Speed of sound in Kaluza-Klein Fermi gas

Anna Horv\'ath; Emese Forg\'acs-Dajka; Gergely G\'abor Barnaf\"oldi

REVIEW 2 major objections 6 minor 22 references

Speed of sound in Kaluza-Klein Fermi gas

T0 review · 2 major / 6 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read A compact fifth dimension would shift the conformal speed of sound from 1/3 to 1/4 and add threshold dips.

desk verdict Plausible but under-derived: the KK speed-of-sound results rest on Ref 13 and an asserted 1/4 limit. read the letter →

arxiv 2502.04974 v1 pith:4WI6L5KI submitted 2025-02-07 hep-ph astro-ph.HEnucl-th

Anna Horváth , Emese Forgács-Dajka , Gergely Gábor Barnaföldi This is my paper · ORCID

classification hep-phastro-ph.HEnucl-th

keywords Kaluza-KleintheoryspeedofsoundequationstateFermigasneutronstarsextradimensionsconformallimitcompactificationradius

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper asks whether a compactified fifth dimension would leave a measurable imprint on the equation of state of cold, dense matter. Using a five-dimensional Kaluza-Klein spacetime with a constant extra-dimensional metric component, the authors model a zero-temperature, electrically neutral Fermi gas with a repulsive potential linear in baryon density and compute the speed of sound squared $c_s^2$. They find two signatures: with a finite number of excitation levels, $c_s^2$ dips each time a new Kaluza-Klein level becomes occupied and then returns to the ordinary three-dimensional conformal limit $1/3$; with infinitely many levels, the extra dimension expands the phase space and the conformal limit becomes $1/4$. Since $c_s^2$ is connected to neutron-star observables, the result identifies a concrete way that extra dimensions could be probed by astrophysical measurements.

What carries the argument

The central object is the Kaluza-Klein mass ladder $\bar m^2(N_\mathrm{exc}) = m^2 + (N_\mathrm{exc}/r_c)^2$, which converts the compact fifth dimension into a discrete tower of effective particle masses via the periodic boundary condition on a circle of radius $r_c$. This ladder carries the argument because the number of occupied levels $N_\mathrm{exc}$ directly controls the available phase space, and each newly opened level adds a fresh threshold in the equation of state. The companion ingredient is the linear repulsive potential $U(n)=\xi n$, which enters through a modified chemical potential $\bar\mu=\mu-U(n)$ and contributes $p_\mathrm{int}=\varepsilon_\mathrm{int}=\frac12 \xi n^2$ to the pressure and energy density. The speed of sound squared $c_s^2=\partial p/\partial\varepsilon$ at fixed entropy is the diagnostic that maps this level structure onto a quantity observable in neutron-star physics.

What would settle it

Recompute $c_s^2$ from the same thermodynamic potential with a density-dependent $g_{55}$ (or with a saturating interaction such as a Skyrme-type potential fitted to nuclear saturation) and check whether the threshold dips and the high-density approach to $1/4$ survive; if they disappear, the signatures are artifacts of the constant-ladder plus linear-potential idealization. A purely observational test would be to look for non-monotonic staircase structure in the sound speed inferred from neutron-star mass-radius or tidal-deformability data near the relevant energy densities.

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Extended reading notes

Core claim

In five-dimensional Kaluza-Klein theory with topology $\mathbb{R}^4\times S^1$ and a constant fifth metric component, the extra dimension appears in four dimensions as a tower of effective masses $\bar m^2(N_\mathrm{exc}) = m^2 + (N_\mathrm{exc}/r_c)^2$, where $r_c$ is the compactification radius and $N_\mathrm{exc}$ is the excitation number. The paper shows numerically that a zero-temperature, neutral Fermi gas built on this ladder, with a repulsive linear potential $U(n)=\xi n$, has a speed of sound squared that starts at zero, rises to a saturation region, and then behaves differently depending on how many levels are open. For finite $N_\mathrm{exc}=10$ and small $r_c$, $c_s^2$ develops one dip at the opening of each new level and, after the last level, tends toward the standard conformal value $1/3$. For $N_\mathrm{exc}=\infty$, the same quantity approaches $1/4$ at high energy density. In the interacting case the sound speed reaches unity at high density while causality is preserved; the influence of $r_c$ is strongest when $\xi$ is small, and for large $r_c$ the level spacing becomes so fine that the dips are washed out.

Load-bearing premise

The result rests on treating the fifth metric component as a constant, so the Kaluza-Klein spectrum is the simple ladder $\bar m^2(N_\mathrm{exc})=m^2+(N_\mathrm{exc}/r_c)^2$, and on modelling the strong interaction by a repulsive potential linear in baryon density, $U(n)=\xi n$; if $g_{55}$ varies with density or the interaction is not linear, the dips and the $1/4$ conformal limit would change.

Editorial extensions

If this is right

A compact extra dimension with radius around $0.01$ fm would imprint a series of dips in $c_s^2$, one per newly occupied Kaluza-Klein level, so a measured staircase-like sound-speed pattern would be direct evidence of the extra dimension.
If infinitely many excitation levels can open, the conformal limit of $c_s^2$ in dense matter shifts from $1/3$ to $1/4$, giving a specific high-density target that differs from ordinary four-dimensional models.
For matter with the linear repulsive potential, $c_s^2$ reaches unity at high densities while remaining causal, so the model survives the causality constraint that rules out many stiff equations of state.
The extra-dimension effects are strongest for small interaction strength and small compactification radius; when $\xi$ is large or $r_c\simeq 100$ fm the level structure is smeared into a continuum and the dips disappear.
At realistic neutron-star central densities around $1100$ MeV/fm$^3$ the first excited level is not yet reached, so current pulsar observations constrain the model only weakly and the new signatures live at higher energies.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

The $1/4$ conformal limit is the natural value for a gas with four spatial dimensions ($c_s^2=1/d$ for a conformal gas), so the infinite-level limit appears to restore full five-dimensional Lorentz symmetry in the equation of state; extending the same ladder construction to $n$ compact dimensions would predict $c_s^2\to 1/(n+3)$.
The dips are in principle a spectral fingerprint: their positions and spacings in energy density are set by $r_c$ and the baryon mass, so a future high-density measurement could read off the compactification radius directly from the sound-speed curve.
The constant-$g_{55}$ assumption ignores the back-reaction of matter on the fifth dimension; a dynamical scalar field would likely shift level thresholds with density and could smear or remove the clean dips, which is a testable modification within the same theoretical setup.
Because the linear potential is what drives $c_s^2$ to unity in the interacting case, replacing it with a saturating nuclear interaction would probably cap the sound speed below unity and change the conformal approach, so the interacting high-density behaviour is an artifact-prone part of the model.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Short proceedings-style note. The authors take their earlier KK equation of state (arXiv:2408.16497) and compute c_s^2 for a zero-temperature Fermi gas with a linear repulsive potential. The headline results — c_s^2 → 1/4 with an infinite tower of KK modes, 1/3 with a finite cutoff, with dips at each threshold — are physically sensible and consistent with the standard result that a massless gas in d spatial dimensions has c_s^2 = 1/d. That is about the extent of the new material; the paper is a parameter scan of a known model, not a new derivation.

What the paper does well: it is honest about the energy scales. It states clearly that realistic neutron star central densities (~1100 MeV/fm^3) are far below the 10^6–10^8 MeV/fm^3 region where the effects appear, so it doesn't overclaim relevance. It also checks causality for all parameter choices, which is easy to forget in toy models. The plots seem to illustrate the qualitative behavior expected.

The soft spot is real: none of the central numbers are derivable from the manuscript. The equation of state, the thermodynamic potential, and the derivative leading to c_s^2 are all referred to Ref. 13. The conformal limit 1/4 is asserted without showing the sum over KK modes or the measure factors (including the k5 = Nexc/rc factor and the spin degeneracy). A referee cannot verify the claimed limits from this text alone. That is not necessarily a fatal flaw for a proceedings-style contribution, but it makes the paper more of an extended abstract. The stress test's concern about the missing derivation is on point: if the continuum replacement is done incorrectly, the limit changes. Since the paper doesn't show it, support is the issue, not a mathematical contradiction.

The interaction U(n)=ξn is a toy choice, not a flaw by itself. The authors note that a more complex potential would be more realistic. The self-citation pattern is acceptable since the EoS is genuinely from their prior work; it would be better if they reproduced the key formulas.

Who is this for? Readers working on KK phenomenology or on EoS models who want a quick look at how the speed of sound behaves in this toy model. It is not a standalone research contribution.

Recommendation: if this is submitted as a proceedings paper, it is acceptable with a request to include the main equations in an appendix. If submitted as a regular paper, a serious referee should demand the derivation of the 1/4 limit and the threshold dips. I would not reject it, but I would require the authors to show their work.

Referee Report

2 major / 6 minor

Summary. The paper claims that in a five-dimensional Kaluza-Klein spacetime with one compactified spatial dimension, the speed of sound squared of a zero-temperature Fermi gas with a repulsive linear interaction U(n)=ξn depends on the number of accessible Kaluza-Klein excitation levels. For a finite maximum excitation number N_exc, the conformal limit is c_s^2=1/3, while for an infinite number of levels it is c_s^2=1/4. The paper also reports dips in c_s^2 at thresholds where new KK modes become occupied, and that the interacting cases saturate at c_s^2=1. The results are presented through plots, with the equation of state taken from the authors' earlier work (Ref. 13).

Significance. If correct, the model offers a phenomenological signature of extra dimensions in the equation of state of dense matter, distinguishing the conformal limit and threshold dips in a bulk transport property. The paper is explicit that realistic neutron-star central densities (about 1100 MeV/fm^3) are far below the energy regime where these effects appear, so the claims are about a hypothetical high-density phase. The connection between higher-dimensional phase space and the speed of sound is conceptually interesting. However, the paper is not self-contained: the central derivation is absent, and the numerical results cannot be reproduced from the manuscript alone. The simplicity of the model is a limitation but not a disqualifying one.

major comments (2)

[Section 3, Fig. 1] The central quantitative claims—the conformal limits c_s^2→1/3 and c_s^2→1/4, and the appearance of dips—are asserted without derivation in this manuscript. Although Eq. (2) gives the single-particle spectrum, the thermodynamic potential, the density sum over KK modes, and the explicit evaluation of Eq. (4) are not shown; the reader is referred to Ref. 13 for the equation of state. To make the paper self-contained and verifiable, please provide at least the key steps: the grand potential per volume, the number density and pressure, and the explicit limit μ→∞ for both finite and infinite N_exc. In particular, the 1/4 result requires demonstrating that the discrete sum over N_exc with spacing dk5=1/r_c reduces to a four-dimensional phase-space integral with the correct measure; any mishandling of the measure changes the limit. Similarly, the finite-N_exc 1/3 result requires showing that each occupied mode becomes ultrarelativistic and that the total pressure and energy density each sum to the 3D massless-gas form. Without these derivations, the headline results cannot be checked.
[Section 3, Fig. 1] The figure is the sole evidence for the dips and for the claimed two-orders-of-magnitude difference in saturation energy between r_c=0.01 fm and r_c=100 fm. The manuscript does not provide the numerical data, the parameter grid, or an analytic expression for even one representative curve. To allow independent verification, please include either a table of c_s^2 values at selected energy densities or an analytic approximation for the non-interacting case, such as the threshold behaviour of the Fermi momentum for each mode, k_Fn^2=μ^2−m_n^2. The dips are said to be 'clearly visible' for N_exc=10, ξ=0, r_c=0.01 fm; a quantitative description (e.g., dip positions in ε and their widths) would strengthen the presentation.

minor comments (6)

[Introduction] There is a typo: 'is which connected' should read 'which is connected'.
[Section 3] The phrase 'Latter denotes' should read 'The latter denotes'.
[Figure 1 caption] The caption says 'Line style: size of the extra dimension, r_c', but the text refers to solid and dashed curves. Please specify in the caption which line style corresponds to which r_c value.
[Section 3] The text says the saturation energy is reached 'at around 10^6−10^8 MeV/fm^3'. This is a wide range; please clarify what determines the lower and upper bounds.
[Section 3] The phrase 'interaction strength of the 5-dimensional interaction' is redundant; consider 'interaction strength' or 'strength of the 5-dimensional interaction'.
[References] Ref. 13 is an arXiv preprint. If the journal requires peer-reviewed references, please check whether it has been published or is under review, and cite the published version if available.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the speed-of-sound results are forward consequences of the stated KK spectrum and linear-potential EoS, not fitted inputs renamed as predictions.

full rationale

The paper's derivation chain is a standard forward model: a KK mass ladder E=sqrt(k^2+(Nexc/rc)^2+m^2), a zero-temperature Fermi-gas EoS, a linear repulsive potential U(n)=xi n, and the thermodynamic derivative c_s^2=dp/depsilon. The reported behaviors (dips at level thresholds, 1/3 for finite Nexc, 1/4 for infinite Nexc, and c_s^2=1 for the interacting case) are mathematical consequences of these stated assumptions, not quantities to which the model parameters were fitted. No parameter is tuned to the speed-of-sound data; xi, rc, and Nexc are scanned model inputs. The paper does rely on the authors' prior Ref. [13] for the detailed EoS, but that reliance supplies a previously constrained model rather than importing the target result itself; the cited EoS was constrained by pulsar data and does not assume the sound-speed curves that are the new output here. The absence of displayed thermodynamic integrals in the text is a reproducibility and support gap, but it is not circularity because no equation in the paper reduces to its own input by construction.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The central claim rests on three free parameters (ξ, r_c, N_exc) and a set of modeling assumptions: a constant fifth metric component producing an evenly spaced KK spectrum, a zero-temperature Fermi gas, and a linear repulsive interaction. No new particles or forces are introduced; the extra dimension is a standard Kaluza-Klein construct.

free parameters (3)

ξ (interaction strength) = 500, 1000, 1500 MeV/fm^3 (scanned)
Strength of the repulsive linear potential U(n)=ξn; a free model parameter, not fitted in this paper.
r_c (compactification radius) = 0.01 fm and 100 fm (scanned)
Size of the extra dimension; a free parameter scanned here, though referenced to pulsar constraints in Ref 13.
N_exc (maximum excitation number) = 10 and ∞ (scanned)
Number of allowed Kaluza-Klein levels; a model choice that controls the phase space.

assumptions (4)

standard math Speed of sound squared is defined as dp/dε at constant entropy
Standard thermodynamic definition used in Eq. (4).
domain assumption The gas is at zero temperature
Approximation for cold dense neutron-star matter; stated in Section 2.
domain assumption The Kaluza-Klein metric is diagonal with constant g55, giving the KK mass ladder
Stated in Section 2, Eq. (1) and following text; this simplifies the extra dimension to a mass spectrum.
ad hoc to paper The baryonic interaction is a repulsive potential linear in density, U(n)=ξ n
Introduced in Section 2 to mimic nuclear-like forces; the authors acknowledge it is simplistic and not derived from QCD.

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Cite this review

Pith. "Pith review of Speed of sound in Kaluza-Klein Fermi gas." pith.science (2026). https://pith.science/paper/4WI6L5KI

@misc{pith2026250204974,
  author       = {Pith},
  title        = {Pith review of: Speed of sound in Kaluza-Klein Fermi gas},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4WI6L5KI}},
  note         = {Machine review of arXiv:2502.04974}
}

read the original abstract

A five-dimensional Kaluza-Klein spacetime model is considered, with one extra compactified spatial dimension. The equation of state of an electrically neutral, zero-temperature Fermi gas with a repulsive linear potential is described. From the equation of state, the speed of sound squared is calculated and shown for different model parameters. Its properties are studied from lower energies up to the conformal limit.

Figures

Figures reproduced from arXiv: 2502.04974 by the authors.

Discussion (0). Continue with ORCID to comment.

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Works this paper leans on

22 extracted references · 20 canonical work pages

[1]

On the Sound Speed in Neutron Stars,

S. Altiparmak, C. Ecker, and L. Rezzolla, “On the Sound Speed in Neutron Stars,” Astrophys. J. Lett., vol. 939, no. 2, p. L34, 2022

work page 2022
[2]

Masses, Radii, and the Equation of State of Neutron Stars,

F. ¨Ozel and P. Freire, “Masses, Radii, and the Equation of State of Neutron Stars,” Ann. Rev. Astron. Astrophys., vol. 54, pp. 401–440, 2016. 6 KK-ActaPhysPol˙2025 printed on February 10, 2025

work page 2016
[3]

Gw170817: Measurements of neutron star radii and equation of state,

B. Abbott et al., “Gw170817: Measurements of neutron star radii and equation of state,” Phys. Rev. Lett., vol. 121, p. 161101, Oct 2018. [Online]. Available: https://link.aps.org/doi/10.1103/PhysRevLett.121.161101

doi:10.1103/physrevlett.121.161101 2018
[4]

Thermodynam- ics of hot strong-interaction matter from ultrarelativistic nuclear collisions,

F. G. Gardim, G. Giacalone, M. Luzum, and J.-Y. Ollitrault, “Thermodynam- ics of hot strong-interaction matter from ultrarelativistic nuclear collisions,” Nature Phys., vol. 16, no. 6, pp. 615–619, 2020

work page 2020
[5]

Constraining neutron-star equation of state using heavy-ion collisions,

C. Y. Tsang, M. B. Tsang, P. Danielewicz, W. G. Lynch, and F. J. Fattoyev, “Constraining neutron-star equation of state using heavy-ion collisions,” 7 2018

work page 2018
[6]

Are nuclear matter properties correlated to neutron star observables?

J.-B. Wei, J.-J. Lu, G. F. Burgio, Z.-H. Li, and H.-J. Schulze, “Are nuclear matter properties correlated to neutron star observables?” The European Physical Journal A, vol. 56, no. 2, Feb. 2020. [Online]. Available: http://dx.doi.org/10.1140/epja/s10050-020-00058-3

work page doi:10.1140/epja/s10050-020-00058-3 2020
[7]

Average speed of sound in neutron stars,

M. Marczenko, “Average speed of sound in neutron stars,” Phys. Rev. C, vol. 110, no. 4, p. 045811, 2024

work page 2024
[8]

Reaching percolation and conformal limits in neutron stars,

M. Marczenko, L. McLerran, K. Redlich, and C. Sasaki, “Reaching percolation and conformal limits in neutron stars,” Phys. Rev. C, vol. 107, p. 025802, Feb 2023. [Online]. Available: https://link.aps.org/doi/10.1103/ PhysRevC.107.025802

work page 2023

Show all 22 references

[9]

Correspondence of Many-flavor Limit and Kaluza-Klein Degrees of Freedom in the Description of Compact Stars,

S. Karsai, G. G. Barnaf¨ oldi, E. Forg´ acs-Dajka, and P. P´ osfay, “Correspondence of Many-flavor Limit and Kaluza-Klein Degrees of Freedom in the Description of Compact Stars,” Acta Phys. Polon. Supp., vol. 10, p. 827, 2017

2017
[10]

Testing a possible way of geometrization of the strong interaction by a Kaluza–Klein star,

G. G. Barnaf¨ oldi, S. Karsai, B. Luk´ acs, and P. P´ osfay, “Testing a possible way of geometrization of the strong interaction by a Kaluza–Klein star,” Int. J. Mod. Phys. A, vol. 31, no. 28&29, p. 1645031, 2016

2016
[11]

Searching extra dimensions in compact stars,

G. Barnaf¨ oldi, P. L´ evai, and B. Luk´ acs, “Searching extra dimensions in compact stars,” Astronomische Nachrichten, vol. 328, no. 8, p. 809–812, Sep
[12]

Estimating Com- pressibility from Maximal-mass Compact Star Observations,

G. G. Barnaf¨ oldi, P. P´ osfay, B. E. Szigeti, and A. Jakov´ ac, “Estimating Com- pressibility from Maximal-mass Compact Star Observations,” Eur. Phys. J. ST, vol. 229, no. 22-23, pp. 3605–3614, 2020

2020
[13]

Application of kaluza-klein theory in modeling compact stars: Exploring extra dimensions,

A. Horv´ ath, E. Forg´ acs-Dajka, and G. G. Barnaf¨ oldi, “Application of kaluza-klein theory in modeling compact stars: Exploring extra dimensions,”
[14]

Zum Unit¨ atsproblem der Physik,

T. Kaluza, “Zum Unit¨ atsproblem der Physik,” Sitzungsber. Preuss. Akad. Wiss. Berlin (Math. Phys. ), vol. 1921, pp. 966–972, 1921

1921
[15]

Quantum Theory and Five-Dimensional Theory of Relativity. (In German and English),

O. Klein, “Quantum Theory and Five-Dimensional Theory of Relativity. (In German and English),” Z. Phys., vol. 37, pp. 895–906, 1926

1926
[16]

Kaluza-Klein gravity,

J. M. Overduin and P. S. Wesson, “Kaluza-Klein gravity,” Phys. Rept., vol. 283, pp. 303–380, 1997

1997
[17]

Construction of a crossing - symmetric, Regge behaved am- plitude for linearly rising trajectories,

G. Veneziano, “Construction of a crossing - symmetric, Regge behaved am- plitude for linearly rising trajectories,” Nuovo Cim. A, vol. 57, pp. 190–197, 1968. KK-ActaPhysPol˙2025 printed on February 10, 2025 7

1968
[18]

The Theory of Kaluza-Klein-Jordan- Thiry revisited,

R. Coquereaux and G. Esposito-Farese, “The Theory of Kaluza-Klein-Jordan- Thiry revisited,” Ann. Inst. H. Poincare Phys. Theor., vol. 52, pp. 113–150, 1990

1990
[19]

N. K. Glendenning, Compact stars: Nuclear physics, particle physics, and general relativity, 1997

1997
[20]

An Inter- pretable Family of Equation of State for Dense Hadronic Matter,

J. Zim´ anyi, B. Luk´ acs, P. L´ evai, J. P. Bondorf, and N. L. Bal´ azs, “An Inter- pretable Family of Equation of State for Dense Hadronic Matter,” Nucl. Phys. A, vol. 484, pp. 647–660, 1988

1988
[2007]

Available: http://dx.doi.org/10.1002/asna.200710806

[Online]. Available: http://dx.doi.org/10.1002/asna.200710806

doi
[2024]

Available: https://arxiv.org/abs/2408.16497

[Online]. Available: https://arxiv.org/abs/2408.16497

arXiv

Pith tools

Reviewed August 8, 2026 · model on record in the stance chip above.

[1] [1]

On the Sound Speed in Neutron Stars,

S. Altiparmak, C. Ecker, and L. Rezzolla, “On the Sound Speed in Neutron Stars,” Astrophys. J. Lett., vol. 939, no. 2, p. L34, 2022

work page 2022

[2] [2]

Masses, Radii, and the Equation of State of Neutron Stars,

F. ¨Ozel and P. Freire, “Masses, Radii, and the Equation of State of Neutron Stars,” Ann. Rev. Astron. Astrophys., vol. 54, pp. 401–440, 2016. 6 KK-ActaPhysPol˙2025 printed on February 10, 2025

work page 2016

[3] [3]

Gw170817: Measurements of neutron star radii and equation of state,

B. Abbott et al., “Gw170817: Measurements of neutron star radii and equation of state,” Phys. Rev. Lett., vol. 121, p. 161101, Oct 2018. [Online]. Available: https://link.aps.org/doi/10.1103/PhysRevLett.121.161101

doi:10.1103/physrevlett.121.161101 2018

[4] [4]

Thermodynam- ics of hot strong-interaction matter from ultrarelativistic nuclear collisions,

F. G. Gardim, G. Giacalone, M. Luzum, and J.-Y. Ollitrault, “Thermodynam- ics of hot strong-interaction matter from ultrarelativistic nuclear collisions,” Nature Phys., vol. 16, no. 6, pp. 615–619, 2020

work page 2020

[5] [5]

Constraining neutron-star equation of state using heavy-ion collisions,

C. Y. Tsang, M. B. Tsang, P. Danielewicz, W. G. Lynch, and F. J. Fattoyev, “Constraining neutron-star equation of state using heavy-ion collisions,” 7 2018

work page 2018

[6] [6]

Are nuclear matter properties correlated to neutron star observables?

J.-B. Wei, J.-J. Lu, G. F. Burgio, Z.-H. Li, and H.-J. Schulze, “Are nuclear matter properties correlated to neutron star observables?” The European Physical Journal A, vol. 56, no. 2, Feb. 2020. [Online]. Available: http://dx.doi.org/10.1140/epja/s10050-020-00058-3

work page doi:10.1140/epja/s10050-020-00058-3 2020

[7] [7]

Average speed of sound in neutron stars,

M. Marczenko, “Average speed of sound in neutron stars,” Phys. Rev. C, vol. 110, no. 4, p. 045811, 2024

work page 2024

[8] [8]

Reaching percolation and conformal limits in neutron stars,

M. Marczenko, L. McLerran, K. Redlich, and C. Sasaki, “Reaching percolation and conformal limits in neutron stars,” Phys. Rev. C, vol. 107, p. 025802, Feb 2023. [Online]. Available: https://link.aps.org/doi/10.1103/ PhysRevC.107.025802

work page 2023