Compact dark objects in neutron star mergers

Bauswein, Andreas; Guo, Gang; Lien, Jr-Hua; Lin, Yen-Hsun; Wu, Meng-Ru

doi:10.1103/physrevd.107.083002

Cited by 18 publications

(5 citation statements)

References 80 publications

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“…Moreover, the first studies show that DM might manifest itself with an additional peak or pronounced oscillation mode in the post-merger GW spectrum [22], generation of an exotic waveform [23], modification in the kilonova ejecta [24], formation of a one-arm spiral instability [25], etc. [26][27][28]. These smoking-gun signals are expected to become feasible with the next generation of GW detectors, i.e., the Einstein Telescope [29], Cosmic Explorer [30], and NEMO [31].…”

Section: Introductionmentioning

confidence: 99%

The Impact of Asymmetric Dark Matter on the Thermal Evolution of Nucleonic and Hyperonic Compact Stars

Giangrandi,

Ávila,

Sagun

et al. 2024

Particles

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We investigate the impact of asymmetric fermionic dark matter (DM) on the thermal evolution of neutron stars (NSs), considering a scenario where DM interacts with baryonic matter (BM) through gravity. Employing the two-fluid formalism, our analysis reveals that DM accrued within the NS core exerts an inward gravitational pull on the outer layers composed of BM. This gravitational interaction results in a noticeable increase in baryonic density within the core of the NS. Consequently, it strongly affects the star’s thermal evolution by triggering the early onsets of the direct Urca (DU) processes, causing enhanced neutrino emission and rapid star cooling. Moreover, the photon emission from the star’s surface is modified due to a reduction in radius. We demonstrate the effect of DM gravitational pull on nucleonic and hyperonic DU processes that become kinematically allowed even for NSs of low mass. We then discuss the significance of observing NSs at various distances from the Galactic center. Given that the DM distribution peaks toward the Galactic center, NSs within this central region are expected to harbor higher fractions of DM, potentially leading to distinct cooling behaviors.

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Section: Introductionmentioning

confidence: 99%

The Impact of Asymmetric Dark Matter on the Thermal Evolution of Nucleonic and Hyperonic Compact Stars

Giangrandi,

Ávila,

Sagun

et al. 2024

Particles

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“…Moreover, for asymmetric DM, in which a particle-antiparticle asymmetry exists in the dark sector [50], and also self-annihilating (symmetric) DM, the cooling and heating of NSs could be altered, which may help to interpret the thermal evolution of NSs [51][52][53][54][55]. In addition, DM core or halo formations within NSs can influence the inspiral phase of their binary systems and also the corresponding gravitational wave (GW) signals, especially in the post-merger stage [56][57][58][59][60][61]. Thanks to the precise mass-radius measurements based on pulse-profile modeling by the NICER telescope [62][63][64], a novel approach has been introduced to probe a DM halo around NSs [11,65], where the variation in the minima in pulse profiles can be severed as a notable signature of the DM halo.…”

Section: Introductionmentioning

confidence: 99%

Exploring the Distribution and Impact of Bosonic Dark Matter in Neutron Stars

Rafiei Karkevandi,

Shahrbaf,

Shakeri

et al. 2024

Particles

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The presence of dark matter (DM) within neutron stars (NSs) can be introduced by different accumulation scenarios in which DM and baryonic matter (BM) may interact only through the gravitational force. In this work, we consider asymmetric self-interacting bosonic DM, which can reside as a dense core inside the NS or form an extended halo around it. It is seen that depending on the boson mass (mχ), self-coupling constant (λ) and DM fraction (Fχ), the maximum mass, radius and tidal deformability of NSs with DM admixture will be altered significantly. The impact of DM causes some modifications in the observable features induced solely by the BM component. Here, we focus on the widely used nuclear matter equation of state (EoS) called DD2 for describing NS matter. We show that by involving DM in NSs, the corresponding observational parameters will be changed to be consistent with the latest multi-messenger observations of NSs. It is seen that for mχ≳200 MeV and λ≲2π, DM-admixed NSs with 4%≲Fχ≲20% are consistent with the maximum mass and tidal deformability constraints.

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“…Moreover, DM will affect tidal deformability parameters and merger dynamics (Ellis et al 2018a;Bezares et al 2019;Leung et al 2022;Bauswein et al 2023). Nowadays, while there are studies investigating possible alternative scenarios beyond standard compact binary mergers described by general relativity in pure vacuum (Abbott et al 2019a), the models used to analyze GW signal do not account directly for DM.…”

Section: Introductionmentioning

confidence: 99%

“…Thus, to understand the effect of DM on the coalescence of NSs, numerical-relativity simulations for different DM fractions, particle mass, and interaction strength are required (Rüter et al2023). As a step in this direction, there have been the first two-fluid 3D simulations of coalescing binary NS admixed with DM with the following studies of GW emission of the merger remnant, e.g., Bauswein et al (2023) and Emma et al (2022). By considering different binary masses and EoSs, Bauswein et al (2023) showed that the GW frequency of the orbiting DM components scales with the compactness of NSs.…”

Section: Introductionmentioning

confidence: 99%

“…As a step in this direction, there have been the first two-fluid 3D simulations of coalescing binary NS admixed with DM with the following studies of GW emission of the merger remnant, e.g., Bauswein et al (2023) and Emma et al (2022). By considering different binary masses and EoSs, Bauswein et al (2023) showed that the GW frequency of the orbiting DM components scales with the compactness of NSs. Moreover, the relations between the DM GW frequency and the dominant post-merger GW frequency of the stellar fluid or the tidal deformability were found, which opens a possibility to probe the EoS effects during the binary inspiral.…”

Section: Introductionmentioning

confidence: 99%

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The Effects of Self-interacting Bosonic Dark Matter on Neutron Star Properties

Giangrandi

Sagun

Ivanytskyi

et al. 2023

ApJ

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We propose a model of asymmetric bosonic dark matter (DM) with self-repulsion. By adopting the two-fluid formalism, we study different DM distribution regimes, either, fully condensed inside the core of a star, or, otherwise, distributed in a dilute halo around a neutron star (NS). We show that for a given total gravitational mass, DM condensed in a core leads to a smaller radius and tidal deformability compared to a pure baryonic star. This effect may be interpreted as an effective softening of the equation of state. On the other hand, the presence of a DM halo increases the tidal deformability and total gravitational mass. As a result, an accumulated DM inside compact stars could mimic an apparent softening/stiffening of strongly interacting matter EoS and constraints we impose on it at high densities. We limit the model parameter space by confronting the cross section of the DM self-interaction to the constraint extracted from the analysis of the Bullet Cluster. Furthermore, from the analysis of the effect of DM particles, interaction strength, and relative DM fractions inside NSs we obtained a rigorous constraint on model parameters. To identify its impact on NSs we consider the DM fraction may reach up to 5%, which could be considered too high in several scenarios. Finally, we discuss several pieces of smoking gun evidence of the presence of DM that is free from the abovementioned degeneracy between the effect of DM and properties of strongly interacting matter. These signals could be probed with future and ongoing astrophysical and gravitational wave surveys.

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Compact dark objects in neutron star mergers

Cited by 18 publications

References 80 publications

The Impact of Asymmetric Dark Matter on the Thermal Evolution of Nucleonic and Hyperonic Compact Stars

The Impact of Asymmetric Dark Matter on the Thermal Evolution of Nucleonic and Hyperonic Compact Stars

Exploring the Distribution and Impact of Bosonic Dark Matter in Neutron Stars

The Effects of Self-interacting Bosonic Dark Matter on Neutron Star Properties

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