Thermal Evolution of Neo-neutron Stars. I. Envelopes, Eddington Luminosity Phase, and Implications for GW170817

Beznogov, Mikhail V.; Page, Dany; Ramírez-Ruiz, E.

doi:10.3847/1538-4357/ab5fd6

Cited by 27 publications

(20 citation statements)

References 112 publications

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“…The initial temperature may change the thermal evolution. But, the dependence on the initial temperature seems to appear only up to ∼ 10 4 sec, the so-call neo-neutron stars era [67]. In this study, to avoid this dependence, we only consider the neutron star models at more than 1 year after they are born.…”

Section: Model Of Cooling Neutron Starsmentioning

confidence: 99%

Gravitational wave asteroseismology on cooling neutron stars

Sotani,

Dohi

2022

Preprint

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We examine the gravitational wave frequencies from neutron stars during thermal evolution, adopting the relativistic Cowling approximation. We particularly focus on the neutron star models, in which the direct Urca (rapid cooling process) does not work, without the superfluidity and superconductivity. For such models, the cooling curve hardly depends on the equation of state (EOS) as well as the mass of neutron star, while we show that the gravitational wave frequencies strongly depend on the both properties. Then, we find that the frequencies of the fundamental and the 1st pressure mode multiplied with the stellar mass are well expressed as a function of the stellar compactness almost independently of the EOS. We also find that the frequency of the 1st gravity mode in later phase of the thermal evolution is strongly correlated with the stellar compactness. In addition, we derive the empirical formula estimating the threshold mass for the onset of the direct Urca inside the neutron star as a function of the nuclear saturation parameter. This formula will give us a constraint on the neutron star properties, if it would be observationally found that the direct Urca occurs (or does not work) inside the neutron star.

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Section: Model Of Cooling Neutron Starsmentioning

confidence: 99%

Gravitational wave asteroseismology on cooling neutron stars

Sotani,

Dohi

2022

Preprint

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“…Processes such as DNB can significantly alter the envelope composition over time and can release additional heat, making it worthwhile to include the burning region of the envelope in future thermal evolution calculations. This would require setting the upper boundary of thermal transport equations to lower densities than ρ b = 10 8 or ρ b = 10 10 instead of using static temperature relations to connect the temperature at those densities to the temperature at the surface (see Beznogov et al 2020 for a more consistent treatment of the envelope applied to young neutron stars).…”

Section: General Effects Of Dnbmentioning

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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“…Comparing with the single NSs originating from the classic core-collapse SNe, the single NSs from the mergers of double WDs may correspond to a specific kind of NSs, showing some different properties, such as circumstellar environments and magnetic fields, etc. Beznogov et al (2020) recently suggested that the NSs originated from AIC may be observable during the neo-NS (i.e., hot NS) stage, in which the NS has just become transparent to neutrinos. Fig.…”

Section: Mass Distribution Of Nssmentioning

confidence: 99%

The formation of neutron star systems through accretion-induced collapse in white-dwarf binaries

Wang,

Liu

2020

Preprint

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The accretion-induced collapse (AIC) scenario was proposed 40 years ago as an evolutionary end state of oxygen-neon white-dwarfs (ONe WDs), linking them to the formation of neutron star (NS) systems. However, there has been no direct detection of any AIC event so far, even though there exists a lot of indirect observational evidence. Meanwhile, the binary evolutionary pathways resulting in NS formation through AIC are still not well investigated. In this article, we review recent studies on the two classic progenitor models of AIC events, i.e., the single-degenerate model (including the ONe WD+MS/RG/He star channels and the CO WD+He star channel) and the doubledegenerate model (including the double CO WD channel, the double ONe WD channel and the ONe WD+CO WD channel). Recent progress on these progenitor models is reviewed, including the binary evolutionary scenarios leading to AIC events, the initial parameter space for producing AIC events, and the related objects (e.g., the pre-AIC systems and the post-AIC systems). For the single-degenerate model, the pre-AIC systems (i.e., the progenitor systems of AIC events) could potentially be identified as cataclysmic variables (such as classical novae, recurrent novae, Ne novae and He novae), symbiotics and supersoft X-ray sources in the observations, whereas the post-AIC systems (i.e., NS systems) could potentially be identified as low-/intermediate-mass X-ray binaries, and the resulting low-/intermediate-mass binary pulsars, most notably millisecond pulsars. For the double-degenerate model, the pre-AIC systems are close double WDs with short orbital periods, whereas the post-AIC systems are single isolated NSs that may correspond to a specific kind of NS with peculiar properties. We also review the predicted rates of AIC events, the mass distribution of NSs produced via AIC, and the gravitational wave (GW) signals from double WDs that are potential GW sources in the Galaxy in the context of future space-based GW detectors, such as LISA, TianQin and Taiji, etc. Recent theoretical and observational constraints on the detection of AIC events are summarized. In order to confirm the existence of the AIC process, and resolve this long-term issue presented by current stellar evolution theories, more numerical simulations and observational identifications are required.

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Thermal Evolution of Neo-neutron Stars. I. Envelopes, Eddington Luminosity Phase, and Implications for GW170817

Cited by 27 publications

References 112 publications

Gravitational wave asteroseismology on cooling neutron stars

Gravitational wave asteroseismology on cooling neutron stars

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

The formation of neutron star systems through accretion-induced collapse in white-dwarf binaries

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