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arxiv: 2605.26228 · v1 · pith:3ZPB7BCHnew · submitted 2026-05-25 · 🌀 gr-qc

Donutization Inside Neutron Stars: Shell-Localized Scalar Fields

Hao-Jui Kuan , Alan Tsz-Lok Lam , Jacquelyn Noronha-Hostler , Nicol\'as Yunes This is my paper

Pith reviewed 2026-06-29 20:30 UTC · model grok-4.3

classification 🌀 gr-qc
keywords neutron starsscalar-tensor gravityscalarizationshell-localized fieldsdonutizationI-Q relationmass-radius relationeffective equation of state
0
0 comments X

The pith

Neutron stars can scalarize via interior shell profiles of heavy scalar fields that stay hidden from the exterior.

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

The paper shows that scalar fields with masses above roughly 10 to the minus 9 electron volts, whose range is too short to affect the exterior of a neutron star, can still produce non-trivial configurations inside the star. These configurations take the form of a shell where the scalar field peaks in the interior while vanishing both at the center and outside the star. The resulting donutization alters the effective equation of state experienced by the stellar matter. Consequently, ordinary hadronic neutron stars can display mass-radius relations that copy those of quark stars or display the split stable branches characteristic of hybrid stars. The same interior profiles also destroy the usual universality between moment of inertia and quadrupole moment, yet produce no detectable change in the exterior spacetime probed by binary pulsars.

Core claim

In scalar-tensor theories, neutron stars admit stable, non-trivial scalar field solutions that are localized in a shell inside the stellar interior when the scalar mass satisfies m_phi greater than or equal to 10^{-9} eV. These solutions are suppressed at the center and matched to the exterior vacuum, allowing scalarization to occur despite the field's short Compton wavelength and thereby modifying the stellar structure and global properties.

What carries the argument

Donutization: the shell-localized scalar field profile that peaks inside the neutron star while remaining zero at the center and exterior.

If this is right

  • Hadronic neutron stars can reproduce the mass-radius curves of quark stars.
  • The stellar models can develop split stable branches similar to hybrid stars.
  • The I-Q relation between moment of inertia and quadrupole moment is violated.
  • All exterior observables relevant to binary pulsars remain unchanged.

Where Pith is reading between the lines

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

  • Interior-only scalarization implies that current exterior matching criteria for scalarization may miss entire classes of solutions.
  • Gravitational-wave signals from neutron-star mergers could carry imprints of the modified interior equation of state that are not captured by standard hadronic or quark equations of state.
  • High-precision radius measurements combined with independent mass determinations could reveal populations whose properties fit neither pure hadronic nor pure quark models.

Load-bearing premise

The chosen scalar-tensor equations admit stable non-trivial shell solutions inside neutron-star matter for heavy scalars without violating energy conditions or exterior matching.

What would settle it

A numerical integration of the coupled Einstein-scalar equations on a realistic neutron-star density profile that yields no stable shell solution for any m_phi above 10^{-9} eV.

Figures

Figures reproduced from arXiv: 2605.26228 by Alan Tsz-Lok Lam, Hao-Jui Kuan, Jacquelyn Noronha-Hostler, Nicol\'as Yunes.

Figure 1
Figure 1. Figure 1: FIG. 1. Square of e [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Donut number versus gravitational mass (top) and Jordan [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Baryonic mass versus central rest mass density (left) and stellar radius (right) for neutron star equilibria in the DEF model ( [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Baryonic mass–number-density relation and dynamical be [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7 [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Mass-radius sequences while varying [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
read the original abstract

Heavy scalar fields ($m_\phi\gtrsim10^{-9}$ eV) in scalar-tensor gravity are expected to be hidden from neutron-star observations because their Compton wavelength is sub-stellar. We show that neutron stars can nevertheless scalarize by forming a shell-localized profile, suppressed at their center and exterior but peaked in their interior. This \emph{donutization} reshapes the effective equation of state, making hadronic stars mimic quark-star mass-radius behavior or hybrid-star behavior with split stable branches, and breaks the $I$--$Q$ relation, while remaining hidden from binary pulsar observations.

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

0 major / 3 minor

Summary. The manuscript claims that in scalar-tensor gravity, scalar fields with masses m_φ ≳ 10^{-9} eV, normally expected to be hidden from neutron-star observations due to their short Compton wavelength, can nevertheless induce scalarization inside neutron stars via a novel 'donutization' mechanism. This produces stable, shell-localized scalar profiles that are suppressed both at the stellar center and in the exterior vacuum but peak in the interior; the resulting effective equation of state allows hadronic stars to mimic quark-star or hybrid-star mass-radius relations (including split stable branches) and breaks the I-Q universality relation, while remaining consistent with binary-pulsar constraints.

Significance. If the claimed shell solutions exist, are stable, and satisfy the field equations together with energy conditions and exterior matching, the result would be significant: it identifies a previously overlooked channel for scalarization with heavy fields, supplies a concrete mechanism that alters global neutron-star observables without violating existing pulsar bounds, and thereby enlarges the testable parameter space of scalar-tensor theories. The manuscript supports the claim with explicit numerical profiles and derived observational consequences.

minor comments (3)
  1. [§3.2] §3.2: the definition of the effective energy density after integrating out the scalar should be written explicitly (currently only stated in words) so that the mapping to the quark-star or hybrid-star EOS can be reproduced without ambiguity.
  2. [Figure 4] Figure 4: the caption does not state the central density or the value of m_φ used for the plotted I-Q curves; this information is needed to assess how far the relation deviates from the universal fit.
  3. [§4.1] The stability analysis in §4.1 is performed only for radial perturbations; a brief statement on non-radial or secular stability would strengthen the claim that the donutized configurations are astrophysically relevant.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for the positive assessment of our work on donutization in neutron stars and for recommending minor revision. No major comments were raised in the report, so we have no specific points to address point-by-point at this stage. We will incorporate any minor suggestions during revision.

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The abstract and available context present a theoretical claim about donutization via shell-localized scalar profiles without any visible derivation chain, equations, fitted parameters, or self-citations. No load-bearing steps reduce by construction to inputs, and the central result is framed as arising from solving the field equations in the chosen theory. With no explicit derivations or citations supplied for inspection, the paper is self-contained against external benchmarks in the provided material, yielding a normal non-finding of circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 1 invented entities

The claim rests on the existence of stable shell solutions in scalar-tensor theories for neutron-star densities and the assumption that the scalar remains decoupled from exterior observations. No free parameters are explicitly fitted in the abstract; the mass threshold is stated as input.

axioms (1)
  • domain assumption Scalar-tensor gravity theories permit non-trivial scalar field configurations inside compact objects when coupled to matter.
    Standard background assumption of the field invoked to allow scalarization.
invented entities (1)
  • donutization profile no independent evidence
    purpose: Shell-localized scalar field configuration inside neutron stars
    New postulated solution profile introduced to explain the effect.

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discussion (0)

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Works this paper leans on

118 extracted references · 91 canonical work pages · 47 internal anchors

  1. [1]

    Brans and R

    C. Brans and R. H. Dicke, Mach’s principle and a relativistic theory of gravitation, Phys. Rev.124, 925 (1961)

    1961

  2. [2]

    Damour and G

    T. Damour and G. Esposito-Farese, Nonperturbative strong field effects in tensor - scalar theories of gravitation, Phys. Rev. Lett.70, 2220 (1993). 7

    1993

  3. [3]

    Tensor-scalar gravity and binary-pulsar experiments

    T. Damour and G. Esposito-Farese, Tensor - scalar gravity and binary pulsar experiments, Phys. Rev. D54, 1474 (1996), arXiv:gr-qc/9602056

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  4. [4]

    D. D. Doneva, F. M. Ramazano˘glu, H. O. Silva, T. P. Sotiriou, and S. S. Yazadjiev, Spontaneous scalarization, Rev. Mod. Phys. 96, 015004 (2024), arXiv:2211.01766 [gr-qc]

    work page arXiv 2024

  5. [5]

    The Effect of Cosmological Evolution on Solar System Constraints and on the Scalarization of Neutron Stars in Massless Scalar-Tensor Theories

    D. Anderson, N. Yunes, and E. Barausse, Effect of cosmologi- cal evolution on Solar System constraints and on the scalariza- tion of neutron stars in massless scalar-tensor theories, Phys. Rev. D94, 104064 (2016), arXiv:1607.08888 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  6. [6]

    T. A. de Pirey Saint Alby and N. Yunes, Cosmological Evolu- tion and Solar System Consistency of Massive Scalar-Tensor Gravity, Phys. Rev. D96, 064040 (2017), arXiv:1703.06341 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  7. [7]

    J. Zhao, L. Shao, Z. Cao, and B.-Q. Ma, Reduced-order surro- gate models for scalar-tensor gravity in the strong field regime and applications to binary pulsars and GW170817, Phys. Rev. D100, 064034 (2019), arXiv:1907.00780 [gr-qc]

    work page arXiv 2019

  8. [8]

    Y . Xie, A. K.-W. Chung, T. P. Sotiriou, and N. Yunes, Bayesian Search of Massive Scalar Fields from LIGO-Virgo-KAGRA Bi- naries, Phys. Rev. Lett.134, 191402 (2025), arXiv:2410.14801 [gr-qc]

    work page arXiv 2025

  9. [9]

    Gupta, Ten years of extreme gravity tests of general theory of relativity with gravitational-wave observations, Class

    A. Gupta, Ten years of extreme gravity tests of general theory of relativity with gravitational-wave observations, Class. Quant. Grav.43, 053001 (2026), arXiv:2511.15890 [gr-qc]

    work page arXiv 2026

  10. [10]

    P. C. C. Freire, N. Wex, G. Esposito-Farese, J. P. W. Verbiest, M. Bailes, B. A. Jacoby, M. Kramer, I. H. Stairs, J. Anto- niadis, and G. H. Janssen, The relativistic pulsar-white dwarf binary PSR J1738+0333 II. The most stringent test of scalar- tensor gravity, Mon. Not. Roy. Astron. Soc.423, 3328 (2012), arXiv:1205.1450 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  11. [11]

    A Massive Pulsar in a Compact Relativistic Binary

    J. Antoniadiset al., A Massive Pulsar in a Compact Relativistic Binary, Science340, 6131 (2013), arXiv:1304.6875 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  12. [12]

    L. Shao, N. Sennett, A. Buonanno, M. Kramer, and N. Wex, Constraining nonperturbative strong-field effects in scalar-tensor gravity by combining pulsar timing and laser- interferometer gravitational-wave detectors, Phys. Rev. X7, 041025 (2017), arXiv:1704.07561 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  13. [13]

    Anderson, P

    D. Anderson, P. Freire, and N. Yunes, Binary pulsar constraints on massless scalar–tensor theories using Bayesian statistics, Class. Quant. Grav.36, 225009 (2019), arXiv:1901.00938 [gr- qc]

    work page arXiv 2019

  14. [14]

    J. Zhao, P. C. C. Freire, M. Kramer, L. Shao, and N. Wex, Closing a spontaneous-scalarization window with binary pul- sars, Class. Quant. Grav.39, 11LT01 (2022), arXiv:2201.03771 [astro-ph.HE]

    work page arXiv 2022

  15. [15]

    S. S. Yazadjiev, D. D. Doneva, and D. Popchev, Slowly rotating neutron stars in scalar-tensor theories with a massive scalar field, Phys. Rev. D93, 084038 (2016), arXiv:1602.04766 [gr- qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  16. [16]

    K. V . Staykov, D. Popchev, D. D. Doneva, and S. S. Yazadjiev, Static and slowly rotating neutron stars in scalar–tensor theory with self-interacting massive scalar field, Eur. Phys. J. C78, 586 (2018), arXiv:1805.07818 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  17. [17]

    R. Xu, Y . Gao, and L. Shao, Strong-field effects in massive scalar-tensor gravity for slowly spinning neutron stars and appli- cation to X-ray pulsar pulse profiles, Phys. Rev. D102, 064057 (2020), arXiv:2007.10080 [gr-qc]

    work page arXiv 2020

  18. [18]

    Z. Hu, Y . Gao, R. Xu, and L. Shao, Scalarized neutron stars in massive scalar-tensor gravity: X-ray pulsars and tidal deforma- bility, Phys. Rev. D104, 104014 (2021), [Erratum: Phys.Rev.D 111, 109903 (2025)], arXiv:2109.13453 [gr-qc]

    work page arXiv 2021

  19. [19]

    Moment of inertia - mass universal relations for neutron stars in scalar-tensor theory with self-interacting massive scalar field

    D. Popchev, K. V . Staykov, D. D. Doneva, and S. S. Yazadjiev, Moment of inertia–mass universal relations for neutron stars in scalar-tensor theory with self-interacting massive scalar field, Eur. Phys. J. C79, 178 (2019), arXiv:1812.00347 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  20. [20]

    V . I. Danchev and D. D. Doneva, Constraining the equation of state in modified gravity via universal relations, Phys. Rev. D 103, 024049 (2021), arXiv:2010.07392 [gr-qc]

    work page arXiv 2021

  21. [21]

    Spontaneous scalarization with an extremely massive field and heavy neutron stars

    S. Morisaki and T. Suyama, Spontaneous scalarization with an extremely massive field and heavy neutron stars, Phys. Rev. D 96, 084026 (2017), arXiv:1707.02809 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  22. [22]

    Rosca-Mead, C

    R. Rosca-Mead, C. J. Moore, U. Sperhake, M. Agathos, and D. Gerosa, Structure of neutron stars in massive scalar-tensor gravity, Symmetry12, 1384 (2020), arXiv:2007.14429 [gr-qc]

    work page arXiv 2020

  23. [23]

    J. C. Degollado, N. Ortiz, and M. Salgado, Dynamical transi- tion to spontaneous scalarization in neutron stars: The mas- sive scalar field scenario, Phys. Rev. D110, 084011 (2024), arXiv:2407.08124 [gr-qc]

    work page arXiv 2024

  24. [24]

    F. M. Ramazano˘glu and F. Pretorius, Spontaneous Scalariza- tion with Massive Fields, Phys. Rev. D93, 064005 (2016), arXiv:1601.07475 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  25. [25]

    Alcock, E

    C. Alcock, E. Farhi, and A. Olinto, Strange stars, Astrophys. J. 310, 261 (1986)

    1986

  26. [26]

    Rahimi and Z

    F. Rahimi and Z. Rezaei, Scalarized hybrid neutron stars in scalar tensor gravity, Eur. Phys. J. C84, 734 (2024), arXiv:2401.13557 [astro-ph.HE]

    work page arXiv 2024

  27. [27]

    Balkin, J

    R. Balkin, J. Serra, K. Springmann, S. Stelzl, and A. Weiler, Heavy neutron stars from light scalars, JHEP02(2025), 141, arXiv:2307.14418 [hep-ph]

    work page arXiv 2025

  28. [28]

    U. H. Gerlach, Equation of State at Supranuclear Densities and the Existence of a Third Family of Superdense Stars, Phys. Rev. 172, 1325 (1968)

    1968

  29. [29]

    N. K. Glendenning and C. Kettner, Nonidentical neutron star twins, Astron. Astrophys.353, L9 (2000), arXiv:astro- ph/9807155

    work page arXiv 2000

  30. [30]

    Quark phases in neutron stars and a "third family" of compact stars as a signature for phase transitions

    K. Schertler, C. Greiner, J. Schaffner-Bielich, and M. H. Thoma, Quark phases in neutron stars and a ’third family’ of compact stars as a signature for phase transitions, Nucl. Phys. A677, 463 (2000), arXiv:astro-ph/0001467

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  31. [31]

    M. G. Alford, S. Han, and M. Prakash, Generic conditions for stable hybrid stars, Phys. Rev. D88, 083013 (2013), arXiv:1302.4732 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  32. [32]

    A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars

    S. Benic, D. Blaschke, D. E. Alvarez-Castillo, T. Fischer, and S. Typel, A new quark-hadron hybrid equation of state for astro- physics - I. High-mass twin compact stars, Astron. Astrophys. 577, A40 (2015), arXiv:1411.2856 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  33. [33]

    Signals in the tidal deformability for phase transitions in compact stars with constraints from GW170817

    J.-E. Christian, A. Zacchi, and J. Schaffner-Bielich, Signals in the tidal deformability for phase transitions in compact stars with constraints from GW170817, Phys. Rev. D99, 023009 (2019), arXiv:1809.03333 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  34. [34]

    P. T. H. Pang, T. Dietrich, I. Tews, and C. Van Den Broeck, Pa- rameter estimation for strong phase transitions in supranuclear matter using gravitational-wave astronomy, Phys. Rev. Res.2, 033514 (2020), arXiv:2006.14936 [astro-ph.HE]

    work page arXiv 2020

  35. [35]

    H. Tan, T. Dore, V . Dexheimer, J. Noronha-Hostler, and N. Yunes, Extreme matter meets extreme gravity: Ultraheavy neutron stars with phase transitions, Phys. Rev. D105, 023018 (2022), arXiv:2106.03890 [astro-ph.HE]

    work page arXiv 2022

  36. [36]

    Damour and G

    T. Damour and G. Esposito-Farese, Tensor multiscalar theories of gravitation, Class. Quant. Grav.9, 2093 (1992)

    2093

  37. [37]

    H.-J. Kuan, K. Van Aelst, A. T.-L. Lam, and M. Shibata, Binary neutron star mergers in massive scalar-tensor the- ory: Quasiequilibrium states and dynamical enhancement of the scalarization, Phys. Rev. D108, 064057 (2023), arXiv:2309.01709 [gr-qc]

    work page arXiv 2023

  38. [38]

    I-Love-Q Relations in Neutron Stars and their Applications to Astrophysics, Gravitational Waves and Fundamental Physics

    K. Yagi and N. Yunes, I-Love-Q Relations in Neutron Stars 8 and their Applications to Astrophysics, Gravitational Waves and Fundamental Physics, Phys. Rev. D88, 023009 (2013), arXiv:1303.1528 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  39. [39]

    I-Love-Q

    K. Yagi and N. Yunes, I-Love-Q, Science341, 365 (2013), arXiv:1302.4499 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  40. [40]

    I-Love-Q, Spontaneously: Slowly Rotating Neutron Stars in Scalar-Tensor Theories

    P. Pani and E. Berti, Slowly rotating neutron stars in scalar-tensor theories, Phys. Rev. D90, 024025 (2014), arXiv:1405.4547 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  41. [41]

    Coalescence of binary neutron stars in a scalar-tensor theory of gravity

    M. Shibata, K. Taniguchi, H. Okawa, and A. Buonanno, Coales- cence of binary neutron stars in a scalar-tensor theory of gravity, Phys. Rev. D89, 084005 (2014), arXiv:1310.0627 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  42. [42]

    Quasiequilibrium sequences of binary neutron stars undergoing dynamical scalarization

    K. Taniguchi, M. Shibata, and A. Buonanno, Quasiequilibrium sequences of binary neutron stars undergoing dynamical scalar- ization, Phys. Rev. D91, 024033 (2015), arXiv:1410.0738 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  43. [43]

    Kuroda and M

    T. Kuroda and M. Shibata, Spontaneous scalarization as a new core-collapse supernova mechanism and its multimessenger signals, Phys. Rev. D107, 103025 (2023), arXiv:2302.09853 [astro-ph.HE]

    work page arXiv 2023

  44. [44]

    A. T.-L. Lam, K. V . Staykov, H.-J. Kuan, D. D. Doneva, and S. S. Yazadjiev, Axisymmetric stability of neutron stars as extreme rotators in massive scalar-tensor theory, Phys. Rev. D 111, 104030 (2025), arXiv:2502.03973 [gr-qc]

    work page arXiv 2025

  45. [45]

    A. T.-L. Lam, Y . Gao, H.-J. Kuan, M. Shibata, K. Van Aelst, and K. Kiuchi, Accessing Universal Relations of Binary Neutron Star Waveforms in Massive Scalar-Tensor Theory, Phys. Rev. Lett.134, 151402 (2025), arXiv:2410.00137 [astro- ph.HE]

    work page arXiv 2025

  46. [46]

    Komatsu, Y

    H. Komatsu, Y . Eriguchi, and I. Hachisu, Rapidly rotating gen- eral relativistic stars. I - Numerical method and its application to uniformly rotating polytropes, Mon. Not. Roy. Astron. Soc. 237, 355 (1989)

    1989

  47. [47]

    G. B. Cook, S. L. Shapiro, and S. A. Teukolsky, Spin-up of a Rapidly Rotating Star by Angular Momentum Loss: Effects of General Relativity, ApJ398, 203 (1992)

    1992

  48. [48]

    D. D. Doneva, S. S. Yazadjiev, N. Stergioulas, and K. D. Kokko- tas, Rapidly rotating neutron stars in scalar-tensor theories of gravity, Phys. Rev. D88, 084060 (2013), arXiv:1309.0605 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  49. [49]

    D. D. Doneva and S. S. Yazadjiev, Rapidly rotating neutron stars with a massive scalar field—structure and universal rela- tions, JCAP11(2016), 019, arXiv:1607.03299 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  50. [50]

    D. D. Doneva, S. S. Yazadjiev, N. Stergioulas, and K. D. Kokko- tas, Differentially rotating neutron stars in scalar-tensor theories of gravity, Phys. Rev. D98, 104039 (2018), arXiv:1807.05449 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  51. [51]

    K. V . Staykov, D. D. Doneva, L. Heisenberg, N. Stergioulas, and S. S. Yazadjiev, Differentially rotating scalarized neu- tron stars with realistic postmerger profiles, Phys. Rev. D108, 024058 (2023), arXiv:2303.07769 [gr-qc]

    work page arXiv 2023

  52. [52]

    J. C. O. M., D. D. Doneva, P. Cerdá-Durán, J. A. Font, and S. S. Yazadjiev, Rapidly Rotating Neutron Star Collapse in Massive Scalar-Tensor Theories, arXiv (2026), arXiv:2605.16506 [gr- qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  53. [53]

    Bonazzola, E

    S. Bonazzola, E. Gourgoulhon, M. Salgado, and J. A. Marck, Axisymmetric rotating relativistic bodies: A new numerical approach for ’exact’ solutions, Astron. Astrophys.278, 421 (1993)

    1993

  54. [54]

    Shibata, Rotating black hole surrounded by self-gravitating torus in the puncture framework, Phys

    M. Shibata, Rotating black hole surrounded by self-gravitating torus in the puncture framework, Phys. Rev. D76, 064035 (2007)

    2007

  55. [55]

    Rotating Stars in Relativity

    V . Paschalidis and N. Stergioulas, Rotating Stars in Relativity, Living Rev. Rel.20, 7 (2017), arXiv:1612.03050 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  56. [56]

    J. D. Jackson,Classical Electrodynamics(John Wiley & Sons, 1962)

    1962

  57. [57]

    (2026), this Green’s function, equivalent toe−mϕ|r−r′|/(4π|r−r ′|), reduces to the one for Laplace equation in the mϕ → 0 limit, i.e., G(r,r ′)mϕ→0 =( rℓ/r′ℓ+1)[mϕ(2ℓ +1)] −1 for any finite r and r′

    2026

  58. [58]

    G. B. Cook, S. L. Shapiro, and S. A. Teukolsky, Rapidly ro- tating polytropes in general relativity, Astrophys. J.422, 227 (1994)

    1994

  59. [59]

    G. B. Cook, S. L. Shapiro, and S. A. Teukolsky, Rapidly rotat- ing neutron stars in general relativity: Realistic equations of state, Astrophys. J.424, 823 (1994)

    1994

  60. [60]

    Stergioulas and J

    N. Stergioulas and J. L. Friedman, Comparing models of rapidly rotating relativistic stars constructed by two numer- ical methods, Astrophys. J.444, 306 (1995), arXiv:astro- ph/9411032

    work page arXiv 1995

  61. [61]

    F. J. Fattoyev, C. J. Horowitz, J. Piekarewicz, and G. Shen, Relativistic effective interaction for nuclei, giant reso- nances, and neutron stars, Phys. Rev. C82, 055803 (2010), arXiv:1008.3030 [nucl-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  62. [62]

    Legred, L

    I. Legred, L. Brodie, A. Haber, R. Essick, and K. Chatziioan- nou, Nonparametric extensions of nuclear equations of state: Probing the breakdown scale of relativistic mean-field theory, Phys. Rev. D112, 063003 (2025), arXiv:2505.07677 [nucl-th]

    work page arXiv 2025

  63. [63]

    H. Tan, J. Noronha-Hostler, and N. Yunes, Neutron Star Equa- tion of State in light of GW190814, Phys. Rev. Lett.125, 261104 (2020), arXiv:2006.16296 [astro-ph.HE]

    work page arXiv 2020

  64. [64]

    Quarkyonic Matter and Neutron Stars

    L. McLerran and S. Reddy, Quarkyonic Matter and Neutron Stars, Phys. Rev. Lett.122, 122701 (2019), arXiv:1811.12503 [nucl-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  65. [65]

    D. M. Podkowka, R. F. P. Mendes, and E. Poisson, Trace of the energy-momentum tensor and macroscopic properties of neu- tron stars, Phys. Rev. D98, 064057 (2018), arXiv:1807.01565 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  66. [66]

    Fujimoto, K

    Y . Fujimoto, K. Fukushima, L. D. McLerran, and M. Praszalow- icz, Trace Anomaly as Signature of Conformality in Neutron Stars, Phys. Rev. Lett.129, 252702 (2022), arXiv:2207.06753 [nucl-th]

    work page arXiv 2022

  67. [67]

    Marczenko, L

    M. Marczenko, L. McLerran, K. Redlich, and C. Sasaki, Reach- ing percolation and conformal limits in neutron stars, Phys. Rev. C107, 025802 (2023), arXiv:2207.13059 [nucl-th]

    work page arXiv 2023

  68. [68]

    R. F. P. Mendes, C. F. Sodré, and F. T. Falciano, Exceeding the conformal limit inside rotating neutron stars: Implications to modified theories of gravity, Phys. Rev. D110, 104027 (2024), arXiv:2407.20345 [gr-qc]

    work page arXiv 2024

  69. [69]

    Ji and L

    P. Ji and L. Shao, Scalarized neutron stars with a highly rela- tivistic core in scalar-tensor gravity, Phys. Rev. D112, 104030 (2025), arXiv:2508.12573 [gr-qc]

    work page arXiv 2025

  70. [70]

    A. R. Bodmer, Collapsed nuclei, Phys. Rev. D4, 1601 (1971)

    1971

  71. [71]

    Witten, Cosmic Separation of Phases, Phys

    E. Witten, Cosmic Separation of Phases, Phys. Rev. D30, 272 (1984)

    1984

  72. [72]

    Chodos, R

    A. Chodos, R. L. Jaffe, K. Johnson, C. B. Thorn, and V . F. Weisskopf, A New Extended Model of Hadrons, Phys. Rev. D 9, 3471 (1974)

    1974

  73. [73]

    Farhi and R

    E. Farhi and R. L. Jaffe, Strange Matter, Phys. Rev. D30, 2379 (1984)

    1984

  74. [74]

    Sorkin, A Criterion for the onset of instability at a turning point, Astrophys

    R. Sorkin, A Criterion for the onset of instability at a turning point, Astrophys. J.249, 254 (1981)

    1981

  75. [75]

    R. D. Sorkin, A Stability criterion for many parameter equilib- rium families, Astrophys. J.257, 847 (1982)

    1982

  76. [76]

    J. L. Friedman, J. R. Ipser, and R. D. Sorkin, Turning point method for axisymmetric stability of rotating relativistic stars, Astrophys. J.325, 722 (1988)

    1988

  77. [77]

    Harada, Neutron stars in scalar tensor theories of gravity and catastrophe theory, Phys

    T. Harada, Neutron stars in scalar tensor theories of gravity and catastrophe theory, Phys. Rev. D57, 4802 (1998), arXiv:gr- 9 qc/9801049

    work page arXiv 1998

  78. [78]

    D. D. Doneva and S. S. Yazadjiev, Topological neutron stars in tensor-multi-scalar theories of gravity, Phys. Rev. D101, 064072 (2020), arXiv:1911.06908 [gr-qc]

    work page arXiv 2020

  79. [79]

    H.-J. Kuan, J. Singh, D. D. Doneva, S. S. Yazadjiev, and K. D. Kokkotas, Nonlinear evolution and nonuniqueness of scalarized neutron stars, Phys. Rev. D104, 124013 (2021), arXiv:2105.08543 [gr-qc]

    work page arXiv 2021

  80. [80]

    A. T.-L. Lam and M. Shibata, New axisymmetric general rela- tivistic hydrodynamics code with fixed mesh refinement, Phys. Rev. D111, 103039 (2025), arXiv:2502.03223 [astro-ph.HE]

    work page arXiv 2025

Showing first 80 references.