Surface X-Ray Emission from Neutron Stars

Chiu, Hong‐Yee; Salpeter, E. E.

doi:10.1103/physrevlett.12.413

Cited by 170 publications

(93 citation statements)

References 3 publications

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“…(64) on the temperature and density is the generic one [1][2][3][4][5][6]. Additional dependence on these parameters is contained in the integral (65).…”

Section: Neutrino Emissivitymentioning

confidence: 99%

“…The reactions can be arranged, in general, according to the number of participating baryons, as the phase space arguments play the central role in controlling their temperature and density dependence [1][2][3][4][5][6]. In the case of neutrino pair bremsstrahlung, the leading order process in the density virial expansion is the two-body reaction…”

Section: Introductionmentioning

confidence: 99%

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Coherent neutrino radiation in supernovae at two loops

Sedrakian

Dieperink

2000

Phys. Rev. D

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We develop a neutrino transport theory, in terms of the real-time nonequilibrium Green's functions, which is applicable to physical conditions arbitrary far from thermal equilibrium. We compute the coherent neutrino radiation in cores of supernovae by evaluating the two-particle-two-hole (2p-2h) polarization function with dressed propagators. The propagator dressing is carried out in the particle-particle channel to all orders in the interaction. We show that at two loops there are two distinct sources of coherence effects in the bremsstrahlung. One is the generically off-shell intermediate state propagation, which leads to the Landau-Pomeranchuk-Migdal type suppression of radiation. We extend previous perturbative results, obtained in the leading order in quasiparticle width, by deriving the exact non-perturbative expression. A new contribution due to off-shell finial/initial baryon states is treated in the leading order in the quasiparticle width. The latter contribution corresponds to processes of higher order than second order in the virial expansion in the number of quasiparticles. At 2p-2h level, the time component of the polarization tensor for the vector transitions vanishes identically in the soft neutrino approximation. Vector current thereby is conserved. The contraction of the neutral axial vector current with tensor interaction among the baryons leads to a non-vanishing contribution to the bremsstrahlung rate. These rates are evaluated numerically for finite temperature pure neutron

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“…(64) on the temperature and density is the generic one [1][2][3][4][5][6]. Additional dependence on these parameters is contained in the integral (65).…”

Section: Neutrino Emissivitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Coherent neutrino radiation in supernovae at two loops

Sedrakian

Dieperink

2000

Phys. Rev. D

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“…These particles not interact with the magnetic fields and therefore their will pass free in magnetosphere forming the neutron wind around collapsing star. When in magnetosphere are the sufficiently value of free neutrons and protons, neutrino can generated by urca-processes when neutrons and protons capture of electron or positron and neutrino radiate by reactions [9] …”

Section: For Relativistic Protons With Energy Frommentioning

confidence: 99%

“…7KH OXPLQRVLW\ RI WKH XQLW ZROXPH E\ ȝ-meson decay is defined by the formula [33] ܳ ఔ ఓ ൎ 4 ή 10 ଷଶ ܶ ଽ ଷ for T 9 .…”

Section: Generation Neutrino By Mesons Decaymentioning

confidence: 99%

Generation of high-energy particles, neutrino and fotons in magnetosphere of collapsing star

Kryvdyk

2014

EPJ Web of Conferences

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Abstract. The generation of particles, photons and neutrinos in magnetosphere of collapsing star are considered. These processes are caused the self-interaction initial accelerating in magnetosphere protons and electrons. The second particles and photons will arise as a result of this self-interaction, which in turn will generate charged particles, photons and neutrino (cascade process). These processes are especially effective for the formation collapsing star magnetosphere from the secondary charged particles. In addition, the particles, photons and neutrinos will be generated in magnetosphere of collapsing star as result of these processes.

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“…If a neutron star were observed to cool slowly, on a timescale of order 1yr/T 4 9 , where T 9 is the core temperature in units of 10 9 K, this would be a clear sign of the core being composed of normal matter (a mixture of neutrons, protons, and electrons, with possible admixtures of other constituents), while if the neutron star were observed to cool rapidly, on a timescale of order 1min/T 4 9 , this would indicate that matter in the core was in an exotic state, such as quark matter, or a Bose condensate of pions or kaons. The reason for the very different timescales is that it was argued that in ordinary matter, the dominant neutrino emission process is the so-called modified Urca process, first discussed by Chiu and Salpeter [6], in which the two reactions n + n → n + p + e − +ν e and n + p + e − → n + n + ν e (1) occur in equal numbers. These reactions are just the usual processes of neutron beta decay and electron capture on protons,…”

Section: Introductionmentioning

confidence: 99%

Neutrino Emission from Dense Matter, and Neutron Star Thermal Evolution

Pethick¹,

Thórsson²

1995

The Lives of the Neutron Stars

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A brief review is given of neutrino emission processes in dense matter, with particular emphasis on recent developments. These include direct Urca processes for nucleons and hyperons, which can give rise to rapid energy loss from the stellar core without exotic matter, and the effect of band structure on neutrino bremsstrahlung from electrons in the crust, which results in much lower energy losses by this process than had previously been estimated.

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Surface X-Ray Emission from Neutron Stars

Cited by 170 publications

References 3 publications

Coherent neutrino radiation in supernovae at two loops

Coherent neutrino radiation in supernovae at two loops

Generation of high-energy particles, neutrino and fotons in magnetosphere of collapsing star

Neutrino Emission from Dense Matter, and Neutron Star Thermal Evolution

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