Mirror neutron stars

Hippert, Maurício; Setford, Jack; Tan, Hung; Curtin, David; Noronha-Hostler, Jacquelyn; Yunes, Nicolás

doi:10.1103/physrevd.106.035025

Cited by 28 publications

(31 citation statements)

References 165 publications

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“…If dark matter is more similar than not to baryonic matter, the dark sector may host a variety of new, interacting particles that give rise to phenomena as rich and diverse as the astrophysical structures of luminous matter. In particular, if the dark matter can efficiently dissipate its kinetic energy, then dark matter itself can collapse to form compact objects such as dark black holes (DBH; D' Amico et al 2018;Shandera et al 2018;Chang et al 2019;Choquette et al 2019;Latif et al 2019), dark white dwarfs (Ryan & Radice 2022), or dark neutron stars (Hippert et al 2022).…”

Section: Introductionmentioning

confidence: 99%

A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter

Gurian

Ryan

Schon

et al. 2022

ApJL

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We study the fragmentation scale of dark gas formed in dissipative dark-matter halos and show that the simple atomic-dark-matter model consistent with all current observations can create low-mass fragments that can evolve into compact objects forbidden by stellar astrophysics. We model the collapse of the dark halo’s dense core by tracing the thermochemical evolution of a uniform-density volume element under two extreme assumptions for density evolution: hydrostatic equilibrium and pressure-free collapse. We then compute the opacity-limited minimum fragment mass from the minimum temperature achieved in these calculations. The results indicate that much of the parameter space is highly unstable to small-scale fragmentation.

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Section: Introductionmentioning

confidence: 99%

A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter

Gurian

Ryan

Schon

et al. 2022

ApJL

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“…This is in contrast to other solutions to the hierarchy problem like TeV-scale supersymmetry, which predicts large LHC signals due to strong production cross sections for new particles, like stops and gluinos [40]. Additionally, because mirror matter contains multiple species that are strongly interacting, it is possible for mirror matter to clump together to form mirror neutron stars (MNSs) [29]. MNSs were found to be very similar to SM NSs, except that they are significantly smaller, with masses M ∼ (0.5 − 1)M and radii R ∼ (4 − 8) km [29].…”

Section: Introductionmentioning

confidence: 90%

“…In recent years, however, the possibility of complex, strongly self-interacting dark matter candidates has been suggested [26][27][28] and the consequence for compact objects explored [29,30]. Specifically, mirror matter [31][32][33][34][35] within the mirror Twin Higgs model [27,28,[35][36][37] is a nearly identical copy of the SM in its matter content and gauge interaction, except that the masses of fundamental particles are scaled up by a factor f /v, where f and v are vacuum expectation values of SM and mirror-sector Higgs fields, respectively.…”

Section: Introductionmentioning

confidence: 99%

“…Additionally, because mirror matter contains multiple species that are strongly interacting, it is possible for mirror matter to clump together to form mirror neutron stars (MNSs) [29]. MNSs were found to be very similar to SM NSs, except that they are significantly smaller, with masses M ∼ (0.5 − 1)M and radii R ∼ (4 − 8) km [29]. These MNSs are entirely new hypothesized, electromagnetically dark, compact objects with completely different mass-radius sequences from SM NSs.…”

Section: Introductionmentioning

confidence: 99%

“…In the inspiral, post-Newtonian theory can be used to describe the orbital motion of the stars and their tidal deformations. Indeed, the previous study [29] has focused on this inspiral stage and the possibility of using measurements of the tidal deformabilities to distinguish between NS binaries and MNS binaries. In this work we extend the inspiral analysis to NS-MNS binaries.…”

Section: Introductionmentioning

confidence: 99%

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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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Baryogenesis through asymmetric reheating in the mirror twin Higgs

Alonso-Álvarez,

Curtin,

Rasovic

et al. 2024

J. High Energ. Phys.

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We present the νϕMTH, a Mirror Twin Higgs (MTH) model realizing asymmetric reheating, baryogenesis and twin-baryogenesis through the out-of-equilibrium decay of a right-handed neutrino without any hard $${\mathbb{Z}}_{2}$$ breaking. The MTH is the simplest Neutral Naturalness solution to the little hierarchy problem and predicts the existence of a twin dark sector related to the Standard Model (SM) by a $${\mathbb{Z}}_{2}$$ symmetry that is only softly broken by a higher twin Higgs vacuum expectation value. The asymmetric reheating cools the twin sector compared to the visible one, thus evading cosmological bounds on ∆Neff. The addition of (twin-)colored scalars allows for the generation of the visible baryon asymmetry and, by the virtue of the $${\mathbb{Z}}_{2}$$ symmetry, also results in the generation of a twin baryon asymmetry. We identify a unique scenario with top-philic couplings for the new scalars that can satisfy all cosmological, proton decay and LHC constraints; yield the observed SM baryon asymmetry; and generate a wide range of possible twin baryon DM fractions, from negligible to unity. The viable regime of the theory contains several hints as to the possible structure of the Twin Higgs UV completion. Our results motivate the search for the rich cosmological and astrophysical signatures of twin baryons, and atomic dark matter more generally, at cosmological, galactic and stellar scales.

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Mirror neutron stars

Cited by 28 publications

References 165 publications

A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter

A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter

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

Baryogenesis through asymmetric reheating in the mirror twin Higgs

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