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arxiv: 2607.00888 · v1 · pith:DPUVYIZ7new · submitted 2026-07-01 · 🌌 astro-ph.HE

A self-consistent single-fluid framework for neutron stars admixed with mirror dark matter

Adamu Issifu , Constan\c{c}a Provid\^encia , Franciele M. da Silva , D\'ebora P. Menezes , Tobias Frederico This is my paper

Pith reviewed 2026-07-02 08:34 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords neutron starsdark mattermirror dark matterequation of statedirect Urca processcompact starsstellar cooling
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The pith

Mirror dark matter admixed with neutron stars softens the equation of state and lowers their maximum masses.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper introduces a self-consistent single-fluid model for neutron stars containing mirror dark matter, where the two sectors interact via a vector current-current coupling that links their chemical potentials. The dark matter fraction is held fixed globally while its local density follows the baryonic density. Calculations with several nuclear models show that this interaction reduces the incompressibility of matter, softens the overall equation of state, raises central densities, and decreases the maximum supported mass. The onset of the direct Urca cooling process moves to higher densities, altering when rapid cooling begins depending on the symmetry energy.

Core claim

We develop a self-consistent framework based on a contact vector current-current interaction that couples the chemical potentials of both sectors through mutual mean-field shifts, with the dark matter fraction F_D = N_D/N_B fixed as a global input parameter. This formulation provides a physically motivated alternative to fixed-density prescriptions, allowing the local DM density to follow the baryonic matter density throughout the stellar interior. As an application, we consider a mirror-DM scenario with exact symmetry between the dark and visible sectors and investigate NS matter using the NL3ωρ, FSU2R, NL3, and DDME2 equations of state. We find that the DM-BM interaction weakens the bindin

What carries the argument

Contact vector current-current interaction that couples the chemical potentials of dark matter and baryonic matter through mutual mean-field shifts, with fixed global DM fraction as input.

If this is right

  • Maximum masses of neutron stars decrease with increasing dark matter fraction.
  • Central densities and compactness of neutron stars increase.
  • The direct Urca process onset moves to higher stellar densities.
  • Rapid cooling onsets shift to more massive stars for stiff symmetry energy models and to less massive stars for soft symmetry energy models.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Mass-radius measurements from gravitational wave events could be reinterpreted to bound the dark matter fraction in neutron stars.
  • The model suggests that scatter in observed neutron star properties might partly arise from varying dark matter admixtures between individual stars.
  • Cooling curve data from isolated neutron stars offers a potential observational test independent of mass limits.

Load-bearing premise

The dark matter fraction is treated as a fixed global input parameter and mirror dark matter is assumed to have exact symmetry with the visible sector.

What would settle it

An observed neutron star mass exceeding the lowered maximum for any dark matter fraction allowed by the model, or cooling data showing rapid cooling onset at masses inconsistent with the predicted shift in direct Urca threshold.

Figures

Figures reproduced from arXiv: 2607.00888 by Adamu Issifu, Constan\c{c}a Provid\^encia, D\'ebora P. Menezes, Franciele M. da Silva, Tobias Frederico.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p009_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p010_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3 [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: shows the mass-radius relation for the three different EOS models studied in this work: NL3ωρ (blue), DDME2 (red), and FSU2R (green), without DM (solid line) and with 2% (dashed), 5% (dot-dash), and 10% (dotted) DM. In addition, the credibility regions for GW170817, HESS J1731−347, PSR J0740+6620, and PSR J0030+045 are also shown, as explained in the cap￾tion. As expected, we observe that the stiffest EOS … view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6 [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: displays the mean-field BM–DM interac￾tion term, L MF DB = αnBnD, which, upon substituting nD = FDnB, (see the discussion below eq. (27)), becomes L MF DB = αFDn 2 B. This expression shows that the BM–DM interaction is governed by the local baryon density, α, and FD (defined in eq. (25)). Consequently, although the interaction strength depends explicitly on nB and FD, its functional form is universal and i… view at source ↗
read the original abstract

We develop a self-consistent framework based on a contact vector current-current interaction that couples the chemical potentials of both sectors through mutual mean-field shifts, with the dark matter (DM) fraction $F_D = N_D/N_B$ fixed as a global input parameter. This formulation provides a physically motivated alternative to fixed-density prescriptions, allowing the local DM density to follow the baryonic matter (BM) density throughout the stellar interior. As an application, we consider a mirror-DM scenario with exact symmetry between the dark and visible sectors and investigate NS matter using the NL3$\omega\rho$, FSU2R, NL3, and DDME2 equations of state (EOSs). We find that the DM--BM interaction weakens the binding of dense matter, reduces its incompressibility, and softens the EOS. Consequently, DM increases the central density and compactness of NSs, lowers their maximum masses, and shifts the onset of the direct Urca process to higher stellar densities. As a consequence, the onset of rapid cooling is shifted to more massive stars for models with a stiff symmetry energy and to less massive stars for models with a soft symmetry energy, depending on the extra compactness that results from the DM admixture. These results demonstrate that mirror-DM admixtures modify both the microscopic composition and macroscopic structure of NSs, with potential implications for their thermal evolution and multimessenger observational signatures.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript develops a single-fluid framework for neutron stars admixed with mirror dark matter based on a contact vector current-current interaction that mutually shifts chemical potentials between baryonic and dark sectors, with the global DM fraction F_D = N_D/N_B imposed as a fixed input parameter. This allows local DM density to track baryonic density. For the NL3ωρ, FSU2R, NL3, and DDME2 RMF equations of state under exact mirror symmetry, the interaction is reported to weaken binding, reduce incompressibility, soften the EOS, raise central densities and compactness, lower maximum masses, and shift the direct Urca onset (to higher masses for stiff symmetry energy models and lower masses for soft ones).

Significance. If the framework holds, the approach supplies a density-following alternative to fixed-density DM prescriptions and yields testable implications for NS maximum masses and cooling curves across multiple EOS families, with potential relevance to multimessenger constraints. Explicit use of four distinct RMF models is a positive feature that allows qualitative trends to be checked for robustness.

major comments (2)
  1. [Framework description] Framework section (abstract and model description): the claim of self-consistency rests on the contact interaction shifting chemical potentials, yet F_D is introduced and held fixed as a global input rather than obtained by solving the coupled equilibrium conditions together with total particle-number conservation; this renders the reported EOS softening, central-density increase, M_max reduction, and Urca shift conditional on externally chosen F_D values.
  2. [Application to RMF EOS models] Results paragraphs for the four EOS models: the shifts in Urca onset and maximum mass are stated only qualitatively, with no tabulated values, no error estimates on the density or mass changes, and no explicit comparison of the interaction-modified EOS against the baseline case at the same F_D; this weakens the ability to judge the size of the reported effects.
minor comments (2)
  1. [Framework description] Notation for the vector coupling strength and the precise form of the mean-field shift in the chemical potentials should be written explicitly (ideally with an equation) rather than described only in words.
  2. [Framework description] The statement that local DM density 'follows' the baryonic density needs a short clarification of how the single-fluid ansatz enforces this while keeping the global ratio fixed.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comments. We address each major comment below.

read point-by-point responses

  1. Referee: Framework section (abstract and model description): the claim of self-consistency rests on the contact interaction shifting chemical potentials, yet F_D is introduced and held fixed as a global input parameter rather than obtained by solving the coupled equilibrium conditions together with total particle-number conservation; this renders the reported EOS softening, central-density increase, M_max reduction, and Urca shift conditional on externally chosen F_D values.

    Authors: We agree that F_D is imposed as a fixed global input parameter and that the quantitative results depend on the specific value chosen for it. The self-consistency of the framework refers to the local DM density being determined dynamically via the mutual mean-field shifts once F_D is specified, rather than being prescribed independently at each density. We will revise the text to make this distinction explicit and to emphasize that F_D functions as a model parameter analogous to those in other admixture studies. revision: yes

  2. Referee: Results paragraphs for the four EOS models: the shifts in Urca onset and maximum mass are stated only qualitatively, with no tabulated values, no error estimates on the density or mass changes, and no explicit comparison of the interaction-modified EOS against the baseline case at the same F_D; this weakens the ability to judge the size of the reported effects.

    Authors: We accept that the results section would benefit from quantitative presentation. In the revised manuscript we will include tables listing the changes in maximum mass, central density, and the stellar mass at direct Urca onset for each of the four RMF models, both with and without the DM interaction, evaluated at the same fixed F_D values. This will enable direct comparison to the baseline cases. revision: yes

Circularity Check

0 steps flagged

No significant circularity; framework treats F_D explicitly as input

full rationale

The paper states that F_D is fixed as a global input parameter and computes consequences for the EOS and stellar structure from the contact interaction and chosen RMF models (NL3ωρ, FSU2R, NL3, DDME2). No step reduces a claimed prediction to a fitted quantity by construction, nor does any load-bearing premise rest on self-citation chains or imported uniqueness theorems. The mean-field coupling of chemical potentials is defined independently of the fixed F_D, and results are presented as conditional on that parameter. This is a standard parametric study with no self-definitional or renaming circularity.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on treating the dark-matter fraction as a fixed global parameter and on assuming exact mirror symmetry between sectors; these choices are stated explicitly in the abstract.

free parameters (1)
  • F_D = N_D/N_B
    Fixed as a global input parameter that sets the overall dark-matter content.
axioms (1)
  • domain assumption Exact symmetry between dark and visible sectors
    Invoked when applying the framework to the mirror-DM scenario.

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discussion (0)

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Reference graph

Works this paper leans on

78 extracted references · 67 canonical work pages · 34 internal anchors

  1. [1]

    and FAPESP Thematic Grants (2023/13749-1 and 2024/17816-8). F.M.S. would like to thank CNPq for fi- nancial support under research project No. 403007/2024-0 and research fellowship No. 201145/2025-1. This work was partially supported by national funds from FCT (Funda¸ c˜ ao para a Ciˆ encia e a Tecnologia, I.P, Portu- gal) under project UID/04564/2025, id...

    work page doi:10.54499/uidb/04564/2025 2023

  2. [2]

    V. C. Rubin, W. K. Ford, Jr., and N. Thonnard, Rota- tional properties of 21 SC galaxies with a large range of luminosities and radii, from NGC 4605 (R=4kpc) to UGC 2885 (R=122kpc)., Astrophys. J.238, 471 (1980)

    1980

  3. [3]

    Bosma, 21-cm line studies of spiral galaxies

    A. Bosma, 21-cm line studies of spiral galaxies. II. The distribution and kinematics of neutral hydrogen in spiral galaxies of various morphological types., ApJ86, 1825 (1981)

    1981

  4. [4]

    A direct empirical proof of the existence of dark matter

    D. Clowe, M. Bradac, A. H. Gonzalez, M. Markevitch, S. W. Randall, C. Jones, and D. Zaritsky, A direct empir- 16 ical proof of the existence of dark matter, Astrophys. J. Lett.648, L109 (2006), arXiv:astro-ph/0608407

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  5. [5]

    Simulating the joint evolution of quasars, galaxies and their large-scale distribution

    V. Springelet al., Simulating the joint evolution of quasars, galaxies and their large-scale distribution, Nature435, 629 (2005), arXiv:astro-ph/0504097

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  6. [6]

    P. A. R. Adeet al.(Planck), Planck 2015 results. XIII. Cosmological parameters, Astron. Astrophys.594, A13 (2016), arXiv:1502.01589 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  7. [7]

    Totani, 20 GeV halo-like excess of the Galactic diffuse emission and implications for dark matter annihilation, JCAP11, 080, arXiv:2507.07209 [astro-ph.HE]

    T. Totani, 20 GeV halo-like excess of the Galactic diffuse emission and implications for dark matter annihilation, JCAP11, 080, arXiv:2507.07209 [astro-ph.HE]

    work page arXiv

  8. [8]

    Profumo, Dark baryon black holes, Phys

    S. Profumo, Dark baryon black holes, Phys. Rev. D111, 095010 (2025), arXiv:2502.16439 [hep-ph]

    work page arXiv 2025

  9. [9]

    Dark Matter Search Results from a One Tonne$\times$Year Exposure of XENON1T

    E. Aprileet al.(XENON), Dark Matter Search Results from a One Ton-Year Exposure of XENON1T, Phys. Rev. Lett.121, 111302 (2018), arXiv:1805.12562 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  10. [10]

    Aprileet al.(XENON), WIMP Dark Matter Search Using a 3.1 Tonne-Year Exposure of the XENONnT Experiment, Phys

    E. Aprileet al.(XENON), WIMP Dark Matter Search Using a 3.1 Tonne-Year Exposure of the XENONnT Experiment, Phys. Rev. Lett.135, 221003 (2025), arXiv:2502.18005 [hep-ex]

    work page arXiv 2025

  11. [11]

    Dark Matter Search Results from 4.2 Tonne-Years of Exposure of the LUX-ZEPLIN (LZ) Experiment

    J. Aalberset al.(LZ), Dark Matter Search Results from 4.2 Tonne-Years of Exposure of the LUX-ZEPLIN (LZ) Experiment, Phys. Rev. Lett.135, 011802 (2025), arXiv:2410.17036 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  12. [12]

    Boet al.(PandaX), Dark Matter Search Results from 1.54 Tonne·Year Exposure of PandaX-4T, Phys

    Z. Boet al.(PandaX), Dark Matter Search Results from 1.54 Tonne·Year Exposure of PandaX-4T, Phys. Rev. Lett. 134, 011805 (2025), arXiv:2408.00664 [hep-ex]

    work page arXiv 2025

  13. [13]

    WIMP Annihilation and Cooling of Neutron Stars

    C. Kouvaris, WIMP Annihilation and Cooling of Neutron Stars, Phys. Rev. D77, 023006 (2008), arXiv:0708.2362 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  14. [14]

    Issifu, P

    A. Issifu, P. Thakur, F. M. da Silva, K. D. Marquez, D. P. Menezes, M. Dutra, O. Louren¸ co, and T. Frederico, Supernova remnants with mirror dark matter and hyper- ons, Phys. Rev. D111, 083026 (2025), arXiv:2412.17946 [hep-ph]

    work page arXiv 2025

  15. [15]

    L. L. Lopes and A. Issifu, XTE J1814-338 as a dark mat- ter admixed neutron star, Phys. Dark Univ.48, 101922 (2025), arXiv:2411.17105 [astro-ph.HE]

    work page arXiv 2025

  16. [16]

    Neutron Stars as Dark Matter Probes

    A. de Lavallaz and M. Fairbairn, Neutron Stars as Dark Matter Probes, Phys. Rev. D81, 123521 (2010), arXiv:1004.0629 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  17. [17]

    Can Neutron stars constrain Dark Matter?

    C. Kouvaris and P. Tinyakov, Can Neutron stars con- strain Dark Matter?, Phys. Rev. D82, 063531 (2010), arXiv:1004.0586 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  18. [18]

    Particle Dark Matter: Evidence, Candidates and Constraints

    G. Bertone, D. Hooper, and J. Silk, Particle dark matter: Evidence, candidates and constraints, Phys. Rept.405, 279 (2005), arXiv:hep-ph/0404175

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  19. [19]

    Shakeri and D

    S. Shakeri and D. R. Karkevandi, Bosonic dark matter in light of the NICER precise mass-radius measurements, Phys. Rev. D109, 043029 (2024), arXiv:2210.17308 [astro- ph.HE]

    work page arXiv 2024

  20. [20]

    A. Das, T. Malik, and A. C. Nayak, Dark matter admixed neutron star properties in light of gravitational wave observations: A two fluid approach, Phys. Rev. D105, 123034 (2022), arXiv:2011.01318 [nucl-th]

    work page arXiv 2022

  21. [21]

    Issifu, P

    A. Issifu, P. Thakur, D. R. Karkevandi, F. M. da Silva, D. P. Menezes, Y. Lim, and T. Frederico, Dark matter heating in evolving protoneutron stars: A two-fluid ap- proach, Phys. Rev. D113, 103042 (2026)

    2026

  22. [22]

    Thakur, T

    P. Thakur, T. Malik, A. Das, T. K. Jha, and C. Providˆ encia, Exploring robust correlations between fermionic dark matter model parameters and neutron star properties: A two-fluid perspective, Phys. Rev. D109, 043030 (2024), arXiv:2308.00650 [hep-ph]

    work page arXiv 2024

  23. [23]

    D. R. Karkevandi, S. Shakeri, V. Sagun, and O. Ivanyt- skyi, Bosonic dark matter in neutron stars and its effect on gravitational wave signal, Phys. Rev. D105, 023001 (2022), arXiv:2109.03801 [astro-ph.HE]

    work page arXiv 2022

  24. [24]

    Issifu, A

    A. Issifu, A. Konstantinou, P. Thakur, and T. Frederico, Rotating protoneutron star admixed with mirror dark matter: A two-fluid approach, Phys. Rev. D112, 103026 (2025), arXiv:2507.20823 [astro-ph.HE]

    work page arXiv 2025

  25. [25]

    Kain, Dark matter admixed neutron stars, Phys

    B. Kain, Dark matter admixed neutron stars, Phys. Rev. D103, 043009 (2021), arXiv:2102.08257 [gr-qc]

    work page arXiv 2021

  26. [26]

    Biesdorf, J

    C. Biesdorf, J. Schaffner-Bielich, and L. Tolos, Masquerad- ing hybrid stars with dark matter, Phys. Rev. D111, 083038 (2025), arXiv:2412.05207 [hep-ph]

    work page arXiv 2025

  27. [27]

    Study of Dark-Matter Admixed Neutron Stars using the Equation of State from the Rotational Curves of Galaxies

    Z. Rezaei, Study of Dark-Matter Admixed Neutron Stars using the Equation of State from the Rotational Curves of Galaxies, Astrophys. J.835, 33 (2017), arXiv:1612.02804 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  28. [28]

    Dark Matter Thermalization in Neutron Stars

    B. Bertoni, A. E. Nelson, and S. Reddy, Dark Matter Thermalization in Neutron Stars, Phys. Rev. D88, 123505 (2013), arXiv:1309.1721 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  29. [29]

    Bounds on self-interacting fermion dark matter from observations of old neutron stars

    J. Bramante, K. Fukushima, J. Kumar, and E. Stopnitzky, Bounds on self-interacting fermion dark matter from ob- servations of old neutron stars, Phys. Rev. D89, 015010 (2014), arXiv:1310.3509 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  30. [30]

    A. Das, T. Malik, and A. C. Nayak, Confronting nuclear equation of state in the presence of dark matter using GW170817 observation in relativistic mean field theory ap- proach, Phys. Rev. D99, 043016 (2019), arXiv:1807.10013 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  31. [31]

    Issifu, D

    A. Issifu, D. P. Menezes, and T. Frederico, Proto-neutron stars with dark matter admixture: A single-fluid approach, Phys. Dark Univ.50, 102149 (2025), arXiv:2506.21378 [astro-ph.HE]

    work page arXiv 2025

  32. [32]

    H. C. Das, A. Kumar, B. Kumar, S. Kumar Biswal, T. Nakatsukasa, A. Li, and S. K. Patra, Effects of dark matter on the nuclear and neutron star matter, Mon. Not. Roy. Astron. Soc.495, 4893 (2020), arXiv:2002.00594 [nucl-th]

    work page arXiv 2020

  33. [33]

    M. I. Gresham and K. M. Zurek, Asymmetric Dark Stars and Neutron Star Stability, Phys. Rev. D99, 083008 (2019), arXiv:1809.08254 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  34. [34]

    Sahoo, S

    R. Sahoo, S. Mukhopadhyay, and M. Bhuyan, Dark matter admixed white dwarfs: A single-fluid approach, Phys. Rev. D113, 123005 (2026), arXiv:2511.17120 [astro-ph.SR]

    work page arXiv 2026

  35. [35]

    New Analysis of Neutron Star Constraints on Asymmetric Dark Matter

    R. Garani, Y. Genolini, and T. Hambye, New analysis of neutron star constraints on asymmetric dark matter, JCAP2019, 035 (2019), arXiv:1812.08773 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  36. [36]

    Bramante and N

    J. Bramante and N. Raj, Dark matter in compact stars, Phys. Rept.1052, 1 (2024), arXiv:2307.14435 [hep-ph]

    work page arXiv 2024

  37. [37]

    Sen and A

    D. Sen and A. Guha, Implications of feebly interacting dark sector on neutron star properties and constraints from GW170817, Mon. Not. Roy. Astron. Soc.504, 3354 (2021), arXiv:2104.06141 [hep-ph]

    work page arXiv 2021

  38. [38]

    Constraining the mass of fermionic dark matter from its feeble interaction with hadronic matter via dark mediators in neutron stars,

    A. Guha and D. Sen, Constraining the mass of fermionic dark matter from its feeble interaction with hadronic matter via dark mediators in neutron stars, Phys. Rev. D109, 043038 (2024), arXiv:2401.14419 [astro-ph.HE]

    work page arXiv 2024

  39. [39]

    The dark matter effect on realistic equation of state in neutron stars

    G. Panotopoulos and I. Lopes, Dark matter effect on realistic equation of state in neutron stars, Phys. Rev. D 96, 083004 (2017), arXiv:1709.06312 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  40. [40]

    Compact stars made of fermionic dark matter

    G. Narain, J. Schaffner-Bielich, and I. N. Mishustin, Com- pact stars made of fermionic dark matter, Phys. Rev. D 74, 063003 (2006), arXiv:astro-ph/0605724

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  41. [41]

    T. F. Motta, P. A. M. Guichon, and A. W. Thomas, Neutron to Dark Matter Decay in Neutron Stars, Int. J. Mod. Phys. A33, 1844020 (2018), arXiv:1806.00903 17 [nucl-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  42. [42]

    G. Baym, D. H. Beck, P. Geltenbort, and J. Shelton, Testing dark decays of baryons in neutron stars, Phys. Rev. Lett.121, 061801 (2018), arXiv:1802.08282 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  43. [43]

    Husain, T

    W. Husain, T. F. Motta, and A. W. Thomas, Conse- quences of neutron decay inside neutron stars, JCAP 2022, 028 (2022), arXiv:2203.02758 [hep-ph]

    work page arXiv 2022

  44. [44]

    N. F. Bell, G. Busoni, S. Robles, and M. Virgato, Ther- malization and annihilation of dark matter in neutron stars, JCAP2024, 006 (2024), arXiv:2312.11892 [hep-ph]

    work page arXiv 2024

  45. [45]

    J. M. Berryman, S. Gardner, and M. Zakeri, How macro- scopic limits on neutron-star baryon loss yield microscopic limits on non-standard-model baryon decay, Phys. Rev. D109, 023021 (2024), arXiv:2305.13377 [hep-ph]

    work page arXiv 2024

  46. [46]

    Garani, A

    R. Garani, A. Gupta, and N. Raj, Observing the ther- malization of dark matter in neutron stars, Phys. Rev. D 103, 043019 (2021), arXiv:2009.10728 [hep-ph]

    work page arXiv 2021

  47. [47]

    Cosmological and Particle Physics Constraints on a New Non-Abelian SU(3) Gauge Model for Ordinary/Dark Matter Interaction

    O. Oliveira, C. A. Bertulani, M. S. Hussein, W. de Paula, and T. Frederico, Cosmological and Particle Physics Con- straints on a New Non-Abelian SU(3) Gauge Model for Ordinary/Dark Matter Interaction, Braz. J. Phys.46, 721 (2016), arXiv:1508.01049 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  48. [48]

    Aprileet al.(XENON), First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment, Phys

    E. Aprileet al.(XENON), First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment, Phys. Rev. Lett.131, 041003 (2023), arXiv:2303.14729 [hep-ex]

    work page arXiv 2023

  49. [49]

    A. H. Abdelhameedet al.(CRESST), First results from the CRESST-III low-mass dark matter program, Phys. Rev. D100, 102002 (2019), arXiv:1904.00498 [astro- ph.CO]

    work page arXiv 2019

  50. [50]

    First results on low-mass dark matter from the CRESST-III experiment

    F. Petriccaet al.(CRESST), First results on low-mass dark matter from the CRESST-III experiment, J. Phys. Conf. Ser.1342, 012076 (2020), arXiv:1711.07692 [astro- ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  51. [51]

    Agneseet al.(SuperCDMS), Search for Low-Mass Dark Matter with CDMSlite Using a Profile Likelihood Fit, Phys

    R. Agneseet al.(SuperCDMS), Search for Low-Mass Dark Matter with CDMSlite Using a Profile Likelihood Fit, Phys. Rev. D99, 062001 (2019), arXiv:1808.09098 [astro-ph.CO]

    work page arXiv 2019

  52. [52]

    Results from the Super Cryogenic Dark Matter Search (SuperCDMS) experiment at Soudan

    R. Agneseet al.(SuperCDMS), Results from the Super Cryogenic Dark Matter Search Experiment at Soudan, Phys. Rev. Lett.120, 061802 (2018), arXiv:1708.08869 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  53. [53]

    Low-Mass Dark Matter Search with CDMSlite

    R. Agneseet al.(SuperCDMS), Low-mass dark matter search with CDMSlite, Phys. Rev. D97, 022002 (2018), arXiv:1707.01632 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  54. [54]

    Interplay between the symmetry energy and the strangeness content of neutron stars

    C. Providencia and A. Rabhi, Interplay between the sym- metry energy and the strangeness content of neutron stars, Phys. Rev. C87, 055801 (2013), arXiv:1212.5911 [nucl-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  55. [55]

    Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints

    L. Tolos, M. Centelles, and A. Ramos, Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints, Astrophys. J.834, 3 (2017), arXiv:1610.00919 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  56. [56]

    The Equation of State for the Nucleonic and Hyperonic Core of Neutron Stars

    L. Tolos, M. Centelles, and A. Ramos, The Equation of State for the Nucleonic and Hyperonic Core of Neu- tron Stars, Publ. Astron. Soc. Austral.34, e065 (2017), arXiv:1708.08681 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  57. [57]

    C. J. Horowitz and J. Piekarewicz, Neutron star structure and the neutron radius of Pb-208, Phys. Rev. Lett.86, 5647 (2001), arXiv:astro-ph/0010227

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  58. [58]

    G. A. Lalazissis, T. Nikˇ si´ c, D. Vretenar, and P. Ring, New relativistic mean-field interaction with density-dependent meson-nucleon couplings, Phys. Rev. C71, 024312 (2005)

    2005

  59. [59]

    D. P. Menezes, A Neutron Star Is Born, Universe7, 267 (2021), arXiv:2106.09515 [astro-ph.HE]

    work page arXiv 2021

  60. [60]

    Typel and H

    S. Typel and H. H. Wolter, Relativistic mean field calcu- lations with density dependent meson nucleon coupling, Nucl. Phys. A656, 331 (1999)

    1999

  61. [61]

    Density Dependent Hadron Field Theory

    C. Fuchs, H. Lenske, and H. H. Wolter, Density depen- dent hadron field theory, Phys. Rev. C52, 3043 (1995), arXiv:nucl-th/9507044

    work page internal anchor Pith review Pith/arXiv arXiv 1995

  62. [62]

    Sedrakian and A

    A. Sedrakian and A. Harutyunyan, Delta-resonances and hyperons in proto-neutron stars and merger remnants, Eur. Phys. J. A58, 137 (2022), arXiv:2202.12083 [nucl- th]

    work page arXiv 2022

  63. [63]

    Hajkarim, J

    F. Hajkarim, J. Schaffner-Bielich, and L. Tolos, Thermody- namic consistent description of compact stars of two inter- acting fluids: the case of neutron stars with Higgs portal dark matter, JCAP2025, 070 (2025), arXiv:2412.04585 [hep-ph]

    work page arXiv 2025

  64. [64]

    Glendenning,Compact Stars: Nuclear Physics, Parti- cle Physics and General Relativity, Astronomy and Astro- physics Library (Springer New York, 2012)

    N. Glendenning,Compact Stars: Nuclear Physics, Parti- cle Physics and General Relativity, Astronomy and Astro- physics Library (Springer New York, 2012)

    2012

  65. [65]

    N. M. Hugenholtz and L. van Hove, A theorem on the single particle energy in a Fermi gas with interaction, Physica24, 363 (1958)

    1958

  66. [66]

    S. S. Avancini, M. E. Bracco, M. Chiapparini, and D. P. Menezes, On the density dependent hadron field theory at finite temperature and its thermodynamical consistency, J. Phys. G30, 27 (2004), arXiv:nucl-th/0311019

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  67. [67]

    J. M. Lattimer, M. Prakash, C. J. Pethick, and P. Haensel, Direct URCA process in neutron stars, Phys. Rev. Lett. 66, 2701 (1991)

    1991

  68. [68]

    Neutron star radii and crusts: uncertainties and unified equations of state

    M. Fortin, C. Providencia, A. R. Raduta, F. Gulminelli, J. L. Zdunik, P. Haensel, and M. Bejger, Neutron star radii and crusts: uncertainties and unified equations of state, Phys. Rev. C94, 035804 (2016), arXiv:1604.01944 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  69. [69]

    Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions

    T. Klahnet al., Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions, Phys. Rev. C74, 035802 (2006), arXiv:nucl-th/0602038

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  70. [70]

    D. Page, J. M. Lattimer, M. Prakash, and A. W. Steiner, Minimal cooling of neutron stars: A New paradigm, Astro- phys. J. Suppl.155, 623 (2004), arXiv:astro-ph/0403657

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  71. [71]

    D. Page, U. Geppert, and F. Weber, The Cooling of compact stars, Nucl. Phys. A777, 497 (2006), arXiv:astro- ph/0508056

    work page arXiv 2006

  72. [72]

    B. P. Abbott, R. Abbott, T. D. Abbott, S. Abraham, F. Acernese,et al., GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs, Phys. Rev. X9, 031040 (2019)

    2019

  73. [73]

    Doroshenko, V

    V. Doroshenko, V. Suleimanov, G. P¨ uhlhofer, and A. San- tangelo, A strangely light neutron star within a supernova remnant, Nature Astronomy6, 1444 (2022)

    2022

  74. [74]

    M. C. Miller, F. K. Lamb, A. J. Dittmann,et al., The Radius of PSR J0740+6620 from NICER and XMM- Newton Data, Astrophys. J. Lett.918, L28 (2021)

    2021

  75. [75]

    T. E. Riley, A. L. Watts, P. S. Ray,et al., A nicer view of the massive pulsar psr j0740+6620 informed by radio tim- ing and xmm-newton spectroscopy, Astrophysical Journal Letters918, L27 (2021), arXiv:2105.06979 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  76. [77]

    T. E. Riley, A. L. Watts, S. Bogdanov,et al., A nicer view of psr j0030+0451: Millisecond pulsar parameter estimation, Astrophysical Journal Letters887, L21 (2019), 18 arXiv:1912.05705 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  77. [78]

    Louren¸ co, T

    O. Louren¸ co, T. Frederico, and M. Dutra, Dark matter component in hadronic models with short-range correla- tions, Phys. Rev. D105, 023008 (2022), arXiv:2112.07716 [nucl-th]

    work page arXiv 2022

  78. [79]

    R-modes as a new probe of dark matter in neutron stars,

    S. Shirke, S. Ghosh, D. Chatterjee, L. Sagunski, and J. Schaffner-Bielich, R-modes as a new probe of dark matter in neutron stars, JCAP2023, 008 (2023), arXiv:2305.05664 [astro-ph.HE]

    work page arXiv 2023