Cooling of neutron stars in soft x-ray transients

Steiner, Andrew W.

doi:10.1103/physrevc.96.035802

Cited by 29 publications

(30 citation statements)

References 76 publications

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“…We find that the most likely models selected by this inference appear incompatible with the cooling of the coldest transiently-accreting sources, such as SAX J1808.4−3658 [37,59]. The suppression of the direct Urca emissivity due to pairing found here cannot explain the low temperatures observed.…”

Section: Conclusion and Discussionmentioning

confidence: 60%

Simultaneous fitting of neutron star structure and cooling data

2019

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Using a model for the equation of state and composition of dense matter and the magnitude of singlet proton superconductivity and triplet neutron superfluidity, we perform the first simultaneous fit of neutron star masses and radii determined from observations of quiescent low-mass x-ray binaries and luminosities and ages determined from observations of isolated neutron stars. We find that the Vela pulsar strongly determines the values inferred for the superfluid/superconducting gaps and the neutron star radius. We find, regardless of whether or not the Vela pulsar is included in the analysis, that the threshold density for the direct Urca process lies between the central density of 1.7 and 2 solar mass neutron stars. We also find that two solar mass stars are unlikely to cool principally by the direct Urca process because of the suppression by neutron triplet superfluidity.PACS numbers: 97.60. Jd, 95.30.Cq, arXiv:1812.00494v2 [nucl-th]

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Section: Conclusion and Discussionmentioning

confidence: 60%

Simultaneous fitting of neutron star structure and cooling data

2019

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“…Whether the enhanced cooling required is associated with exotic matter remains nevertheless unknown, which necessitate a further complete study quantifying all possible uncertainties. It is also intriguing that the estimated low to intermediate mass for the accreting neutron star in SAX J1808.4 3658 [30] could hardly fit in standard models given its extremely low luminosity [31], which implies some exotic composition might be present in its core.…”

Section: Hints That Neutrons and Protons Are Not Enoughmentioning

confidence: 99%

Observability of sharp phase transitions in neutron stars

Han

2019

AIP Conference Proceedings

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With central densities as high as 5-10 times the nuclear saturation density, neutron stars exhibit extreme conditions that cannot be observed elsewhere. They are ideal astrophysical laboratories for probing the composition and properties of cold, ultradense matter. We shall discuss taking into account currently available data from observation, how to reveal possible sharp phase transitions in dense neutron star cores. GLOBAL ASPECTS OF STABLE HYBRID STARSThe global structure of compact stars, including properties such as the mass, radius, tidal deformability, and the moment of inertia, are obtained for a realistic EoS by numerically solving Einstein equations of hydrostatic equilibrium, the Tolman-Oppenheimer-Volkov (TOV) equations [4,5]. Due to poorly constrained short-distance behavior of twoand three-nucleon interaction, there are large uncertainties in the nuclear matter EoS above 1-2 times saturation density, leading to variations in predicted radii and maximum masses of neutron stars. In the densest inner cores of neutron stars, exotic matter such as hyperons, meson condensates, or deconfined quarks may appear and even dominate. There are phenomenological models that describe possible novel phases, limited by the non-perturbative nature of Quantum Chromodynamics (QCD) at pertinent densities that prevents rigorous predictions. *

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“…Then the deep crustal heating is not strong enough to destroy the isothermality of stellar interiors supported by a high thermal conductivity. These sources can be called quasi-stationary (e.g., Han and Steiner 2017). When the star transits from an active state to quiescence, the observed surface luminosity drops quickly to the quiescent level.…”

Section: Deep Crustal Heatingmentioning

confidence: 99%

Afterburst thermal relaxation in neutron star crusts

Chaikin

Kaminker

Yakovlev

2018

Astrophys Space Sci

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We study thermal relaxation in a neutron star after internal heating events (outbursts) in the crust. We consider thin and thick spherically symmetric heaters, superfluid and non-superfluid crusts, stars with open and forbidden direct Urca processes in their cores. In particular, we analyze long-term thermal relaxation after deep crustal heating produced by nuclear transformations in fully or partly accreted crusts of transiently accreting neutron stars. This long-term relaxation has a typical relaxation time and an overall finite duration time for the crust to thermally equilibrate with the core. Neutron superfluidity in the inner crust greatly affects the relaxation if the heater is located in the inner crust. It shortens and unifies the time of emergence of thermal wave from the heater to the surface. This is important for the interpretation of observed outbursts of magnetars and transiently accreting neutron stars in quasi-persistent low-mass X-ray binaries.

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Cooling of neutron stars in soft x-ray transients

Cited by 29 publications

References 76 publications

Simultaneous fitting of neutron star structure and cooling data

Simultaneous fitting of neutron star structure and cooling data

Observability of sharp phase transitions in neutron stars

Afterburst thermal relaxation in neutron star crusts

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