Diffusive heat blanketing envelopes of neutron stars

Beznogov, Mikhail V.; Potekhin, A. Y.; Yakovlev, D. G.

doi:10.1093/mnras/stw751

Cited by 36 publications

(63 citation statements)

References 185 publications

(479 reference statements)

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“…The curves are calculated using the approximate analytic expressions [13] for a 1.4 M star. The stars of age t 10-100 yr are thought to be thermally relaxed inside with a noticeable temperature gradient remaining only in a thin surface layer called the heat blanketing envelope (e.g., [14][15][16]). The stars with t 10 5 yr (including the Vela pulsar) are believed to be cooling predominantly via the neutrino emission from their superdense cores.…”

Section: Introductionmentioning

confidence: 99%

Thermal Spectrum and Neutrino Cooling Rate of the Vela Pulsar

Ofengeim¹,

Zyuzin²

2018

Particles

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Abstract:We reanalyse the X-ray spectrum of the PSR B0833-45 (the Vela pulsar) using the data of the Chandra space observatory. In contrast to previous works, we consider a wide range of possible masses and radii of the pulsar. The derived surface temperature of the star T ∞ s = 0.66−0.01 MK (1σ level over the entire mass and radius range of our study) is consistent with earlier results. However, the preferable values of Vela's mass and radius given by the spectral analysis are different from those used previously; they are consistent with modern equation of state models of neutron star matter. In addition, we evaluate the Vela's surface temperature as a function of assumed values of its mass and radius. This allows us to analyse the neutrino cooling rates consistent with the evaluated surface temperatures and explore the additional restrictions that could be set on the Vela's mass and radius using different versions of the neutron star cooling theory.

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Section: Introductionmentioning

confidence: 99%

Thermal Spectrum and Neutrino Cooling Rate of the Vela Pulsar

Ofengeim¹,

Zyuzin²

2018

Particles

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“…An interesting effect, first noticed by Beznogov et al (2016), is that the replacement of H by 4 He increases the photon luminosity. This effect is caused by the different mass to charge ratio of H, which results in the discontinuity of ρ and is related to the lower opacities of He at high T and fixed ρ, revealed in both op and opal tables.…”

Section: Accreted Envelopesmentioning

confidence: 93%

Magnetic neutron star cooling and microphysics

Potekhin

Chabrier

2018

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Aims. We study the relative importance of several recent updates of microphysics input to the neutron star cooling theory and the effects brought about by superstrong magnetic fields of magnetars, including the effects of the Landau quantization in their crusts. Methods. We use a finite-difference code for simulation of neutron-star thermal evolution on timescales from hours to megayears with an updated microphysics input. The consideration of short timescales ( 1 yr) is made possible by a treatment of the heatblanketing envelope without the quasistationary approximation inherent to its treatment in traditional neutron-star cooling codes. For the strongly magnetized neutron stars, we take into account the effects of Landau quantization on thermodynamic functions and thermal conductivities. We simulate cooling of ordinary neutron stars and magnetars with non-accreted and accreted crusts and compare the results with observations. Results. Suppression of radiative and conductive opacities in strongly quantizing magnetic fields and formation of a condensed radiating surface substantially enhance the photon luminosity at early ages, making the life of magnetars brighter but shorter. These effects together with the effect of strong proton superfluidity, which slows down the cooling of kiloyear-aged neutron stars, can explain thermal luminosities of about a half of magnetars without invoking heating mechanisms. Observed thermal luminosities of other magnetars are still higher than theoretical predictions, which implies heating, but the effects of quantizing magnetic fields and baryon superfluidity help to reduce the discrepancy.

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“…All the fits are obtained for an envelope with surface gravity g s,0 = 2.4271 × 10 14 cm s −2 but can be scaled for any g s using Y = (T s /1MK)(g s,0 /g s ) 1/4 (Gudmundsson et al 1983). We use an adapted version of the analytic functions (Equation A1) presented by Beznogov et al (2016).…”

Section: Appendix A: Analytic T S -T B Relationsmentioning

confidence: 99%

The effect of diffusive nuclear burning in neutron star envelopes on cooling in accreting systems

Wijngaarden

Chang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Valuable information about the neutron star interior can be obtained by comparing observations of thermal radiation from a cooling neutron star crust with theoretical models. Nuclear burning of lighter elements that diffuse to deeper layers of the envelope can alter the relation between surface and interior temperatures and can change the chemical composition over time. We calculate new temperature relations and consider two effects of diffusive nuclear burning (DNB) for H-C envelopes. First, we consider the effect of a changing envelope composition and find that hydrogen is consumed on short timescales and our temperature evolution simulations correspond to those of a hydrogen-poor envelope within ∼100 days. The transition from a hydrogen-rich to a hydrogen-poor envelope is potentially observable in accreting NS systems as an additional initial decline in surface temperature at early times after the outburst. Second, we find that DNB can produce a non-negligible heat flux, such that the total luminosity can be dominated by DNB in the envelope rather than heat from the deep interior. However, without continual accretion, heating by DNB in H-C envelopes is only relevant for <1-80 days after the end of an accretion outburst, as the amount of light elements is rapidly depleted. Comparison to crust cooling data shows that DNB does not remove the need for an additional shallow heating source. We conclude that solving the time-dependent equations of the burning region in the envelope selfconsistently in thermal evolution models instead of using static temperature relations would be valuable in future cooling studies.

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Diffusive heat blanketing envelopes of neutron stars

Cited by 36 publications

References 185 publications

Thermal Spectrum and Neutrino Cooling Rate of the Vela Pulsar

Thermal Spectrum and Neutrino Cooling Rate of the Vela Pulsar

Magnetic neutron star cooling and microphysics

The effect of diffusive nuclear burning in neutron star envelopes on cooling in accreting systems

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