arxiv: 2512.19907 · v2 · submitted 2025-12-22 · 🌌 astro-ph.HE · hep-ph· nucl-th

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Astrophysical constraints on the cold equation of state of the strongly interacting matter

G\'abor Kasza , J\'anos Tak\'atsy , Gy\"orgy Wolf

Authors on Pith no claims yet

Pith reviewed 2026-05-16 20:03 UTC · model grok-4.3

classification 🌌 astro-ph.HE hep-phnucl-th

keywords neutron starsequation of statedense mattertidal deformabilityGW170817perturbative QCDNICERmaximum mass

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The pith

Massive neutron stars and GW170817 tidal data give the tightest limits on the cold dense-matter equation of state.

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

The authors parametrize the cold equation of state of strongly interacting matter and let its parameters vary while enforcing a match to perturbative QCD at roughly forty times nuclear density. They then apply four sets of astrophysical data: the mass of the heaviest known pulsar, NICER mass-radius measurements for several pulsars, and the tidal deformability extracted from the binary neutron star merger GW170817. Within this setup the requirement that the equation of state support very massive neutron stars together with the tidal-deformability bound removes the largest fraction of parameter space. A reader cares because the surviving equations of state determine the internal structure, maximum mass, and merger signals of all neutron stars.

Core claim

Within the chosen parametrization the existence of very massive neutron stars and the tidal deformability constraint from GW170817 restrict the admissible parameter space of the cold equation of state more effectively than current NICER mass-radius data or the perturbative-QCD matching condition alone.

What carries the argument

A flexible parametrization of the cold equation of state matched to perturbative QCD at high density and constrained by neutron-star mass and tidal-deformability observations.

If this is right

Only equations of state that remain sufficiently stiff at densities several times nuclear density survive.
The pressure and speed of sound at intermediate densities become bounded from below.
NICER data, while consistent, do not yet exclude as much parameter space as the mass and tidal constraints.
Future higher-precision radius or tidal measurements will further shrink the allowed region.

Where Pith is reading between the lines

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

The same constrained equations of state can be fed directly into merger simulations to predict gravitational-wave signals for the next observing run.
Heavy-ion collision data at intermediate densities could be cross-checked against the surviving parameter window.
If the parametrization misses a first-order phase transition the quoted bounds would loosen.

Load-bearing premise

The parametrization is flexible enough to capture every physically allowed behavior of dense matter.

What would settle it

A neutron star whose mass lies well above the current highest measured value or a tidal deformability measurement lying outside the allowed window would rule out the remaining parameter region.

read the original abstract

At present, the only experimental access to the properties of cold, dense strongly interacting matter is provided by astrophysical observations. Neutron stars are the only known systems in the Universe that reach densities several times higher than normal nuclear density at nearly zero temperature, making them unique laboratories for studying dense matter. Since most neutron star observables are sensitive to the equation of state (EOS), observational data place stringent constraints on the EOS of strongly interacting matter. In this work, we investigate constraints arising from perturbative QCD calculations at asymptotically high densities ($\rho \approx 40 \rho_0$), the mass of the heaviest observed neutron star (a black widow pulsar), NICER mass-radius measurements, and the tidal deformability inferred from the binary neutron star merger GW170817. We parametrize the EOS and allow its parameters to vary freely, using observational data to constrain the admissible parameter space. We find that neutron star observations significantly restrict the EOS of dense strongly interacting matter. While NICER has already provided measurements for five pulsars, the associated uncertainties remain relatively large. Within our modeling framework, we find that the existence of very massive neutron stars and constraints on the tidal deformability provide the most restrictive constraints on the EOS.

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.

Desk Editor's Note private letter to a colleague

This applies a standard parametrized-EOS fit to pQCD plus current max-mass, NICER, and GW170817 data and finds the astrophysical pieces dominate the bounds.

read the letter

The paper runs a conventional parametrization of the cold dense-matter EOS, anchors it to perturbative QCD at roughly 40 times nuclear saturation density, and then folds in the heaviest observed neutron-star mass, NICER radius data, and the tidal deformability from GW170817. The central result is that the maximum-mass and tidal constraints are the most restrictive within their framework, while NICER uncertainties are still too large to compete. That conclusion tracks with what the data look like elsewhere, so the exercise is at least consistent on its own terms. The work is transparent about using public inputs and shows how the different constraints interact in one plot or table, which is useful for quick reference. The soft spot is the pQCD anchor. The paper treats the high-density result as a hard upper envelope without a quantified band on the matching density or on the renormalization-scale and truncation errors in the perturbative series. If those systematics are larger than assumed, the allowed volume at intermediate densities grows and the claimed dominance of the astrophysical data weakens. The parametrization itself is not shown to be dense enough in function space to guarantee that no plausible EOS is excluded before the data are applied. This is incremental but solid enough to be worth referee time. It is aimed at people who need an updated summary of where the current observations sit on the EOS plane rather than a new methodological advance. I would send it to review; the inputs are reproducible and a careful check of the numerics and the pQCD matching procedure would be straightforward.

Referee Report

2 major / 2 minor

Summary. The manuscript parametrizes the cold dense-matter equation of state (EOS) and applies constraints from perturbative QCD at ρ≈40ρ0, the mass of the heaviest observed neutron star, NICER mass-radius data for five pulsars, and the tidal deformability inferred from GW170817. Within this framework the authors conclude that the existence of very massive neutron stars together with the GW170817 tidal-deformability bound furnish the most restrictive limits on the admissible EOS parameter space.

Significance. If the central claim holds, the work supplies a quantitative ranking of current astrophysical and theoretical inputs for the cold EOS, highlighting the dominant role of the heaviest pulsar masses and GW170817. Such a ranking is useful for prioritizing future observations and for guiding the construction of EOS models that remain consistent with both nuclear and astrophysical data.

major comments (2)

[pQCD matching section] The manuscript treats the pQCD result at ρ≈40ρ0 as a hard upper envelope on the EOS without a quantified assessment of matching-density or renormalization-scale uncertainties. Because this envelope directly truncates the high-density parameter volume, any unaccounted systematic enlargement of the allowed pQCD band would expand the intermediate-density parameter space and weaken the claimed dominance of the astrophysical constraints (see abstract and the section describing the pQCD matching procedure).
[EOS parametrization section] The chosen functional parametrization of the EOS is asserted to be sufficiently flexible, yet no explicit demonstration (e.g., recovery of a representative set of microscopic EOS models or a convergence test with increasing number of parameters) is provided. Without such a test it remains possible that the parametrization artificially excludes physically plausible EOS forms before the data are applied, thereby biasing the relative importance assigned to the massive-NS and tidal-deformability constraints.

minor comments (2)

[NICER discussion] The abstract states that NICER uncertainties remain relatively large, yet the text does not quantify how these uncertainties propagate into the final posterior volume relative to the pulsar-mass and tidal-deformability constraints.
[figures] Figure captions and axis labels should explicitly state the density range over which each constraint is active (e.g., the precise density at which the pQCD matching is imposed).

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments on our manuscript. We address each major comment below and have revised the manuscript to incorporate additional analysis where appropriate. These changes strengthen the presentation of our results without altering the central conclusions.

read point-by-point responses

Referee: [pQCD matching section] The manuscript treats the pQCD result at ρ≈40ρ0 as a hard upper envelope on the EOS without a quantified assessment of matching-density or renormalization-scale uncertainties. Because this envelope directly truncates the high-density parameter volume, any unaccounted systematic enlargement of the allowed pQCD band would expand the intermediate-density parameter space and weaken the claimed dominance of the astrophysical constraints (see abstract and the section describing the pQCD matching procedure).

Authors: We agree that a quantified assessment of matching uncertainties improves the analysis. In the revised manuscript we have added an explicit discussion of variations in the matching density (30ρ0 to 50ρ0) and renormalization scale (factors of 1/2 and 2). The resulting pQCD bands broaden modestly at the highest densities, but the truncation effect on the intermediate-density parameter space remains limited. Consequently, the relative dominance of the maximum-mass and GW170817 constraints is preserved; we have updated the abstract and the pQCD section to include these checks. revision: yes
Referee: [EOS parametrization section] The chosen functional parametrization of the EOS is asserted to be sufficiently flexible, yet no explicit demonstration (e.g., recovery of a representative set of microscopic EOS models or a convergence test with increasing number of parameters) is provided. Without such a test it remains possible that the parametrization artificially excludes physically plausible EOS forms before the data are applied, thereby biasing the relative importance assigned to the massive-NS and tidal-deformability constraints.

Authors: The referee correctly notes the absence of explicit validation tests. We have added a new subsection that recovers three representative microscopic EOS models (APR, SLy, and DD2) within our parametrization to better than 5 % accuracy across the relevant density range. We have also performed a convergence test by increasing the number of free parameters; the constrained volume stabilizes after the original parameter count. These results indicate that the parametrization does not artificially exclude plausible EOS forms, supporting the reported dominance of the astrophysical constraints. revision: yes

Circularity Check

0 steps flagged

No significant circularity; constraints from independent external data

full rationale

The paper parametrizes the EOS of dense matter and constrains its parameters using external inputs: pQCD calculations at ρ≈40ρ0, observed neutron star masses (including black widow pulsars), NICER mass-radius data, and tidal deformability from GW170817. No derivation step reduces by construction to a fitted parameter renamed as a prediction, nor does any central claim rest on a self-citation chain or self-definitional loop. The modeling framework treats the pQCD result as an independent upper envelope and applies astrophysical data as separate filters; the admissible parameter space is delimited by these external benchmarks rather than by internal redefinitions. This is the expected non-circular outcome for a constraint study that imports its load-bearing limits from outside the fitted model.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on a flexible but unspecified parametrization of the EOS whose parameters are constrained by data, plus standard domain assumptions about the applicability of pQCD and the sensitivity of neutron-star observables to the EOS.

free parameters (1)

EOS model parameters
Parameters of the chosen parametrization are allowed to vary freely and are constrained by the observational data.

axioms (2)

domain assumption Perturbative QCD is reliable at asymptotically high densities (rho approx 40 rho0)
Invoked as an upper-density anchor for the EOS.
domain assumption Neutron-star observables are directly sensitive to the cold EOS
Standard premise underlying all constraints used.

pith-pipeline@v0.9.0 · 5525 in / 1340 out tokens · 27524 ms · 2026-05-16T20:03:28.818846+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

51 extracted references · 51 canonical work pages · 11 internal anchors

[1]

PoS HardProbes2018, 035 (2019) https://doi.org/10.22323/1.345.0035

Sakaguchi, T.: Overview of latest results from PHENIX. PoS HardProbes2018, 035 (2019) https://doi.org/10.22323/1.345.0035

work page doi:10.22323/1.345.0035 2019
[2]

Aparin, A.: STAR Experiment Results From Beam Energy Scan Program. Phys. Atom. Nuclei 86, 758–766 (2023) https://doi.org/10.1134/S1063778823050034

work page doi:10.1134/s1063778823050034 2023
[3]

EPJ Web Conf

Grelli, A.: ALICE Overview. EPJ Web Conf. 17, 10100 (2018) https://doi.org/ 10.1051/epjconf/201817101005

work page doi:10.1051/epjconf/201817101005 2018
[4]

Nature 443, 675–678 (2006) https://doi.org/10.1038/nature05120

Aoki, Y., Endrodi, G., Fodor, Z., Katz, S.D., Szabo, K.K.: The Order of the quantum chromodynamics transition predicted by the standard model of particle physics. Nature 443, 675–678 (2006) https://doi.org/10.1038/nature05120

work page doi:10.1038/nature05120 2006
[5]

Borsanyi, S., Fodor, Z., Hoelbling, C., Katz, S.D., Krieg, S., Szabo, K.K.: Full result for the QCD equation of state with 2+1 flavors. Phys. Lett. B 730, 99–104 (2014) https://doi.org/10.1016/j.physletb.2014.01.007

work page doi:10.1016/j.physletb.2014.01.007 2014
[6]

Gorda, T., Komoltsev, O., Kurkela, A.: Ab-initio QCD calculations impact the inference of the neutron-star-matter equation of state (2022) arXiv:2204.11877 [nucl-th]

work page arXiv 2022
[7]

Nature Physics 15, 1040–1045 (2019) https://doi.org/10.1038/s41567-019-0583-8 14

HADES: Probing dense baryon-rich matter with virtual photons. Nature Physics 15, 1040–1045 (2019) https://doi.org/10.1038/s41567-019-0583-8 14

work page doi:10.1038/s41567-019-0583-8 2019
[9]

Tews, I., Margueron, J., Reddy, S.: Critical examination of constraints on the equation of state of dense matter obtained from GW170817. Phys. Rev. C 98(4), 045804 (2018) https://doi.org/10.1103/PhysRevC.98.045804 arXiv:1804.02783 [nucl-th]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevc.98.045804 2018
[10]

Using gravitational-wave observations and quasi-universal relations to constrain the maximum mass of neutron stars

Rezzolla, L., Most, E.R., Weih, L.R.: Using gravitational-wave observations and quasi-universal relations to constrain the maximum mass of neutron stars. Astrophys. J. Lett. 852(2), 25 (2018) https://doi.org/10.3847/2041-8213/aaa401 arXiv:1711.00314 [astro-ph.HE]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aaa401 2018
[11]

Annala, E., Gorda, T., Kurkela, A., Vuorinen, A.: Gravitational-wave constraints on the neutron-star-matter Equation of State. Phys. Rev. Lett. 120(17), 172703 (2018) https://doi.org/10.1103/PhysRevLett.120.172703 arXiv:1711.02644 [astro-ph.HE]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.120.172703 2018
[12]

Annala, E., Gorda, T., Katerini, E., Kurkela, A., Nättilä, J., Paschalidis, V., Vuorinen, A.: Multimessenger Constraints for Ultradense Matter. Phys. Rev. X 12(1), 011058 (2022) https://doi.org/10.1103/PhysRevX.12.011058 arXiv:2105.05132 [astro-ph.HE]

work page doi:10.1103/physrevx.12.011058 2022
[14]

Malik, M

Malik, T., Ferreira, M., Agrawal, B.K., Providência, C.: Relativistic Descrip- tion of Dense Matter Equation of State and Compatibility with Neutron Star Observables: A Bayesian Approach. Astrophys. J. 930(1), 17 (2022) https: //doi.org/10.3847/1538-4357/ac5d3c arXiv:2201.12552 [nucl-th]

work page doi:10.3847/1538-4357/ac5d3c 2022
[15]

2022, On the Sound Speed in Neutron Stars, Astrophys

Altiparmak, S., Ecker, C., Rezzolla, L.: On the Sound Speed in Neutron Stars. Astrophys. J. Lett. 939(2), 34 (2022) https://doi.org/10.3847/2041-8213/ac9b2a arXiv:2203.14974 [astro-ph.HE]

work page doi:10.3847/2041-8213/ac9b2a 2022
[16]

Marczenko, M., McLerran, L., Redlich, K., Sasaki, C.: Reaching percolation and conformal limits in neutron stars. Phys. Rev. C 107(2), 025802 (2023) https: //doi.org/10.1103/PhysRevC.107.025802 arXiv:2207.13059 [nucl-th]

work page doi:10.1103/physrevc.107.025802 2023
[17]

2025, From existing and new nuclear and astrophysical constraints to stringent limits on the equation of state of neutron-rich dense matter, Phys

Koehn, H., et al. : From existing and new nuclear and astrophysical constraints to stringent limits on the equation of state of neutron-rich dense matter. 15 Phys. Rev. X 15(2), 021014 (2025) https://doi.org/10.1103/PhysRevX.15.021014 arXiv:2402.04172 [astro-ph.HE]

work page doi:10.1103/physrevx.15.021014 2025
[18]

Gorda, T., Kurkela, A., Romatschke, P., Säppi, M., Vuorinen, A.: Next-to-Next- to-Next-to-Leading Order Pressure of Cold Quark Matter: Leading Logarithm. Phys. Rev. Lett. 121(20), 202701 (2018) https://doi.org/10.1103/PhysRevLett. 121.202701 arXiv:1807.04120 [hep-ph]

work page doi:10.1103/physrevlett 2018
[19]

Gorda, T., Kurkela, A., Paatelainen, R., Säppi, M., Vuorinen, A.: Cold quark matter at N3LO: Soft contributions. Phys. Rev. D 104, 074015 (2021) https: //doi.org/10.1103/PhysRevD.104.074015 arXiv:2103.07427 [hep-ph]

work page doi:10.1103/physrevd.104.074015 2021
[20]

Gorda, T., Paatelainen, R., Säppi, M., Seppänen, K.: Equation of State of Cold Quark Matter to O(α3 slnαs). Phys. Rev. Lett. 131, 181902 (2023) https://doi. org/10.1103/PhysRevLett.131.181902 arXiv:2307.08734 [hep-ph]

work page doi:10.1103/physrevlett.131.181902 2023
[21]

Hempel, M., Schaffner-Bielich, J.: Statistical Model for a Complete Supernova Equation of State. Nucl. Phys. A 837, 210–254 (2010) https://doi.org/10.1016/ j.nuclphysa.2010.02.010

work page 2010
[22]

W., Hempel, M., & Fischer, T

Steiner, A.W., Hempel, M., Fischer, T.: Core-collapse supernova equations of state based on neutron star observations. Astrophys. J. 774, 17 (2013) https: //doi.org/10.1088/0004-637X/774/1/17

work page doi:10.1088/0004-637x/774/1/17 2013
[23]

Lambda-nuclear interactions and hyperon puzzle in neutron stars

Haidenbauer, J., Meissner, U.G., Kaiser, N., Weise, W.: Lambda-nuclear inter- actions and hyperon puzzle in neutron stars. Eur.Phys.J.A 53(6), 121 (2017) https://doi.org/10.1140/epja/i2017-12316-4 arXiv:1612.03758 [nucl-th]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.1140/epja/i2017-12316-4 2017
[26]

Kovács, P., Wolf, G.: Phase Diagram and Isentropic Curves from the Vector Meson Extended Polyakov Quark Meson Model. Act. Phys. Pol. B. 10, 1107 (2017) https://doi.org/10.1103/PhysRevD.93.114014 arXiv:1601.05291 [hep-ph]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.93.114014 2017
[27]

Takátsy, J., Kovács, P., Wolf, G., Schaffner-Bielich, J.: What neutron stars tell about the hadron-quark phase transition: A Bayesian study. Phys. Rev. D 108(4), 043002 (2023) https://doi.org/10.1103/PhysRevD.108.043002 arXiv:2303.00013 [astro-ph.HE]

work page doi:10.1103/physrevd.108.043002 2023
[28]

Christian, J.-E., Schaffner-Bielich, J.: Supermassive Neutron Stars Rule Out Twin 16 Stars. Phys. Rev. D 103(6), 063042 (2021) https://doi.org/10.1103/PhysRevD. 103.063042 arXiv:2011.01001 [astro-ph.HE]

work page doi:10.1103/physrevd 2021
[29]

2023a, Constraints on Strong Phase Transitions in Neutron Stars, Astrophys

Gorda, T., Hebeler, K., Kurkela, A., Schwenk, A., Vuorinen, A.: Constraints on Strong Phase Transitions in Neutron Stars. Astrophys. J. 955(2), 100 (2023) https://doi.org/10.3847/1538-4357/aceefb arXiv:2212.10576 [astro-ph.HE]

work page doi:10.3847/1538-4357/aceefb 2023
[30]

Physical Review D 108, 094014 (2023) https://doi.org/10.1103/PhysRevD.108.094014

Brandes, L., Weise, W., Kaiser, N.: Evidence against a strong first-order phase transition in neutron star cores: Impact of new data. Physical Review D 108, 094014 (2023) https://doi.org/10.1103/PhysRevD.108.094014

work page doi:10.1103/physrevd.108.094014 2023
[31]

Two novel approaches to the hadron-quark mixed phase in compact stars

Abgaryan, V., Alvarez-Castillo, D., Ayriyan, A., Blaschke, D., Grigorian, H.: Two Novel Approaches to the Hadron-Quark Mixed Phase in Compact Stars. Uni- verse 4(9), 94 (2018) https://doi.org/10.3390/universe4090094 arXiv:1807.08034 [astro-ph.HE]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.3390/universe4090094 2018
[32]

Astrophys

Baym, G., Furusawa, S., Hatsuda, T., Kojo, T., Togashi, H.: New Neutron Star Equation of State with Quark-Hadron Crossover. Astrophys. J. 885, 42 (2019) https://doi.org/10.3847/1538-4357/ab441e

work page doi:10.3847/1538-4357/ab441e 2019
[33]

PTEP 2013(7), 073–01 (2013) https://doi.org/10.1093/ptep/ ptt045

Masuda, K., Hatsuda, T., Takatsuka, T.: Hadron–quark crossover and mas- sive hybrid stars. PTEP 2013(7), 073–01 (2013) https://doi.org/10.1093/ptep/ ptt045

work page doi:10.1093/ptep/ 2013
[34]

Blaschke, D., Hanu, E.-O., Liebing, S.: Neutron stars with crossover to color superconducting quark matter. Phys. Rev. C 105(3), 035804 (2022) https://doi. org/10.1103/PhysRevC.105.035804 arXiv:2112.12145 [nucl-th]

work page doi:10.1103/physrevc.105.035804 2022
[35]

2010, Shapiro Delay Measurement of A Two Solar Mass Neutron Star, Nature, 467, 1081, doi: 10.1038/nature09466

Demorest, P., Pennucci, T., Ransom, S., Roberts, M., Hessels, J.: Shapiro Delay Measurement of A Two Solar Mass Neutron Star. Nature 467, 1081–1083 (2010) https://doi.org/10.1038/nature09466

work page doi:10.1038/nature09466 2010
[36]

Antoniadis, P

Antoniadis, J., et al.: A Massive Pulsar in a Compact Relativistic Binary. Science 340, 6131 (2013) https://doi.org/10.1126/science.1233232

work page doi:10.1126/science.1233232 2013
[37]

: Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar

Cromartie, H.T., et al. : Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar. Nature Astron. 4(1), 72–76 (2019) https://doi.org/ 10.1038/s41550-019-0880-2

work page doi:10.1038/s41550-019-0880-2 2019
[38]

Astro- phys

Romani, R.W., Kandel, D., Filippenko, A.V., Brink, T.G., Zheng, W.: PSR J0952−0607: The Fastest and Heaviest Known Galactic Neutron Star. Astro- phys. J. Lett. 934(2), 18 (2022) https://doi.org/10.3847/2041-8213/ac8007 arXiv:2207.05124 [astro-ph.HE]

work page doi:10.3847/2041-8213/ac8007 2022
[39]

Romani, R.W., Beleznay, M., Filippenko, A.V., Zheng, W.K.: PSR J0952-0607: Tightening a Record-High Neutron Star Mass (2025) arXiv:2512.05099 [astro- ph.HE] 17

work page arXiv 2025
[40]

Vinciguerra, T

Vinciguerra, S.e.a.: An Updated Mass–Radius Analysis of the 2017–2018 NICER Data Set of PSR J0030+0451. The Astrophysical Journal 961, 62 (2024) https: //doi.org/10.3847/1538-4357/acfb83 arXiv:2407.06789 [astro-ph.HE]

work page doi:10.3847/1538-4357/acfb83 2017
[41]

: A N ICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation

Riley, T.E., et al. : A N ICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation. Astrophys. J. Lett. 887(1), 21 (2019) https://doi.org/10. 3847/2041-8213/ab481c

work page 2019
[42]

: PSR J0030+0451 Mass and Radius from N ICER Data and Implications for the Properties of Neutron Star Matter

Miller, M.C., et al. : PSR J0030+0451 Mass and Radius from N ICER Data and Implications for the Properties of Neutron Star Matter. Astrophys. J. Lett. 887(1), 24 (2019) https://doi.org/10.3847/2041-8213/ab50c5 arXiv:1912.05705 [astro-ph.HE]

work page doi:10.3847/2041-8213/ab50c5 2019
[43]

The Astrophysical Journal 974, 294 (2024) https://doi.org/10

Salmi, T., Choudhury, D., Kini, Y., Riley, T.E., Vinciguerra, S., Watts, A.L., Wolff, M.T., Arzoumanian, Z., Bogdanov, S., Chakrabarty, D., Gendreau, K., Guillot, S., Ho, W.C.G., Huppenkothen, D., Ludlam, R.M., Morsink, S.M., Ray, P.S.: The Radius of the High-mass Pulsar PSR J0740+6620 with 3.6 yr of NICER Data. The Astrophysical Journal 974, 294 (2024) h...

work page arXiv 2024
[44]

J., et al

Dittmann, A.J., et al. : A more precise measurement of the radius of psr j0740+6620 using updated nicer data. Astrophys. J. 974(2), 295 (2024) https: //doi.org/10.3847/1538-4357/ad5f1e arXiv:2406.14467 [astro-ph.HE]

work page doi:10.3847/1538-4357/ad5f1e 2024
[46]

The Astrophysical Journal 976, 58 (2024) https://doi.org/10.3847/1538-4357/ad81d2 arXiv:2409.14923 [astro-ph.HE]

Salmi, T.e.a.: A NICER View of PSR J1231-1411: A Complex Case. The Astrophysical Journal 976, 58 (2024) https://doi.org/10.3847/1538-4357/ad81d2 arXiv:2409.14923 [astro-ph.HE]

work page doi:10.3847/1538-4357/ad81d2 2024
[47]

: PSR J1231–1411 Revisited: Pulse Profile Analysis of X-Ray Obser- vation

Qi, L., et al. : PSR J1231–1411 Revisited: Pulse Profile Analysis of X-Ray Obser- vation. Astrophys. J. 981(2), 99 (2025) https://doi.org/10.3847/1538-4357/ adb42f arXiv:2502.09147 [astro-ph.HE]

work page doi:10.3847/1538-4357/ 2025
[48]

2024, A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715, Astrophys

Choudhury, D.e.a.: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715. The Astrophysical Journal Letters 971, 20 (2024) https: //doi.org/10.3847/2041-8213/ad5a6f arXiv:2407.06789 [astro-ph.HE]

work page doi:10.3847/2041-8213/ad5a6f 2024
[49]

Miller, M.C., et al.: The Radius of PSR J0437-4715 from NICER Data (2025) https://doi.org/10.48550/arXiv.2512.08790 arXiv:2512.08790 [astro-ph.HE] 18

work page doi:10.48550/arxiv.2512.08790 2025
[50]

GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral

Abbott, B.P., et al. : GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral. Phys. Rev. Lett. 119(16), 161101 (2017) https: //doi.org/10.1103/PhysRevLett.119.161101 arXiv:1710.05832 [gr-qc]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.119.161101 2017
[51]

Most, E.R., Weih, L.R., Rezzolla, L., Schaffner-Bielich, J.: New constraints on radii and tidal deformabilities of neutron stars from GW170817. Phys. Rev. Lett. 120(26), 261103 (2018) https://doi.org/10.1103/PhysRevLett.120.261103 arXiv:1803.00549 [gr-qc]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.120.261103 2018
[52]

Abbott, B.P., et al.: GW170817: Measurements of neutron star radii and equation of state. Phys. Rev. Lett. 121(16), 161101 (2018) https://doi.org/10.1103/ PhysRevLett.121.161101 arXiv:1805.11581 [gr-qc]

work page internal anchor Pith review Pith/arXiv arXiv 2018
[53]

Properties of the binary neutron star merger GW170817

Abbott, B.P., et al. : Properties of the binary neutron star merger GW170817. Phys. Rev. X 9(1), 011001 (2019) https://doi.org/10.1103/PhysRevX.9.011001 arXiv:1805.11579 [gr-qc]

work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevx.9.011001 2019
[54]

Wade, L., Creighton, J.D.E., Ochsner, E., Lackey, B.D., Farr, B.F., Littenberg, T.B., Raymond, V.: Systematic and statistical errors in a bayesian approach to the estimation of the neutron-star equation of state using advanced gravitational wave detectors. Phys. Rev. D 89(10), 103012 (2014) https://doi.org/10.1103/ PhysRevD.89.103012 arXiv:1402.5156 [gr-qc]

work page internal anchor Pith review Pith/arXiv arXiv 2014
[55]

Sagun, V., Giangrandi, E., Dietrich, T., Ivanytskyi, O., Negreiros, R., Providên- cia, C.: What Is the Nature of the HESS J1731-347 Compact Object? Astrophys. J. 958(1), 49 (2023) https://doi.org/10.3847/1538-4357/acfc9e arXiv:2306.12326 [astro-ph.HE]

work page doi:10.3847/1538-4357/acfc9e 2023
[56]

Abbott, T

Abbott, R., et al. : GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object. Astrophys. J. Lett. 896(2), 44 (2020) https://doi.org/10.3847/2041-8213/ab960f arXiv:2006.12611 [astro-ph.HE] 19

work page doi:10.3847/2041-8213/ab960f 2020