fluid binary mergers [25]. In the case of a DM halo, mass shedding could occur much earlier than for the baryonic component.…”

Section: Discussionsupporting

confidence: 92%

“…These quasiequlibrium configurations can be used as initial data for NR inspiral simulations of DM admixed NS binaries. The BAM code can already evolve mirror DM [25] and could be easily extended to allow for general EoS for the DM fluid.…”

Section: Discussionmentioning

confidence: 99%

“…Up to our knowledge, the first two-fluid NR simulations describing binaries of DM admixed NSs were performed by Emma et al [25] for a mixture of BM and mirror DM only interacting via the gravitational field. The results demonstrate that these systems tend to have a longer inspiral phase with increasing amount of DM, which could be associated to the lower deformability of DM admixed NSs.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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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Section: Discussionsupporting

confidence: 92%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Rüter¹,

Sagun²,

Tichy³

et al. 2023

Preprint

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“…The results summarized above differ from other recent studies on mirror matter admixture on NSs [8,49,50] and binary NS mergers [51]. These other studies explored mirror matter candidates that, apart from discrete symmetries, are identical to SM particles.…”

Section: Introductioncontrasting

confidence: 81%

Dark Matter or Regular Matter in Neutron Stars? How to tell the difference from the coalescence of compact objects

Hippert¹,

Emily²,

Tan³

et al. 2022

Preprint

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The mirror twin Higgs model is a candidate for (strongly-interacting) complex dark matter, which mirrors SM interactions with heavier quark masses. A consequence of this model are mirror neutron stars -exotic stars made entirely of mirror matter, which are significantly smaller than neutron stars and electromagnetically dark. This makes mergers of two mirror neutron stars detectable and distinguishable in gravitational wave observations, but can we observationally distinguish between regular neutron stars and those that may contain some mirror matter? This is the question we study in this paper, focusing on two possible realizations of mirror matter coupled to standard model matter within a compact object: (i) mirror matter captured by a neutron star and (ii) mirror neutron star-neutron star coalescences. Regarding (i), we find that (non-rotating) mirror-matter-admixed neutron stars no longer have a single mass-radius sequence, but rather exist in a two-dimensional mass-radius plane. Regarding (ii), we find that binary systems with mirror neutron stars would span a much wider range of chirp masses and completely different binary Love relations, allowing merger remnants to be very light black holes. The implications of this are that gravitational wave observations with advanced LIGO and Virgo, and X-ray observations with NICER, could detect or constrain the existence of mirror matter through searches with wider model and parameter priors.

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“…In addition to LIGO/Virgo/KAGRA results Abbott et al (2021), this bound could be further constrain thanks to the upcoming GW missions such as LISA Baker et al (2019) and Einstein telescopes Maggiore et al (2020). Note that the presence of DM core/halo should be precisely taken into account in numerical-relativity simulations to compute GW spectrum and waveforms during merger and postmerger phases of a binary system containing at least a DM admixed NS Ellis et al (2018a); Giudice et al (2016); Bezares et al (2019); Emma et al (2022).…”

Section: Conclusion and Remarksmentioning

confidence: 97%

Bosonic Dark Matter in Light of the NICER Precise Mass-Radius Measurements

Shakeri¹,

Karkevandi²

2022

Preprint

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We explore the presence of self-interacting bosonic dark matter (DM) whithin neutron stars (NSs) in light of the latest mass-radius measurements of the Neutron Star Interior Composition Explorer (NICER). The bosonic DM is distributed in NSs as a core for DM particles with high mass, low fraction and low self-coupling constant or as a halo for particles with low mass, high fraction and high self-coupling constant leading to formation of DM admixed NSs. We focus on the evolution of the visible and dark radius of the mixed object due to DM model parameters and fractions. It is shown that DM core formation reduces the visible radius and total mass pushing them below observational limits while halo formation is in favor of the latest mass-radius constraints. Applying joint constraints for radius of 1.4M NSs and the maximum mass from NICER and LIGO/Virgo observations, we scan over the parameter space of the bosonic DM model to obtain an allowed region. It turns out that the maximum mass limit provides a more stringent constraint compare to the radius one. Our investigation allows for the exclusion of a large portion of DM fractions for sub-GeV bosons and limited the amount of accumulated DM to be less than ∼ 4% for the entire mass range at the strong coupling regime λ = π. In this paper, we introduce main features of the pulse profile corresponding to the DM admixed NS and the effect of DM halo on the light bending is considered extensively as an independent probe for the DM model. We find that the depth of minimum fluxes in the pulse profiles crucially depend on the amount of DM distributed around NS and its compactness. The current/future astrophysics missions via precise measurements of compact object properties may test the possibility of the existence of DM within NSs and break the degeneracies between different scenarios to interpret exotic observations.

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Numerical Simulations of Dark Matter Admixed Neutron Star Binaries

Cited by 24 publications

References 79 publications

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

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

Dark Matter or Regular Matter in Neutron Stars? How to tell the difference from the coalescence of compact objects

Bosonic Dark Matter in Light of the NICER Precise Mass-Radius Measurements

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