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REVIEW 4 major objections 5 minor 45 references

Cooling of neutron stars in soft X-ray transients with realistic crust composition

T0 review · 4 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read The new nHD-equilibrium crust models fit observed transient cooling as well as the traditional model, and both require unexplained extras (shallow heating and reduced conductivity) to match the data.

desk verdict Careful consolidation: SGC crust models behave like traditional ones and still need shallow heating; the imported nHD assumption is the load-bearing caveat. read the letter →

arxiv 2411.14395 v1 pith:2TLPHGTV submitted 2024-11-21 astro-ph.HE

A. Y. Potekhin , A. I. Chugunov , N. N. Shchechilin , M. E. Gusakov This is my paper · ORCID
classification astro-ph.HE
keywords neutronstarsdensemattersoftX-raytransientscrustcoolingaccretedstarnHDequilibriumshallowheatingthermalconductivity
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

Soft X-ray transients are neutron stars that are episodically heated by accretion and then cool in quiescence; their cooling curves are one of the few direct probes of the structure and composition of the neutron-star crust. This paper tests whether a new family of accreted-crust models, built on the assumption that free neutrons diffuse into hydrostatic and diffusion equilibrium during accretion, can reproduce the observed post-outburst cooling of the two best-monitored sources, MXB 1659-29 and IGR J17480-2446. The result is that the new models and the traditional 2018 model are similar in their ability to fit the data: the new models still need an extra shallow heating source to explain MXB 1659-29, and they still need a strongly suppressed thermal conductivity in a thin outer-crust layer to explain the slow cooling of IGR J17480-2446. If the paper is right, the cooling observations currently in hand do not distinguish between the two crust-model families, and the extra physics those observations demand is real and still unidentified.

What carries the argument

The load-bearing construction is the nHD equilibrium condition: during accretion, free neutrons in the inner crust redistribute by diffusion until the crust reaches hydrostatic and diffusion equilibrium. This condition fixes the composition, the impurity parameter Qimp (the charge variance that scatters electrons and reduces thermal conductivity), and the heat released per accreted baryon, so these inputs are no longer free parameters but outputs of a nuclear reaction-network calculation. The paper combines three nHD-based crust models, corresponding to three representative thermonuclear ash compositions, with analytical fits for the inner-crust equation of state and a stellar thermal-evolution code, and compares the resulting cooling curves with the observed light curves of the two transients. The nHD assumption is the essential difference from the traditional model, in which free neutrons are assumed to move together with the nuclei.

What would settle it

One decisive test is a nuclear-physics estimate of the diffusion coefficient of free neutrons in the inner crust at densities of order $10^{11}$ to $10^{12}$ g/$cm^{3}$; if the resulting equilibration time is longer than a typical accretion outburst, the nHD equilibrium condition on which all the new models rest is not satisfied, and the paper's comparison would no longer test a physically realized crust.

Watch

Extended reading notes

Core claim

The paper's central finding is a comparison rather than a new mechanism: when the three new nHD-equilibrium crust models (the paper's K, RP, and SB ash versions) are used to simulate the same two transients, their cooling curves fall in the same range as those of the traditional 2018 model. For MXB 1659-29, the SB version with the lowest allowed outer-inner crust pressure matches the observed light curves if a shallow heating source of about 0.85 MeV per baryon is added; the K and RP versions cool too slowly because their impurity parameter is large, and thus do not fit. For IGR J17480-2446, none of the new models matches the observed slow cooling unless a layer near the bottom of the outer crust is treated as amorphous, with the thermal conductivity suppressed to the level of independent ion scattering. The total deep crustal heating in the new models is only about 0.2-0.6 MeV per accreted baryon, compared to about 1.5-2 MeV in the traditional model, yet the extra ingredients required to fit observations are the same for both families.

Load-bearing premise

The new models all assume that free neutrons diffuse rapidly enough in the inner crust during accretion to reach hydrostatic and diffusion equilibrium; if that diffusion is too slow, the predicted compositions, impurity parameters, and heating profiles do not apply.

Editorial extensions

If this is right

  • If the paper's result holds, the Superburst-ash nHD model can describe the MXB 1659-29 cooling data, but only with an added shallow heating of roughly 0.85 MeV per accreted baryon.
  • The K and RP versions of the new models are disfavored for MXB 1659-29 because their high impurity parameter makes the crust cool too slowly.
  • For IGR J17480-2446, the new models predict faster cooling than observed unless a layer near the bottom of the outer crust is assigned a strongly suppressed thermal conductivity, modeled as an amorphous solid.
  • The observed cooling therefore does not yet choose between the new nHD-equilibrium crust models and the traditional model; both need the same kinds of extra physics.
  • The much smaller deep crustal heating in the new models (about 0.2-0.6 MeV per baryon versus 1.5-2 MeV) does not, by itself, break the degeneracy, because the required shallow heating compensates in the quasi-steady quiescent state.

Reading between the lines

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

  • Beyond the paper, the fitted 'shallow heating' energy of about 0.85-1 MeV per baryon is comparable in size to the deep crustal heating itself, which suggests that whatever mechanism produces it, possibly nuclear reactions in the outer envelope rather than crust physics, is a first-order ingredient for all future transient-cooling fits.
  • The paper's need for a low-conductivity layer in one source but not the other hints that the conductivity suppression may be source-dependent, perhaps tied to accretion history or magnetic field; that is testable by extending the same fits to other transients with well-measured cooling curves.
  • A Bayesian model-comparison over a larger sample of transients could quantify how strongly the data prefer the new nHD-equilibrium models over the traditional model, something the two-source comparison here leaves open.
  • If the nHD equilibrium is correct, then the extra 'shallow heating' term may be absorbing a real deficit in the deep crustal heating of the new models; resolving that would require a microphysical calculation rather than further tuning of the heating parameter.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 5 minor

Summary. The paper simulates the thermal evolution of the neutron stars in two soft X-ray transients, MXB 1659-29 and IGR J17480-2446, using the new SGC family of accreted-crust models based on realistic thermonuclear ash compositions and the nHD equilibrium condition, and compares the resulting cooling curves with those of the traditional Fantina et al. (2018) (F+18) model and with observed post-outburst temperatures. The main finding is that the SGC models, in particular the Superburst (SB) ash variant, can reproduce the MXB 1659-29 cooling curves only after introducing a shallow-heating source, while all SGC variants require an additional low-conductivity amorphous layer to reproduce IGR J17480-2446. The authors conclude that the new and traditional crust models are similar in their explanatory power and that both need extra ingredients beyond the current deep-crustal-heating theory.

Significance. If the conclusions hold, the paper is a valuable calibration result: it shows that the thermodynamically consistent SGC crust models, despite their more realistic composition and heating profiles, do not remove the long-standing need for shallow heating and for a strongly reduced thermal conductivity in some sources. This is important for future attempts to use crust-cooling observations to constrain dense-matter microphysics, because it narrows the space of model predictions that can be tested against data. The paper also reduces the number of free parameters by taking the impurity parameter Qimp and composition directly from the SGC tables, and it makes the adopted crust tables publicly available, which is a useful contribution. The significance is limited, however, because the key comparisons depend on several fitted quantities (Esh, the outburst-II accretion rate, and the location of the amorphous layer) and because the nHD equilibrium condition underlying all SGC models is imported without an independent test in this manuscript.

major comments (4)
  1. [Sections 1 and 2] The entire SGC family of crust models rests on the nHD equilibrium condition, which assumes that free neutrons in the inner crust diffuse on timescales shorter than the accretion residence time so that the composition, Qimp, and heating profile follow the Gusakov-Chugunov and Shchechilin et al. calculations. The present paper adopts this condition without evaluating its kinetic feasibility. If neutron diffusion is suppressed on accretion timescales, the SGC composition and heating tables describe an unphysical crust, and the comparison in Figs. 3, 5, and 6 would not be a test of the claimed new-model content. Please add a quantitative justification, either an order-of-magnitude estimate of the neutron diffusion timescale versus the advection timescale or a reference to a direct calculation, and state how the conclusions would change if diffusion is slow.
  2. [Section 3.1, Fig. 3] The paper states that Esh is adjusted so that each simulated light curve matches the first observation after outburst I, and that Mdot_II is chosen as the value providing the best fits after outburst II. Consequently, the agreement of the SB and F+18 curves with the data is not a parameter-free prediction of the models; it is a test of the shape of the cooling curve after normalizing to one point. This does not by itself invalidate the conclusion that shallow heating is required, but the comparison between model families is weaker than the text implies. Please quantify the sensitivity of the conclusions to the fitted values, for example by showing the range of Esh and Mdot_II that is consistent with the data, and indicate whether the relative ranking of the models is robust within those ranges.
  3. [Section 3.2, Fig. 6] The amorphous layer for IGR J17480-2446 is introduced with an assumed structure factor S=1 (Qimp=<Z>^2) and its location between about 3e10 and 3e11 g cm^-3 is chosen to minimize the discrepancy with the observed cooling curve. This is a genuinely new ad hoc ingredient, and its position is a fitted parameter. The conclusion that the SGC models require a strong conductivity reduction is therefore conditional on this placement and on the independent-scatterer model. Please either provide a physical argument for why an amorphous layer should appear preferentially at that density or show that the inferred need for reduced conductivity is insensitive to moving the layer within a plausible range.
  4. [Section 3.1 and Conclusions] The central claim that 'SGC models are similar to traditional models' is based mainly on the SB ash variant: the K and RP variants are found to be incompatible with the MXB 1659-29 observations (Fig. 3 and the discussion in Section 3.1). Since the three ash models are presented as representative rather than as a weighted set, the conclusion generalizes from one member of the SGC family. Please discuss whether the ash composition appropriate for MXB 1659-29 can be constrained independently, and whether the similarity conclusion would survive if K or RP were the correct ashes for this source.
minor comments (5)
  1. [Section 3.1] The adopted accretion rate during outburst II is given as Mdot_II = 1.8e-9 M_sun/yr, but no uncertainty is quoted; given that this value is fitted to the cooling data, an error estimate would help the reader judge the significance of the agreement in the right panel of Fig. 3.
  2. [Figure 3 caption] The legend uses subscripts on GC, K, RP, and SB to denote Poi values, but the subscript values are small and hard to read in a printed figure; please enlarge the legend fonts or list the Poi values explicitly in the caption.
  3. [Figure 6 caption] There is a typo: 'vertical doted lines' should read 'vertical dotted lines'.
  4. [Section 4, first paragraph] The phrase 'unlike the past analyses, which treated ... Qimp as free ... fitting parameter' is slightly overstated, because in the present analysis the location and extent of the amorphous layer for IGR J17480-2446 are still effectively free parameters; please rephrase to distinguish the treatment of Qimp from the new fitted layer parameters.
  5. [Appendix A] The fitting formulas for P(rho), rho(P), and Ynf are useful, but the paper does not state the accuracy of the Ynf fit in the extrapolated region rho > rho_max; a sentence on the expected uncertainty of the extrapolation would be helpful.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the SGC-model comparison is tested against independent observations, and the fitted shallow-heating parameter does not reduce the central claim to the model inputs.

full rationale

The paper's central conclusion—that the SGC and traditional (F+18) crust models are similar in their ability to explain SXT cooling and both require extra ingredients—is not equivalent to its inputs. The SGC crust compositions, Qimp, and heating profiles are adopted as fixed model inputs from the authors' prior work (Gusakov & Chugunov 2020, 2021; Shchechilin et al. 2021-2023), and the F+18 model is an independent traditional calculation; the thermal evolution is then computed with a simulation code and compared with external observational data for MXB 1659-29 and IGR J17480-2446. The shallow-heating energy Esh is calibrated to the first post-outburst observation in each source, but the subsequent cooling curves are genuine predictions of the calibrated model, and the finding that both model families need shallow heating or conductivity suppression is an empirical residual inference rather than a quantity defined by the fit. The nHD equilibrium condition is imported from prior self-cited work and is an untested physical assumption; even if it fails, that would undermine the realism of the SGC models (a correctness/fragility concern), not make the paper's comparison circular. The self-citations to Paper I and GC/SGC are standard uses of prior results with stated assumptions and do not supply the conclusion by construction.

Assumptions & free parameters 4 free parameters · 5 assumptions · 2 invented entities

The central claim rests on the SGC crust models (prior work by the same group), on standard deep crustal heating, and on two ad hoc ingredients: shallow heating (Esh fitted) and, for IGR, an amorphous low-conductivity layer. The number of genuinely free parameters is moderate, and the comparison with observations uses them explicitly.

free parameters (4)
  • Esh (shallow heating energy per accreted baryon) = 0.85 MeV (SB), 1 MeV (F+18), varied for K and RP models
    Adjusted so the simulated light curve matches the first observed cooling point after outburst I of MXB 1659-29; Section 3.1.
  • Poi (pressure at outer-inner crust interface) = 6.4e29 to 1e30 dyn/cm2; P(0)_oi values 7.26, 7.75, 7.29 x 10^29 dyn/cm2 for K, RP, SB
    Free parameter in SGC models, varied across the allowed range; it controls composition, Qimp, and heating layer positions; Section 2.
  • Accretion rate during outburst II of MXB 1659-29 (Mdot_II) = 1.8e-9 Msun/yr
    Adopted constant rate chosen to provide best fits of cooling curves after outburst II; Section 3.1.
  • Amorphous layer location and extent for IGR J17480-2446 = 3e10 to 3e11 g/cm3
    Placed near the bottom of the outer crust to minimize discrepancy; other placements did not give acceptable agreement; Section 3.2.
assumptions (5)
  • domain assumption Deep crustal heating scenario: nuclear reactions during accretion deposit heat in the crust, and quiescent thermal emission is powered by its relaxation.
    Standard framework used throughout, stated in Section 1.
  • domain assumption nHD equilibrium: free neutrons in the inner crust diffuse to hydrostatic and diffusion equilibrium during accretion.
    Basis of SGC models, cited from Gusakov and Chugunov (2020, 2021) in Section 1.
  • domain assumption BSk24 EoS is valid for core and for deep crust beyond rho_max = 2e12 g/cm3.
    Used to extend SGC EoS with a pressure shift; Section 2 and Appendix A.
  • domain assumption Mean ion approximation with <Z>, <A>, Qimp adequately represents thermal conductivity and neutrino emissivity.
    Stated in Section 2.
  • ad hoc to paper A layer of amorphous crust with structure factor S = 1 (Qimp = <Z>^2) models strongly suppressed conductivity.
    Introduced in Section 3.2 for IGR J17480-2446, with location chosen to fit observations.
invented entities (2)
  • Shallow heating source
    purpose: Extra heat deposited at low densities to match early cooling observations.
    Not supplied by current crust models; energy Esh is fitted to the first cooling point; Section 3.1.
  • Amorphous (glassy) crust layer
    purpose: Layer with strongly suppressed thermal conductivity to slow the cooling of IGR J17480-2446.
    Postulated structural disorder, modeled by Qimp=<Z>^2; no independent measurement; Section 3.2.

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Pith. "Pith review of Cooling of neutron stars in soft X-ray transients with realistic crust composition." pith.science (2026). https://pith.science/paper/2TLPHGTV

@misc{pith2026241114395,
  author       = {Pith},
  title        = {Pith review of: Cooling of neutron stars in soft X-ray transients with realistic crust composition},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2TLPHGTV}},
  note         = {Machine review of arXiv:2411.14395}
}
read the original abstract

Thermal radiation of neutron stars in soft X-ray transients (SXTs) in a quiescent state is believed to be powered by the heat deposited in the stellar crust due to nuclear reactions during accretion. Confronting observations of this radiation with simulations helps to verify theoretical models of the dense matter in neutron stars. We simulate the thermal evolution of the SXTs with theoretical models of the equation of state and composition of the accreted crust. The new family of such models were recently developed within a thermodynamically consistent approach by modeling the nuclear evolution of an accreted matter as it sinks toward the stellar center, starting from representative thermonuclear ash compositions. The crust cooling curves computed with the traditional and modern theory are compared with observations of SXTs MXB 1659-29 and IGR J17480-2446. We show that the new and traditional models of the accreted neutron star crusts are similar in their capability to explain the thermal evolution of neutron stars in SXTs. Both kinds of models require inclusion of additional ingredients not supplied by the current theory, such as the shallow heating and variation of thermal conductivity, to fit observations.

Figures

Figures reproduced from arXiv: 2411.14395 by the authors.

Figure 1
Figure 1. EoS models. Upper panel: Pressure P as function of mass density ρ is plotted according to the tabular composition in the outer crust and analytic fits in the inner crust, extended beyond the computed data range as explained in the text. Red solid, magenta short-dashed, and blue long-dashed lines show the EoS with the Kepler (K), Extreme rp (RP),and Superburst (SB) models for the accreted crust, respectively, with Po… view at source ↗
Figure 2
Figure 2. Upper panel: Total heat Eh, generated per accreted baryon in a layer from the star surface to a given mass density ρ, according to the model of Fantina et al. (2018) (F+18, dotted line), the model of Gusakov and Chugunov (2021) with Poi = P (cat) oi (GC, dashed line), and the model of Shchechilin et al. (2023) with Poi = P (cat) oi for the SB ashes (solid line). The gaps on the lines (best visible in the F+18 case) … view at source ↗
Figure 3
Figure 3. Simulated light curves for the outbursts I ( [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (2 more)
Figure 5
Figure 5. Figure 5: Simulated light curves for the crust cooling after [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]
Figure 6
Figure 6. Figure 6: Simulated light curves for the NS in IGR J17480 [PITH_FULL_IMAGE:figures/full_fig_p007_6.png]

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Works this paper leans on

45 extracted references · 44 canonical work pages

  1. [1]

    Gapless neutron superfluidity can explain the late time cooling of transiently accreting neutron stars

    Allard, V., Chamel, N., 2024a. Gapless neutron superfluidity can explain the late time cooling of transiently accreting neutron stars. https://ui.adsabs.harvard.edu/abs/2024PhRvL.132r1001A/abstract , 132, 181001

    work page

  2. [2]

    Gapless neutron superfluidity in the crust of the accreting neutron stars KS 1731--260 and MXB 1659--29

    Allard, V., Chamel, N., 2024b. Gapless neutron superfluidity in the crust of the accreting neutron stars KS 1731--260 and MXB 1659--29. https://ui.adsabs.harvard.edu/abs/2024EPJA...60..116A/abstract , 60, 116

    work page

  3. [3]

    Nuclear heating and melted layers in the inner crust of an accreting neutron star

    Brown, E.F., 2000. Nuclear heating and melted layers in the inner crust of an accreting neutron star. https://ui.adsabs.harvard.edu/abs/2000ApJ...531..988B/abstract , 531, 988

    work page 2000

  4. [4]

    Mapping crustal heating with the cooling light curves of quasi-persistent transients

    Brown, E.F., Cumming, A., 2009. Mapping crustal heating with the cooling light curves of quasi-persistent transients. https://ui.adsabs.harvard.edu/abs/2009ApJ...698.1020B/abstract , 698, 1020

    work page 2009

  5. [5]

    Cooling of the crust in the neutron star low-mass X-ray binary MXB 1659 - 29

    Cackett, E.M., Wijnands, R., Miller, J.M., Brown, E.F., Degenaar, N., 2008. Cooling of the crust in the neutron star low-mass X-ray binary MXB 1659 - 29. https://ui.adsabs.harvard.edu/abs/2008ApJ...687L..87C/abstract , 687, L87

    work page 2008

  6. [6]

    A change in the quiescent X-ray spectrum of the neutron star low-mass X-ray binary MXB 1659--29

    Cackett, E.M., Brown, E.F., Cumming, A., Degenaar, N., Fridriksson, J.K., Homan, J., Miller, J.M., Wijnands, R., 2013. A change in the quiescent X-ray spectrum of the neutron star low-mass X-ray binary MXB 1659--29. https://ui.adsabs.harvard.edu/abs/2013ApJ...774..131C/abstract , 774, 131

    work page 2013

  7. [7]

    Dependence of X-ray burst models on nuclear reaction rates

    Cyburt, R.H., Amthor, A.M., Heger, A., Johnson, E., Keek, L., Meisel, Z., Schatz, H., Smith, K., 2016. Dependence of X-ray burst models on nuclear reaction rates. https://ui.adsabs.harvard.edu/abs/2016ApJ...830...55C/abstract , 830, 55

    work page 2016

  8. [8]

    The accretion-heated crust of the transiently accreting 11-Hz X-ray pulsar in the globular cluster Terzan 5

    Degenaar, N., Wijnands, R., 2011. The accretion-heated crust of the transiently accreting 11-Hz X-ray pulsar in the globular cluster Terzan 5. https://ui.adsabs.harvard.edu/abs/2011MNRAS.414L..50D/abstract , 414, L50

    work page 2011

Show all 45 references
  1. [9]

    Late-time cooling of neutron star transients and the physics of the inner crust

    Deibel, A., Cumming, A., Brown, E.F., Reddy, S., 2017. Late-time cooling of neutron star transients and the physics of the inner crust. https://ui.adsabs.harvard.edu/abs/2017ApJ...839...95D/abstract , 839, 95

    2017

  2. [10]

    Crustal heating in accreting neutron stars from the nuclear energy-density functional theory

    Fantina, A.F., Zdunik, J.L., Chamel, N., Pearson, J.M., Haensel, P., Goriely, S., 2018. Crustal heating in accreting neutron stars from the nuclear energy-density functional theory. I. Proton shell effects and neutron-matter constraint. https://ui.adsabs.harvard.edu/abs/2018A ...

    2018

  3. [11]

    K., Muno, M

    Galloway, D. K., Muno, M. P., Hartman, J. M., Psaltis, D., and Chakrabarty, D., 2008. Thermonuclear (Type I) X-ray bursts observed by the Rossi X-ray Timing Explorer. https://ui.adsabs.harvard.edu/abs/2008ApJS..179..360G/abstract , 179, 360

    2008

  4. [12]

    Thermodynamically consistent equation of state for an accreted neutron star crust

    Gusakov, M.E., Chugunov, A.I., 2020. Thermodynamically consistent equation of state for an accreted neutron star crust. https://ui.adsabs.harvard.edu/abs/2020PhRvL.124s1101G/abstract , 124, 191101

    2020

  5. [13]

    Heat release in accreting neutron stars

    Gusakov, M.E., Chugunov, A.I., 2021. Heat release in accreting neutron stars. https://ui.adsabs.harvard.edu/abs/2021PhRvD.103j1301G/abstract , 103, L101301

    2021

  6. [14]

    E., Chugunov, A

    Gusakov, M. E., Chugunov, A. I., 2024. Thermodynamically consistent accreted crust of neutron stars: The role of proton shell effects. https://ui.adsabs.harvard.edu/abs/2024PhRvD.109l3032G/abstract , 109, 123032

    2024

  7. [15]

    Non-equilibrium processes in the crust of an accreting neutron star

    Haensel, P., Zdunik, J.L., 1990. Non-equilibrium processes in the crust of an accreting neutron star. https://ui.adsabs.harvard.edu/abs/1990A , 227, 431

    1990

  8. [16]

    Nuclear composition and heating in accreting neutron-star crusts

    Haensel, P., Zdunik, J.L., 2003. Nuclear composition and heating in accreting neutron-star crusts. https://ui.adsabs.harvard.edu/abs/2003A , 404, L33

    2003

  9. [17]

    Models of crustal heating in accreting neutron stars

    Haensel, P., Zdunik, J.L., 2008. Models of crustal heating in accreting neutron stars. https://ui.adsabs.harvard.edu/abs/2008A , 480, 459

    2008

  10. [18]

    O., Zheng, J., Maccarone, T

    Heinke, C. O., Zheng, J., Maccarone, T. J., Degenaar, N., Bahramian, A., Sivakoff, G. R.\ 2024. Catalog of outbursts of neutron star LMXBs. https://ui.adsabs.harvard.edu/abs/2024arXiv240718867H/abstract arXiv:2407.18867

    2024

  11. [19]

    Amorphous and heterogeneous phase of neutron star matter

    Jones, P.B., 1999. Amorphous and heterogeneous phase of neutron star matter. https://ui.adsabs.harvard.edu/abs/1999PhRvL..83.3589J/abstract , 83, 3589

    1999

  12. [20]

    First-principles point-defect calculations for solid neutron star matter

    Jones, P.B., 2001. First-principles point-defect calculations for solid neutron star matter. https://ui.adsabs.harvard.edu/abs/2001MNRAS.321..167J/abstract , 321, 167

    2001

  13. [21]

    Multi-zone models of superbursts from accreting neutron stars

    Keek, L., Heger, A., 2011. Multi-zone models of superbursts from accreting neutron stars. https://ui.adsabs.harvard.edu/abs/2011ApJ...743..189K/abstract , 743, 189

    2011

  14. [22]

    Fast neutrino cooling in the accreting neutron star MXB 1659 - 29

    Mendes, M., Fattoyev, F.J., Cumming, A., Gale, C., 2022. Fast neutrino cooling in the accreting neutron star MXB 1659 - 29. https://ui.adsabs.harvard.edu/abs/2022ApJ...938..119M/abstract , 938, 119

    2022

  15. [23]

    Nuclear ground-state masses and deformations: FRDM(2012)

    M\"oller, P., Sierk, A., Ichikawa, T., Sagawa, H., 2016. Nuclear ground-state masses and deformations: FRDM(2012). https://ui.adsabs.harvard.edu/abs/2016ADNDT.109....1M/abstract At.\ Data Nucl.\ Data Tables, 109--110, 1

    2012

  16. [24]

    Continued cooling of the accretion-heated neutron star crust in the X-ray transient IGR J17480 - 2446 located in the globular cluster Terzan 5

    Ootes, L.S., Vats, S., Page, D., Wijnands, R., Parikh, A.S., Degenaar, N., Wijngaarden, M.J.P., Altamirano, D., Bahramian, A., Cackett, E., et al., 2019. Continued cooling of the accretion-heated neutron star crust in the X-ray transient IGR J17480 - 2446 located in the globul...

    2019

  17. [25]

    Distances of the bulge globular clusters Terzan 5, Liller 1, UKS 1, and Terzan 4 based on HST NICMOS photometry

    Ortolani, S., Barbuy, B., Bica, E., Zoccali, M., Renzini, A., 2007. Distances of the bulge globular clusters Terzan 5, Liller 1, UKS 1, and Terzan 4 based on HST NICMOS photometry. https://ui.adsabs.harvard.edu/abs/2007A , 470, 1043

    2007

  18. [26]

    Forecasting neutron star temperatures: predictability and variability

    Page, D., Reddy, S., 2013. Forecasting neutron star temperatures: predictability and variability. https://ui.adsabs.harvard.edu/abs/2013PhRvL.111x1102P/abstract , 111, 241102

    2013

  19. [27]

    The spin and orbit of the newly discovered pulsar IGR J17480 - 2446

    Papitto, A., D'A\` , A., Motta, S., Riggio, A., Burderi, L., Di Salvo, T., Belloni, T., Iaria, R., 2011. The spin and orbit of the newly discovered pulsar IGR J17480 - 2446. https://ui.adsabs.harvard.edu/abs/2011A , 526. L3

    2011

  20. [28]

    Consistent accretion-induced heating of the neutron-star crust in MXB 1659--29 during two different outbursts

    Parikh, A.S., Wijnands, R., Ootes, L.S., Page, D., Degenaar, N., Bahramian, A., Brown, E.F., Cackett, E.M., Cumming, A., Heinke, C., et al., 2019. Consistent accretion-induced heating of the neutron-star crust in MXB 1659--29 during two different outbursts. https://ui.adsabs.h...

    2019

  21. [29]

    Unified equations of state for cold non-accreting neutron stars with Brussels--Montreal functionals -- I

    Pearson, J.M., Chamel, N., Potekhin, A.Y., Fantina, A.F., Ducoin, C., Dutta, A.K., Goriely, S., 2018. Unified equations of state for cold non-accreting neutron stars with Brussels--Montreal functionals -- I. Role of symmetry energy. https://ui.adsabs.harvard.edu/abs/2018MNRAS....

    2018

  22. [30]

    Magnetic neutron star cooling and microphysics

    Potekhin, A.Y., Chabrier, G., 2018. Magnetic neutron star cooling and microphysics. https://ui.adsabs.harvard.edu/abs/2018A , 609, A74

    2018

  23. [31]

    Crust structure and thermal evolution of neutron stars in soft X-ray transients

    Potekhin, A.Y., Chabrier, G., 2021. Crust structure and thermal evolution of neutron stars in soft X-ray transients. https://ui.adsabs.harvard.edu/abs/2021A , 645, A102

    2021

  24. [32]

    Neutron stars -- cooling and transport

    Potekhin, A.Y., Pons, J.A., Page, D., 2015. Neutron stars -- cooling and transport. https://ui.adsabs.harvard.edu/abs/2015SSRv..191..239P/abstract , 191, 239

    2015

  25. [33]

    Thermal evolution and quiescent emission of transiently accreting neutron stars

    Potekhin, A.Y., Chugunov, A.I., Chabrier, G., 2019. Thermal evolution and quiescent emission of transiently accreting neutron stars. https://ui.adsabs.harvard.edu/abs/2019A , 629, A88

    2019

  26. [34]

    Thermal evolution of neutron stars in soft X-ray transients with thermodynamically consistent models of the accreted crust

    Potekhin, A.Y., Gusakov, M.E., Chugunov, A.I., 2023. Thermal evolution of neutron stars in soft X-ray transients with thermodynamically consistent models of the accreted crust. https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.4830P/abstract , 522, 4830

    2023

  27. [35]

    Crustal emission and the quiescent spectrum of the neutron star in KS 1731--260

    Rutledge, R., Bildsten, L., Brown, E.F., Pavlov, G.G., Zavlin, V.E., Ushomirsky, G., 2002. Crustal emission and the quiescent spectrum of the neutron star in KS 1731--260. https://ui.adsabs.harvard.edu/abs/2002ApJ...580..413R/abstract , 580, 413

    2002

  28. [36]

    Nuclear compositions in the inner crust of neutron stars

    Sato, K., 1979. Nuclear compositions in the inner crust of neutron stars. https://ui.adsabs.harvard.edu/abs/1979PThPh..62..957S/abstract , 62, 957

    1979

  29. [37]

    https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.3860S/abstract , 507, 3860

    Shchechilin, N.N., Gusakov, M.E., Chugunov, A.I., 2021, Deep crustal heating for realistic compositions of thermonuclear ashes. https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.3860S/abstract , 507, 3860

    2021

  30. [38]

    Accreting neutron stars: heating of the upper layers of the inner crust

    Shchechilin, N.N., Gusakov, M.E., Chugunov, A.I., 2022. Accreting neutron stars: heating of the upper layers of the inner crust. https://ui.adsabs.harvard.edu/abs/2022MNRAS.515L...6S/abstract , 515, L6

    2022

  31. [39]

    Accreting neutron stars: composition of the upper layers of the inner crust

    Shchechilin, N.N., Gusakov, M.E., Chugunov, A.I., 2023. Accreting neutron stars: composition of the upper layers of the inner crust. https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.4643S/abstract , 523, 4643

    2023

  32. [40]

    The endpoint of the rp-process on accreting neutron stars

    Schatz, H., Aprahamian, A., Barnard, V., Bildsten, L., Cumming, A., Ouellette, M., Rauscher, T., Thielemann, F.-K., Wiescher, M., 2001. The endpoint of the rp-process on accreting neutron stars. https://ui.adsabs.harvard.edu/abs/2001NuPhA.688..150S/abstract , 688, 150

    2001

  33. [41]

    Neutron star cooling after deep crustal heating in the X-ray transient KS 1731-260

    Shternin, P.S., Yakovlev, D.G., Haensel, P., Potekhin, A.Y., 2007. Neutron star cooling after deep crustal heating in the X-ray transient KS 1731-260. https://ui.adsabs.harvard.edu/abs/2007MNRAS.382L..43S/abstract , 382, L43

    2007

  34. [42]

    Quiescent thermal emission from neutron stars in low-mass X-ray binaries

    Turlione, A., Aguilera, D.N., Pons, J.A., 2015. Quiescent thermal emission from neutron stars in low-mass X-ray binaries. https://ui.adsabs.harvard.edu/abs/2015A , 577, A5

    2015

  35. [43]

    Testing the deep-crustal heating model using quiescent neutron-star very-faint X-ray transients and the possibility of partially accreted crusts in accreting neutron stars

    Wijnands, R., Degenaar, N., Page, D., 2013. Testing the deep-crustal heating model using quiescent neutron-star very-faint X-ray transients and the possibility of partially accreted crusts in accreting neutron stars. https://ui.adsabs.harvard.edu/abs/2013MNRAS.432.2366W/abstra...

    2013

  36. [44]

    Cooling of accretion-heated neutron stars

    Wijnands, R., Degenaar, N., Page, D., 2017. Cooling of accretion-heated neutron stars. https://ui.adsabs.harvard.edu/abs/2017JApA...38...49W/abstract , 38, 49

    2017

  37. [45]

    Models for Type I X-ray bursts with improved nuclear physics

    Woosley, S.E., Heger, A., Cumming, A., Hoffman, R.D., Pruet, J., Rauscher, T., Fisker, J.L., Schatz, H., Brown, B.A., Wiescher, M., 2004. Models for Type I X-ray bursts with improved nuclear physics. https://ui.adsabs.harvard.edu/abs/2004ApJS..151...75W/abstract , 151, 75

    2004

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.