Thermal properties and detectability of neutron stars. II. Thermal evolution of rotation-powered neutron stars

Tsuruta, S.

doi:10.1016/s0370-1573(97)00041-0

Cited by 177 publications

(170 citation statements)

References 204 publications

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“…Note that Itoh and Tsuneto analyzed only the asymptote (210). In both papers the same asymptote (210) was obtained but with different numerical factors ξ. Wolf (1966) (c) Triplet-state neutron pairing In this case the neutron gap is anisotropic.…”

Section: Modified Urca Processes In Superfluid Mattermentioning

confidence: 76%

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.

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Section: Modified Urca Processes In Superfluid Mattermentioning

confidence: 76%

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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“…Since the lifetime of binary neutron stars from the birth to the merger is longer than ∼ 10 8 yrs for the observed systems [50], the temperature of each neutron star will be very low ( < ∼ 10 5 K) [51] at the onset of merger; i.e., the thermal energy per nucleon is much smaller than the Fermi energy of neutrons. Hence, cold nuclear EOSs are employed in giving the initial condition.…”

Section: Initial Condition and Setting For Simulationmentioning

confidence: 99%

Merger of binary neutron stars to a black hole: Disk mass, short gamma-ray bursts, and quasinormal mode ringing

2006

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Three-dimensional simulations for the merger of binary neutron stars are performed in the framework of full general relativity. We pay particular attention to the black hole formation case and to the resulting mass of the surrounding disk for exploring possibility for formation of the central engine of short-duration gamma-ray bursts (SGRBs). Hybrid equations of state are adopted mimicking realistic, stiff nuclear equations of state (EOSs), for which the maximum allowed gravitational mass of cold and spherical neutron stars, M sph , is larger than 2M⊙. Such stiff EOSs are adopted motivated by the recent possible discovery of a heavy neutron star of mass ∼ 2.1 ± 0.2M⊙. For the simulations, we focus on binary neutron stars of the ADM mass M > ∼ 2.6M⊙. For an ADM mass larger than the threshold mass M thr , the merger results in prompt formation of a black hole irrespective of the mass ratio QM with 0.65 < ∼ QM ≤ 1. The value of M thr depends on the EOSs and is approximately written as 1.3-1.35M sph for the chosen EOSs. For the black hole formation case, we evolve the spacetime using a black hole excision technique and determine the mass of a quasistationary disk surrounding the black hole. The disk mass steeply increases with decreasing the value of QM for given ADM mass and EOS. This suggests that a merger with small value of QM is a candidate for producing central engine of SGRBs. For M < M thr , the outcome is a hypermassive neutron star of a large ellipticity. Because of the nonaxisymmetry, angular momentum is transported outward. If the hypermassive neutron star collapses to a black hole after the longterm angular momentum transport, the disk mass may be > ∼ 0.01M⊙ irrespective of QM . Gravitational waves are computed in terms of a gauge-invariant wave extraction technique. In the formation of the hypermassive neutron star, quasiperiodic gravitational waves of frequency between 3 and 3.5 kHz are emitted irrespective of EOSs. The effective amplitude of gravitational waves can be > ∼ 5 × 10 −21 at a distance of 50 Mpc, and hence, it may be detected by advanced laser-interferometers. For the black hole formation case, the black hole excision technique enables a longterm computation and extraction of ring-down gravitational waves associated with a black hole quasinormal mode. It is found that the frequency and amplitude are ≈ 6.5-7 kHz and ∼ 10 −22 at a distance of 50 Mpc for the binary of mass M ≈ 2.7-2.9M⊙.

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“…Two-dimensional calculations of heat transport with magnetic field have been presented by Schaaf (1990a,b) who however restricted himself to the thin envelope and an uniform magnetic field. Tsuruta (1998) has presented results of two-dimensional cooling calculations of neutron stars which included the quantizing effect of a dipolar magnetic field in the envelope. These 2D calculations showed that the 1D approximation is indeed very good when the field affects heat transport only in the thin envelope.…”

Section: Outer Boundary: T B (B)-t S (B) Relationmentioning

confidence: 99%

Temperature distribution in magnetized neutron star crusts

Geppert¹,

Kueker²,

Page³

2004

A&A

123

150

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Abstract. We investigate the influence of different magnetic field configurations on the temperature distribution in neutron star crusts. We consider axisymmetric dipolar fields which are either restricted to the stellar crust, "crustal fields", or allowed to penetrate the core, "core fields". By integrating the two-dimensional heat transport equation in the crust, taking into account the classical (Larmor) anisotropy of the heat conductivity, we obtain the crustal temperature distribution, assuming an isothermal core. Including classical and quantum magnetic field effects in the envelope as a boundary condition, we deduce the corresponding surface temperature distributions. We find that core fields result in practically isothermal crusts unless the surface field strength is well above 10 15 G while for crustal fields with surface strength above a few times 10 12 G significant deviations from crustal isothermality occur at core temperatures inferior or equal to 10 8 K. At the stellar surface, the cold equatorial region produced by the suppression of heat transport perpendicular to the field by the Larmor rotation of the electrons in the envelope, present for both core and crustal fields, is significantly extended by that classical suppression at higher densities in the case of crustal fields. This can result, for crustal fields, in two small warm polar regions which will have observational consequences: the neutron star has a small effective thermally emitting area and the X-ray pulse profiles are expected to have a distinctively different shape compared to the case of a neutron star with a core field. These features, when compared with X-ray data on thermal emission of young cooling neutron stars, would provide a first step toward a new way of studying the magnetic flux distribution within a neutron star.

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Thermal properties and detectability of neutron stars. II. Thermal evolution of rotation-powered neutron stars

Cited by 177 publications

References 204 publications

Neutrino emission from neutron stars

Neutrino emission from neutron stars

Merger of binary neutron stars to a black hole: Disk mass, short gamma-ray bursts, and quasinormal mode ringing

Temperature distribution in magnetized neutron star crusts

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