Structure of neutron star envelopes

Gudmundsson, E. H.; Pethick, C. J.; Epstein, Richard I.

doi:10.1086/161292

Cited by 303 publications

(347 citation statements)

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“…For weakly magnetized, isolated cooling neutron stars, ρ b is usually set at 10 10 g cm −3 (Gudmundsson et al 1983), but in general it varies from 10 8 g cm −3 for neutron stars with rapid variations of thermal emission ) to ρ drip for relatively hot and strongly magnetized neutron stars (Potekhin et al 2003).…”

Section: Blanketing Envelopesmentioning

confidence: 99%

“…A more accurate but less simple fit was constructed by . The T b -T s relation is mainly regulated by the thermal conductivity in the "sensitivity strip" (Gudmundsson et al 1983) that plays the role of a "bottleneck" for the heat leakage. Its position lies around the line where κ r = κ e (as a rule, around ρ ∼ 10 5 -10 7 g cm −3 for B = 0) and depends on the stellar structure, the boundary temperature T b , the magnetic field B B B in the vicinity of the given surface point, and the chemical composition of the envelope.…”

Section: Blanketing Envelopesmentioning

confidence: 99%

“…Neglecting also the non-uniformity of the energy flux through the envelope due to the neutrino emission (which is small, if the neutron star is not too hot, as we discuss below) and the variation of the temperature T s over the surface (which varies on larger length scales than z b ), one can obtain, instead of Eq. (4), the much simpler thermal structure equation (Gudmundsson et al 1983;Van Riper 1988) …”

Section: Blanketing Envelopesmentioning

confidence: 99%

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Neutron Stars—Cooling and Transport

2015

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Observations of thermal radiation from neutron stars can potentially provide information about the states of supranuclear matter in the interiors of these stars with the aid of the theory of neutron-star thermal evolution. We review the basics of this theory for isolated neutron stars with strong magnetic fields, including most relevant thermodynamic and kinetic properties in the stellar core, crust, and blanketing envelopes.

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Section: Blanketing Envelopesmentioning

confidence: 99%

Section: Blanketing Envelopesmentioning

confidence: 99%

Section: Blanketing Envelopesmentioning

confidence: 99%

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Neutron Stars—Cooling and Transport

2015

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“…Thermal relaxation of the neutron star crust occurs on the scale of a few tens of years, while the relaxation time of the outer envelopes is still shorter (Lattimer et al 1994;Gnedin et al 2001;Fortin et al 2010). Therefore, the outer envelopes are considered quasistationary for most of the astrophysical problems, and their thermal structure is calculated at stationary equilibrium (Gudmundsson et al 1983). In particular, Fushiki & Lamb (1987) applied this approximation to the stability analysis of H and He shells of accreting neutron stars, and Brown & Bildsten (1998) and Cumming & Bildsten (2001) applied it to the stability analysis of carbon shells.…”

Section: Conductive Coolingmentioning

confidence: 99%

Thermonuclear fusion in dense stars

Potekhin

Chabrier

2012

A&A

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We study the plasma correlation effects on nonresonant thermonuclear reactions of carbon and oxygen in the interiors of white dwarfs and liquid envelopes of neutron stars. We examine the effects of electron screening on thermodynamic enhancement of thermonuclear reactions in dense plasmas beyond the linear mixing rule. Using these improved enhancement factors, we calculate carbon and oxygen ignition curves in white dwarfs and neutron stars. The energy balance and ignition conditions in neutron star envelopes are evaluated, taking their detailed thermal structure into account. The result is compared to the simplified "one-zone model", which is routinely used in the literature. We also consider the effect of strong magnetic fields on the ignition curves in the ocean of magnetars.

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“…The properties of the atmosphere of a sufficiently hot, nascent neutron star should differ significantly from those considered in Gudmundsson et al (1983) and Potekhin et al (1997), especially since at hot temperatures (T 10 9 K) the atmosphere might not be transparent to neutrinos, and thus the neutrino transport equations have to be considered. The coupled equations of neutrino and photon transport, in the atmosphere of a neutron star, were solved by Salpeter & Shapiro (1981), and Duncan et al (1986).…”

Section: Cooling Of Young Hot Neutron Starsmentioning

confidence: 96%

Cooling of young neutron stars in GRB associated to supernovae

Negreiros

Ruffini

Bianco

et al. 2012

A&A

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Context. The traditional study of neutron star cooling has been generally applied to quite old objects such as the Crab Pulsar (957 years) or the central compact object in Cassiopeia A (330 years) with an observed surface temperature ∼10 6 K. However, recent observations of the late (t = 10 8 -10 9 s) emission of the supernovae (SNe) associated to GRBs (GRB-SN) show a distinctive emission in the X-ray regime consistent with temperatures ∼10 7 -10 8 K. Similar features have been also observed in two Type Ic SNe SN 2002ap and SN 1994I that are not associated to GRBs. Aims. We advance the possibility that the late X-ray emission observed in GRB-SN and in isolated SN is associated to a hot neutron star just formed in the SN event, here defined as a neo-neutron star. Methods. We discuss the thermal evolution of neo-neutron stars in the age regime that spans from ∼1 min (just after the proto-neutron star phase) all the way up to ages <10-100 yr. We examine critically the key factor governing the neo-neutron star cooling with special emphasis on the neutrino emission. We introduce a phenomenological heating source, as well as new boundary conditions, in order to mimic the high temperature of the atmosphere for young neutron stars. In this way we match the neo-neutron star luminosity to the observed late X-ray emission of the GRB-SN events: URCA-1 in GRB980425-SN1998bw, URCA-2 in GRB030329-SN2003dh, and URCA-3 in GRB031203-SN2003lw. Results. We identify the major role played by the neutrino emissivity in the thermal evolution of neo-neutron stars. By calibrating our additional heating source at early times to ∼10 12 -10 15 erg/g/s, we find a striking agreement of the luminosity obtained from the cooling of a neo-neutron stars with the prolonged (t = 10 8 -10 9 s) X-ray emission observed in GRB associated with SN. It is therefore appropriate a revision of the boundary conditions usually used in the thermal cooling theory of neutron stars, to match the proper conditions of the atmosphere at young ages. The traditional thermal processes taking place in the crust might be enhanced by the extreme high-temperature conditions of a neo-neutron star. Additional heating processes that are still not studied within this context, such as e + e − pair creation by overcritical fields, nuclear fusion, and fission energy release, might also take place under such conditions and deserve further analysis. Conclusions. Observation of GRB-SN has shown the possibility of witnessing the thermal evolution of neo-neutron stars. A new campaign of dedicated observations is recommended both of GRB-SN and of isolated Type Ic SN.

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Structure of neutron star envelopes

Cited by 303 publications

References 0 publications

Neutron Stars—Cooling and Transport

Neutron Stars—Cooling and Transport

Thermonuclear fusion in dense stars

Cooling of young neutron stars in GRB associated to supernovae

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