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arxiv: 2503.19691 · v4 · submitted 2025-03-25 · ✦ hep-ph · astro-ph.HE· nucl-th

Strongly Interacting Dark Matter admixed Neutron Stars

Yannick Dengler , Suchita Kulkarni , Axel Maas , Kevin Radl This is my paper

Pith reviewed 2026-05-22 22:42 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.HEnucl-th
keywords strongly interacting dark matterneutron starsequation of stateG2 gauge theorymixed starsdark matter accumulation
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0 comments X

The pith

Strongly interacting dark matter from a one-flavor G2 gauge theory can mix into neutron stars while staying consistent with observations.

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

The paper tests whether dark matter that interacts via a non-Abelian gauge force, modeled by a one-flavor G2 gauge theory with composite fermions, can accumulate inside neutron stars. It combines the resulting dark-matter equation of state with model-agnostic interpolations for ordinary nuclear matter and solves the structure equations for the mixed stars. The calculation shows that the dark-matter component produces changes in mass and radius similar to those from other dark-matter models and that the mixed configurations remain compatible with existing neutron-star mass and radius data inside the reported uncertainties. A reader would care because the work supplies the first concrete check of a first-principles non-Abelian dark-matter equation of state against astrophysical constraints rather than against collider data alone.

Core claim

Strongly-interacting dark matter described by a QCD-like one-flavor G2 gauge theory, which supports composite fermionic dark matter stabilized by Fermi pressure, has a similar impact on neutron stars as other model equations of state and can be accommodated by constraints from neutron star observations within our uncertainties.

What carries the argument

The first-principles equation of state derived from the one-flavor G2 gauge theory for the dark-matter component, which is added to ordinary-matter equations of state to compute the structure of mixed stars.

If this is right

  • Mixed neutron stars containing this dark matter produce mass-radius relations that overlap with those from other dark-matter models.
  • Current neutron-star observations do not exclude the presence of this strongly interacting dark matter within the uncertainties of the calculation.
  • The dark-matter component remains stable against gravitational collapse inside the star because of its Fermi pressure.

Where Pith is reading between the lines

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

  • Future higher-precision radius measurements could tighten the allowed dark-matter fraction in neutron stars for this model.
  • The same G2 equation of state could be tested against other compact objects such as white dwarfs if the density regime overlaps.
  • If the model survives tighter constraints, it would link a specific non-Abelian dark-matter candidate directly to astrophysical observables.

Load-bearing premise

The G2 gauge-theory equation of state for dark matter remains valid at the densities and temperatures reached inside neutron stars, and the ordinary-matter EOS interpolation accurately captures the relevant nuclear physics.

What would settle it

A precise mass-radius measurement for a neutron star that lies outside the range allowed by the mixed-star models with this G2 dark-matter equation of state would rule out the claim that such dark matter is accommodated within uncertainties.

read the original abstract

Dark matter may accumulate in neutron stars given its gravitational interaction and abundance. We investigate the influence of strongly-interacting dark matter, described by a QCD-like one-flavor $G_2$ gauge theory, on neutron stars. This choice allows to test, for the first time, a first-principles-determined non-Abelian dark matter equation of state, which supports composite fermionic dark matter and thus a Fermi-pressure-stabilized dark matter component. The ordinary matter part of the mixed star is described by available model-agnostic equations of state that interpolate between the low-density regime and high-density regime. We find that strongly-interacting dark matter has a similar impact on neutron stars as other model equation of states and confirm that strongly-interacting dark matter can be accommodated by constraints from neutron star observations within our uncertainties.

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 studies neutron stars containing a dark-matter component whose equation of state is taken from a first-principles lattice calculation in a one-flavor G2 gauge theory. Ordinary-matter equations of state are constructed via model-agnostic interpolations between low- and high-density regimes. The central claim is that the resulting mass-radius relations remain compatible with existing neutron-star observational constraints within the reported uncertainties and that the strongly-interacting DM produces effects qualitatively similar to those obtained with other model equations of state.

Significance. A first-principles, non-Abelian lattice EOS for composite fermionic dark matter is a genuine novelty in the neutron-star literature. If the zero-temperature, zero-chemical-potential G2 pressure-density relation can be shown to remain valid inside a ~2 M_⊙ star, the work would supply a concrete, falsifiable benchmark for strongly-interacting DM admixed compact objects. The present manuscript, however, does not supply that demonstration, so the quantitative compatibility statement rests on an unverified extrapolation.

major comments (2)
  1. [Methods / EOS construction (exact section number not visible in supplied text)] The manuscript states that the G2 lattice EOS is used directly for the DM component, yet provides no section demonstrating that the same functional form continues to hold at the baryon densities and gravitational potentials reached in the core of a 2 M_⊙ star (several times nuclear saturation density). The skeptic note correctly identifies this as the load-bearing assumption; without an explicit check or finite-temperature correction, the allowed DM-fraction window and the resulting mass-radius curves cannot be regarded as robust.
  2. [Results / uncertainty quantification] The abstract and conclusion assert compatibility “within our uncertainties,” but the uncertainty budget is not broken down into contributions from the G2 extrapolation, the ordinary-matter interpolation, and the observational constraints. Consequently it is impossible to judge whether the compatibility statement survives a plausible variation of the high-density G2 pressure.
minor comments (2)
  1. [Sec. 2] Notation for the DM fraction and the two-fluid Tolman-Oppenheimer-Volkoff equations should be introduced once in a dedicated subsection rather than inline.
  2. [Figures 3-5] Figure captions should explicitly state the range of DM fractions shown and whether the curves correspond to the central or extremal values of the ordinary-matter EOS band.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report. We address each major comment below and indicate the revisions we will make to the manuscript.

read point-by-point responses

  1. Referee: [Methods / EOS construction (exact section number not visible in supplied text)] The manuscript states that the G2 lattice EOS is used directly for the DM component, yet provides no section demonstrating that the same functional form continues to hold at the baryon densities and gravitational potentials reached in the core of a 2 M_⊙ star (several times nuclear saturation density). The skeptic note correctly identifies this as the load-bearing assumption; without an explicit check or finite-temperature correction, the allowed DM-fraction window and the resulting mass-radius curves cannot be regarded as robust.

    Authors: We agree that applying the zero-temperature, zero-chemical-potential G2 lattice EOS directly at the densities and gravitational potentials inside a ~2 M_⊙ neutron star constitutes a central assumption. The lattice calculation supplies the first-principles relation for composite fermionic DM, and we adopt it as a benchmark to explore qualitative effects on the mass-radius relation. An explicit demonstration of its validity under stellar conditions would require new lattice simulations at finite density, which lie outside the scope of the present work. We will revise the Methods section to expand the discussion of this assumption, its range of applicability, and the absence of finite-temperature corrections (justified by the cold DM component). revision: partial

  2. Referee: [Results / uncertainty quantification] The abstract and conclusion assert compatibility “within our uncertainties,” but the uncertainty budget is not broken down into contributions from the G2 extrapolation, the ordinary-matter interpolation, and the observational constraints. Consequently it is impossible to judge whether the compatibility statement survives a plausible variation of the high-density G2 pressure.

    Authors: We accept that a more transparent uncertainty budget is needed to support the compatibility statement. In the revised manuscript we will add an explicit breakdown in the Results section, separating contributions from (i) the model-agnostic ordinary-matter interpolations, (ii) the explored range of DM fractions, and (iii) the NICER and gravitational-wave observational constraints. For the G2 component we will clarify that the lattice EOS is used with its reported statistical errors while systematic uncertainties from the high-density extrapolation remain unquantified; this limitation will be stated explicitly so readers can assess robustness. revision: yes

Circularity Check

0 steps flagged

No significant circularity; EOS inputs external and results are direct numerical outcomes

full rationale

The derivation applies an externally sourced first-principles G2 lattice EOS for the DM component and model-agnostic interpolations for ordinary matter to the Tolman-Oppenheimer-Volkoff equations. No prediction is obtained by fitting a parameter to a subset of the target data and then re-using that parameter; no load-bearing step reduces to a self-citation whose content is itself unverified; and the compatibility statement is a computed comparison against external observational bounds rather than a definitional identity.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review supplies no explicit list of fitted parameters, background axioms, or new postulated entities; all such entries are therefore left empty.

pith-pipeline@v0.9.0 · 5672 in / 1122 out tokens · 31765 ms · 2026-05-22T22:42:11.058549+00:00 · methodology

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Reference graph

Works this paper leans on

99 extracted references · 99 canonical work pages · 45 internal anchors

  1. [1]

    V. C. Rubin, W. K. Ford, Jr. and N. Thonnard,Extended rotation curves of high-luminosity spiral galaxies. IV. Systematic dynamical properties, Sa through Sc,Astrophys. J. Lett.225 (1978) L107–L111

    work page 1978

  2. [2]

    Bambi and A

    C. Bambi and A. D. Dolgov,Introduction to Particle Cosmology. UNITEXT for Physics. Springer, 2015, 10.1007/978-3-662-48078-6

    work page doi:10.1007/978-3-662-48078-6 2015

  3. [3]

    Dark Matter

    M. Cirelli, A. Strumia and J. Zupan,Dark Matter,2406.01705

    work page internal anchor Pith review Pith/arXiv arXiv

  4. [4]

    D. N. Spergel and P. J. Steinhardt,Observational evidence for selfinteracting cold dark matter,Phys. Rev. Lett.84(2000) 3760–3763, [astro-ph/9909386]. – 19 – 1.0 1.5 2.0 Mtot [M ⊙ ] mC = 0.5GeV EoS I light EoS I heavy EoS II heavy EoS III light EoS III heavy 1.0 1.5 2.0 Mtot [M ⊙ ] mC = 1GeV 1.0 1.5 2.0 Mtot [M ⊙ ] mC = 2GeV 9 10 11 12 13 14 RO [km] 1.0 1...

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  5. [5]

    Dark Matter Halos as Particle Colliders: A Unified Solution to Small-Scale Structure Puzzles from Dwarfs to Clusters

    M. Kaplinghat, S. Tulin and H.-B. Yu,Dark Matter Halos as Particle Colliders: Unified Solution to Small-Scale Structure Puzzles from Dwarfs to Clusters,Phys. Rev. Lett.116 (2016) 041302, [1508.03339]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  6. [6]

    Dark Matter Self-interactions and Small Scale Structure

    S. Tulin and H.-B. Yu,Dark Matter Self-interactions and Small Scale Structure,Phys. Rept. 730(2018) 1–57, [1705.02358]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  7. [7]

    Sagunski, S

    L. Sagunski, S. Gad-Nasr, B. Colquhoun, A. Robertson and S. Tulin,Velocity-dependent Self-interacting Dark Matter from Groups and Clusters of Galaxies,JCAP01(2021) 024, [2006.12515]

    work page arXiv 2021

  8. [8]

    K. E. Andrade, J. Fuson, S. Gad-Nasr, D. Kong, Q. Minor, M. G. Roberts et al.,A stringent upper limit on dark matter self-interaction cross-section from cluster strong lensing,Mon. Not. Roy. Astron. Soc.510(2021) 54–81, [2012.06611]

    work page arXiv 2021

  9. [9]

    Eckert, S

    D. Eckert, S. Ettori, A. Robertson, R. Massey, E. Pointecouteau, D. Harvey et al., Constraints on dark matter self-interaction from the internal density profiles of X-COP – 20 – 0.05 0.10 0.15 0.20 MD [M ⊙ ] mC = 0.5GeV EoS I light EoS I heavy EoS II heavy EoS III light EoS III heavy 0.05 0.10 0.15 0.20 MD [M ⊙ ] mC = 1GeV 0.05 0.10 0.15 0.20 MD [M ⊙ ] mC...

    work page arXiv 2022

  10. [10]

    Bose et al.,Report of the Topical Group on Physics Beyond the Standard Model at Energy Frontier for Snowmass 2021,2209.13128

    T. Bose et al.,Report of the Topical Group on Physics Beyond the Standard Model at Energy Frontier for Snowmass 2021,2209.13128

    work page arXiv 2021

  11. [11]

    Adhikari et al.,Astrophysical Tests of Dark Matter Self-Interactions,2207.10638

    S. Adhikari et al.,Astrophysical Tests of Dark Matter Self-Interactions,2207.10638

    work page arXiv

  12. [12]

    The distribution of dark matter in galaxies

    P. Salucci,The distribution of dark matter in galaxies,Astron. Astrophys. Rev.27(2019) 2, [1811.08843]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  13. [13]

    B. Carr, K. Kohri, Y. Sendouda and J. Yokoyama,Constraints on primordial black holes, Rept. Prog. Phys.84(2021) 116902, [2002.12778]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  14. [14]

    The equation of state for nucleon matter and neutron star structure

    A. Akmal, V. R. Pandharipande and D. G. Ravenhall,The Equation of state of nucleon matter and neutron star structure,Phys. Rev. C58(1998) 1804–1828, [nucl-th/9804027]

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  15. [15]

    J. M. Lattimer and M. Prakash,Neutron star structure and the equation of state, Astrophys. J.550(2001) 426, [astro-ph/0002232]

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  16. [16]

    Masses, Radii, and Equation of State of Neutron Stars

    F. Özel and P. Freire,Masses, Radii, and the Equation of State of Neutron Stars,Ann. Rev. Astron. Astrophys.54(2016) 401–440, [1603.02698]. – 21 – 2 4 6 8 10 RD [km] mC = 0.5GeV EoS I light EoS I heavy EoS II heavy EoS III light EoS III heavy 2 3 4 5 6 RD [km] mC = 1GeV 1.4 1.6 1.8 2.0 2.2 RD [km] mC = 2GeV 8 10 12 14 16 RO [km] 0.40 0.45 0.50 0.55 0.60 R...

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  17. [17]

    On the capture of dark matter by neutron stars

    T. Güver, A. E. Erkoca, M. Hall Reno and I. Sarcevic,On the capture of dark matter by neutron stars,JCAP05(2014) 013, [1201.2400]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  18. [18]

    Giangrandi, V

    E. Giangrandi, V. Sagun, O. Ivanytskyi, C. Providência and T. Dietrich,The Effects of Self-interacting Bosonic Dark Matter on Neutron Star Properties,Astrophys. J.953(2023) 115, [2209.10905]

    work page arXiv 2023

  19. [19]

    Giangrandi, H

    E. Giangrandi, H. R. Rüter, N. Kunert, M. Emma, A. Abac, A. Adhikari et al.,Numerical Relativity Simulations of Dark Matter Admixed Binary Neutron Stars,2504.20825

    work page arXiv

  20. [20]

    Grippa, G

    F. Grippa, G. Lambiase and T. K. Poddar,Searching for New Physics in an Ultradense Environment: A Review on Dark Matter Admixed Neutron Stars,Universe11(2025) 74, [2412.09381]

    work page arXiv 2025

  21. [21]

    Del Popolo, M

    A. Del Popolo, M. Le Delliou and M. Deliyergiyev,Neutron Stars and Dark Matter, Universe6(2020) 222, [2410.06078]

    work page arXiv 2020

  22. [22]

    Gendreau, Z

    K. Gendreau, Z. Arzoumanian, E. Ferrara and C. B. Markwardt,NICER: The Neutron Star Interior Composition Explorer, pp. 1321–1341. Springer Nature Singapore, Singapore,

    work page

  23. [23]

    10.1007/978-981-19-6960-7_152. – 22 – 102 104 106 108 Λ mC = 0.5GeV EoS I light EoS I heavy EoS II heavy EoS III light EoS III heavy 102 104 106 108 Λ mC = 1GeV 102 104 106 108 Λ mC = 2GeV 0.5 1.0 1.5 2.0 2.5 Mtot [M ⊙ ] 102 104 106 108 Λ mC = 4GeV 0.5 1.0 1.5 2.0 2.5 Mtot [M ⊙ ] 0.5 1.0 1.5 2.0 2.5 Mtot [M ⊙ ] 0.5 1.0 1.5 2.0 2.5 Mtot [M ⊙ ] 0.5 1.0 1.5 ...

    work page doi:10.1007/978-981-19-6960-7_152

  24. [24]

    Search for Dark Matter Effects on Gravitational Signals from Neutron Star Mergers

    J. Ellis, A. Hektor, G. Hütsi, K. Kannike, L. Marzola, M. Raidal et al.,Search for Dark Matter Effects on Gravitational Signals from Neutron Star Mergers,Phys. Lett. B781 (2018) 607–610, [1710.05540]. [24]LIGO Scientific, Virgocollaboration, B. P. Abbott et al.,GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral,Phys. Rev. Let...

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  25. [25]

    Quantum chromodynamics on the lattice,

    C. Gattringer and C. B. Lang,Quantum chromodynamics on the lattice. Lect. Notes Phys., 2010, 10.1007/978-3-642-01850-3

    work page doi:10.1007/978-3-642-01850-3 2010

  26. [26]

    Friman, C

    B. Friman, C. Hohne, J. Knoll, S. Leupold, J. Randrup, R. Rapp et al., eds.,The CBM physics book: Compressed baryonic matter in laboratory experiments, vol. 814. 2011, 10.1007/978-3-642-13293-3

    work page doi:10.1007/978-3-642-13293-3 2011

  27. [27]

    Quddus, G

    A. Quddus, G. Panotopoulos, B. Kumar, S. Ahmad and S. K. Patra,GW170817 constraints on the properties of a neutron star in the presence of WIMP dark matter,J. Phys. G47 (2020) 095202, [1902.00929]

    work page arXiv 2020

  28. [28]

    Quddus, G

    A. Quddus, G. Panotopoulos, B. Kumar, S. Ahmad and S. K. Patra,GW170817 Constraints on Equations-of-states of a Neutron Star in the Presence of WIMP Dark Matter,JPS Conf. Proc.31(2020) 011053

    work page 2020

  29. [29]

    Biesdorf, J

    C. Biesdorf, J. Schaffner-Bielich and L. Tolos,Masquerading hybrid stars with dark matter, 2412.05207

    work page arXiv

  30. [30]

    Hajkarim, J

    F. Hajkarim, J. Schaffner-Bielich and L. Tolos,Thermodynamic Consistent Description of – 24 – Compact Stars of Two Interacting Fluids: The Case of Neutron Stars with Higgs Portal Dark Matter,2412.04585

    work page arXiv

  31. [31]

    Kunkel, S

    S. Kunkel, S. Wystub and J. Schaffner-Bielich,Determining proto-neutron stars’ minimal mass with chirally constrained nuclear equations of state,2411.14930

    work page arXiv

  32. [32]

    Wystub, Y

    S. Wystub, Y. Dengler, J.-E. Christian and J. Schaffner-Bielich,Constraining exotic compact stars composed of bosonic and fermionic dark matter with gravitational wave events,Mon. Not. Roy. Astron. Soc.521(2023) 1393–1398, [2110.12972]

    work page arXiv 2023

  33. [33]

    S. L. Pitz and J. Schaffner-Bielich,Generating ultra-compact neutron stars with bosonic dark matter,2408.13157

    work page arXiv

  34. [34]

    R. F. Diedrichs, N. Becker, C. Jockel, J.-E. Christian, L. Sagunski and J. Schaffner-Bielich, Tidal deformability of fermion-boson stars: Neutron stars admixed with ultralight dark matter,Phys. Rev. D108(2023) 064009, [2303.04089]

    work page arXiv 2023

  35. [35]

    Dengler, J

    Y. Dengler, J. Schaffner-Bielich and L. Tolos,Second Love number of dark compact planets and neutron stars with dark matter,Phys. Rev. D105(2022) 043013, [2111.06197]

    work page arXiv 2022

  36. [36]

    Tolos, J

    L. Tolos, J. Schaffner-Bielich and Y. Dengler,Dark Compact Planets,Phys. Rev. D92 (2015) 123002, [1507.08197]

    work page arXiv 2015

  37. [37]

    Quark stars admixed with dark matter

    P. Mukhopadhyay and J. Schaffner-Bielich,Quark stars admixed with dark matter,Phys. Rev. D93(2016) 083009, [1511.00238]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  38. [38]

    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(2017) 33, [1612.02804]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  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. D96(2017) 083004, [1709.06312]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  40. [40]

    Dark halos around neutron stars and gravitational waves

    A. Nelson, S. Reddy and D. Zhou,Dark halos around neutron stars and gravitational waves, JCAP07(2019) 012, [1803.03266]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  41. [41]

    Dark Matter Effects On Neutron Star Properties

    J. Ellis, G. Hütsi, K. Kannike, L. Marzola, M. Raidal and V. Vaskonen,Dark Matter Effects On Neutron Star Properties,Phys. Rev. D97(2018) 123007, [1804.01418]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  42. [42]

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

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  43. [43]

    Ivanytskyi, V

    O. Ivanytskyi, V. Sagun and I. Lopes,Neutron stars: New constraints on asymmetric dark matter,Phys. Rev. D102(2020) 063028, [1910.09925]

    work page arXiv 2020

  44. [44]

    D. R. Karkevandi, S. Shakeri, V. Sagun and O. Ivanytskyi,Bosonic dark matter in neutron stars and its effect on gravitational wave signal,Phys. Rev. D105(2022) 023001, [2109.03801]

    work page arXiv 2022

  45. [45]

    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(2021) 3354–3363, [2104.06141]

    work page arXiv 2021

  46. [46]

    Guha and D

    A. Guha and D. Sen,Feeble DM-SM interaction via new scalar and vector mediators in rotating neutron stars,JCAP09(2021) 027, [2106.10353]

    work page arXiv 2021

  47. [47]

    Possible Implications of Asymmetric Fermionic Dark Matter for Neutron Stars

    I. Goldman, R. N. Mohapatra, S. Nussinov, D. Rosenbaum and V. Teplitz,Possible Implications of Asymmetric Fermionic Dark Matter for Neutron Stars,Phys. Lett. B725 (2013) 200–207, [1305.6908]. – 25 –

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  48. [48]

    Effects of fermionic dark matter on properties of neutron stars

    Q.-F. Xiang, W.-Z. Jiang, D.-R. Zhang and R.-Y. Yang,Effects of fermionic dark matter on properties of neutron stars,Phys. Rev. C89(2014) 025803, [1305.7354]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  49. [49]

    A. Li, F. Huang and R.-X. Xu,Too massive neutron stars: The role of dark matter?, Astropart. Phys.37(2012) 70–74, [1208.3722]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  50. [50]

    Effects of mirror dark matter on neutron stars

    F. Sandin and P. Ciarcelluti,Effects of mirror dark matter on neutron stars,Astropart. Phys.32(2009) 278–284, [0809.2942]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  51. [51]

    S. C. Leung, M. C. Chu and L. M. Lin,Dark-matter admixed neutron stars,Phys. Rev. D 84(2011) 107301, [1111.1787]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  52. [52]

    S. C. Leung, M. C. Chu and L. M. Lin,Equilibrium Structure and Radial Oscillations of Dark Matter Admixed Neutron Stars,Phys. Rev. D85(2012) 103528, [1205.1909]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  53. [53]

    M. F. Barbat, J. Schaffner-Bielich and L. Tolos,Comprehensive study of compact stars with dark matter,Phys. Rev. D110(2024) 023013, [2404.12875]

    work page arXiv 2024

  54. [54]

    Hippert, J

    M. Hippert, J. Setford, H. Tan, D. Curtin, J. Noronha-Hostler and N. Yunes,Mirror neutron stars,Phys. Rev. D106(2022) 035025, [2103.01965]

    work page arXiv 2022

  55. [55]

    Issifu, P

    A. Issifu, P. Thakur, F. M. da Silva, K. D. Marquez, D. P. Menezes, M. Dutra et al., Supernova Remnants with Mirror Dark Matter and Hyperons,2412.17946

    work page arXiv

  56. [56]

    D. R. Karkevandi, M. Shahrbaf, S. Shakeri and S. Typel,Exploring the Distribution and Impact of Bosonic Dark Matter in Neutron Stars,Particles7(2024) 201–213, [2402.18696]

    work page arXiv 2024

  57. [57]

    Shakeri and D

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

    work page arXiv 2024

  58. [58]

    Y. Ema, R. McGehee, M. Pospelov and A. Ray,Dark matter catalyzed baryon destruction, Phys. Rev. D111(2025) 023005, [2405.18472]

    work page arXiv 2025

  59. [59]

    The SIMP Miracle

    Y. Hochberg, E. Kuflik, T. Volansky and J. G. Wacker,Mechanism for Thermal Relic Dark Matter of Strongly Interacting Massive Particles,Phys. Rev. Lett.113(2014) 171301, [1402.5143]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  60. [60]

    The SIMPlest Miracle

    Y. Hochberg, E. Kuflik, H. Murayama, T. Volansky and J. G. Wacker,Model for Thermal Relic Dark Matter of Strongly Interacting Massive Particles,Phys. Rev. Lett.115(2015) 021301, [1411.3727]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  61. [61]

    Kulkarni, A

    S. Kulkarni, A. Maas, S. Mee, M. Nikolic, J. Pradler and F. Zierler,Low-energy effective description of darkSp(4)theories,SciPost Phys.14(2023) 044, [2202.05191]

    work page arXiv 2023

  62. [62]

    Template Composite Dark Matter : SU(2) gauge theory with 2 fundamental flavours

    V. Drach, A. Hietanen, C. Pica, J. Rantaharju and F. Sannino,Template Composite Dark Matter:SU(2)gauge theory with 2 fundamental flavours,PoSLA TTICE2015(2016) 234, [1511.04370]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  63. [63]

    Towards the phase diagram of dense two-color matter

    S. Cotter, P. Giudice, S. Hands and J.-I. Skullerud,Towards the phase diagram of dense two-color matter,Phys.Rev.D87(2013) 034507, [1210.4496]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  64. [64]

    T. Boz, P. Giudice, S. Hands and J.-I. Skullerud,Dense two-color QCD towards continuum and chiral limits,Phys. Rev. D101(2020) 074506, [1912.10975]

    work page arXiv 2020

  65. [65]

    Hands, S

    S. Hands, S. Kim, D. Lawlor, A. Lee-Mitchell and J.-I. Skullerud,Dense QC2D. What’s up with that?!?, in41st International Symposium on Lattice Field Theory, 12, 2024. 2412.15872

    work page arXiv 2024

  66. [66]

    S. L. Liebling and C. Palenzuela,Dynamical boson stars,Living Rev. Rel.26(2023) 1, [1202.5809]. – 26 –

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  67. [67]

    Exceptional Confinement in G(2) Gauge Theory

    K. Holland, P. Minkowski, M. Pepe and U. J. Wiese,Exceptional confinement in G(2) gauge theory,Nucl. Phys.B668(2003) 207–236, [hep-lat/0302023]

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  68. [68]

    A. Maas, L. von Smekal, B. Wellegehausen and A. Wipf,The phase diagram of a gauge theory with fermionic baryons,Phys.Rev.D86(2012) 111901, [1203.5653]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  69. [69]

    B. H. Wellegehausen, A. Maas, A. Wipf and L. von Smekal,Hadron masses and baryonic scales inG 2-QCD at finite density,Phys. Rev. D89(2014) 056007, [1312.5579]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  70. [70]

    Constructing a neutron star in G2-QCD

    O. Hajizadeh and A. Maas,Constructing a neutron star from the lattice in G2-QCD,Eur. Phys. J. A53(2017) 207, [1702.08724]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  71. [71]

    J. B. Kogut, M. A. Stephanov, D. Toublan, J. J. M. Verbaarschot and A. Zhitnitsky,QCD - like theories at finite baryon density,Nucl. Phys. B582(2000) 477–513, [hep-ph/0001171]

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  72. [72]

    Constraining neutron star matter with QCD

    A. Kurkela, E. S. Fraga, J. Schaffner-Bielich and A. Vuorinen,Constraining neutron star matter with Quantum Chromodynamics,Astrophys. J.789(2014) 127, [1402.6618]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  73. [73]

    SIMP Spectroscopy

    Y. Hochberg, E. Kuflik and H. Murayama,SIMP Spectroscopy,JHEP05(2016) 090, [1512.07917]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  74. [74]

    Cosmology and Accelerator Tests of Strongly Interacting Dark Matter

    A. Berlin, N. Blinov, S. Gori, P. Schuster and N. Toro,Cosmology and Accelerator Tests of Strongly Interacting Dark Matter,Phys. Rev. D97(2018) 055033, [1801.05805]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  75. [75]

    Pomper and S

    J. Pomper and S. Kulkarni,Low energy effective theories of composite dark matter with real representations,2402.04176

    work page arXiv

  76. [76]

    Bernreuther, N

    E. Bernreuther, N. Hemme, F. Kahlhoefer and S. Kulkarni,Dark matter relic density in strongly interacting dark sectors with light vector mesons,Phys. Rev. D110(2024) 035009, [2311.17157]

    work page arXiv 2024

  77. [77]

    J. R. Oppenheimer and G. M. Volkoff,On massive neutron cores,Phys. Rev.55(1939) 374–381

    work page 1939

  78. [78]

    Mendes, J.-E

    M. Mendes, J.-E. Christian, F. J. Fattoyev and J. Schaffner-Bielich,Constraining twin stars with cold neutron star cooling data,Phys. Rev. D111(2025) 063007, [2408.05287]

    work page arXiv 2025

  79. [79]

    Christian, J

    J.-E. Christian, J. Schaffner-Bielich and S. Rosswog,Which first order phase transitions to quark matter are possible in neutron stars?,Phys. Rev. D109(2024) 063035, [2312.10148]

    work page arXiv 2024

  80. [80]

    Cold Quark Matter

    A. Kurkela, P. Romatschke and A. Vuorinen,Cold Quark Matter,Phys. Rev. D81(2010) 105021, [0912.1856]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

Showing first 80 references.