Dark matter or regular matter in neutron stars? How to tell the difference from the coalescence of compact objects

Hippert, Maurício; Emily, Dillingham,; Tan, Hung; Curtin, David; Noronha-Hostler, Jacquelyn; Yunes, Nicolás

doi:10.1103/physrevd.107.115028

Cited by 21 publications

(4 citation statements)

References 101 publications

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“…On much smaller scales, the signatures of an ADM subcomponent can potentially be spectacular. The ADM gas clouds can collapse and condense into dark compact objects, giving rise to dark white dwarfs (Ryan & Radice 2022) and non-stellar-mass black holes (Shandera et al 2018;Fernandez et al 2022), as well as mirror (neutron) stars (Curtin & Setford 2020a, 2020bHippert et al 2023Hippert et al , 2022 if there is dark nuclear physics).…”

Section: Introductionmentioning

confidence: 99%

Simulating Atomic Dark Matter in Milky Way Analogs

Roy,

Shen,

Lisanti

et al. 2023

ApJL

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Dark sector theories naturally lead to multicomponent scenarios for dark matter where a subcomponent can dissipate energy through self-interactions, allowing it to efficiently cool inside galaxies. We present the first cosmological hydrodynamical simulations of Milky Way analogs where the majority of dark matter is collisionless cold dark matter (CDM) but a subcomponent (6%) is strongly dissipative minimal atomic dark matter (ADM). The simulations, implemented in GIZMO and utilizing FIRE-2 galaxy formation physics to model the standard baryonic sector, demonstrate that the addition of even a small fraction of dissipative dark matter can significantly impact galactic evolution despite being consistent with current cosmological constraints. We show that ADM gas with roughly standard model–like masses and couplings can cool to form a rotating “dark disk” with angular momentum closely aligned with the visible stellar disk. The morphology of the disk depends sensitively on the parameters of the ADM model, which affect the cooling rates in the dark sector. The majority of the ADM gas gravitationally collapses into dark “clumps” (regions of black hole or mirror star formation), which form a prominent bulge and a rotating thick disk in the central galaxy. These clumps form early and quickly sink to the inner ∼kiloparsec of the galaxy, affecting the galaxy’s star formation history and present-day baryonic and CDM distributions.

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Section: Introductionmentioning

confidence: 99%

Simulating Atomic Dark Matter in Milky Way Analogs

Roy,

Shen,

Lisanti

et al. 2023

ApJL

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“…We focus on electromagnetic signals of mirror stars, but microlensing surveys will also be highly sensitive in the near future; see Winch et al (2022). Furthermore, mirror stellar relics are expected to give rise to distinctive gravitationalwave signals from merger events, including mirror white dwarfs (Ryan & Radice 2022), mirror neutron stars (Hippert et al 2022(Hippert et al , 2023, and black holes with unusual masses sourced by ADM collapse (Pollack et al 2015;Shandera et al 2018;Singh et al 2021;Gurian et al 2022b;Fernandez et al 2024). simulated in Roy et al (2023) We now briefly summarize the most important points of the analyzes by Curtin & Setford (2020a, 2020b, which demonstrated the existence of observable optical and X-ray signatures of mirror stars.…”

Section: Mirror Star Reviewmentioning

confidence: 99%

Electromagnetic Signatures of Mirror Stars

Armstrong,

Gurbuz,

Curtin

et al. 2024

ApJ

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Mirror stars are a generic prediction of dissipative dark matter (DM) models, including minimal atomic DM and twin baryons in the mirror twin Higgs model. Mirror stars can capture regular matter from the interstellar medium through extremely suppressed kinetic mixing interactions between the regular and the dark photon. This accumulated “nugget” will draw heat from the mirror star core and emit highly characteristic X-ray and optical signals. In this work, we devise a general parameterization of mirror star nugget properties that is independent of the unknown details of mirror star stellar physics, and use the Cloudy spectral synthesis code to obtain realistic and comprehensive predictions for the thermal emissions from optically thin mirror star nuggets. We find that mirror star nuggets populate an extremely well-defined and narrow region of the Hertzsprung–Russell diagram that only partially overlaps with the white dwarf population. Our detailed spectral predictions, which we make publicly available, allow us to demonstrate that optically thin nuggets can be clearly distinguished from white dwarf stars by their continuum spectrum shape, and from planetary nebulae and other optically thin standard sources by their highly exotic emission-line ratios. Our work will enable realistic mirror star telescope searches, which may reveal the detailed nature of DM.

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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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Dark matter or regular matter in neutron stars? How to tell the difference from the coalescence of compact objects

Cited by 21 publications

References 101 publications

Simulating Atomic Dark Matter in Milky Way Analogs

Simulating Atomic Dark Matter in Milky Way Analogs

Electromagnetic Signatures of Mirror Stars

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

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