Transport of neutrinos in hot neutron-star matter

Sawyer, R. F.; Soni, A. A.

doi:10.1086/157146

Cited by 57 publications

(41 citation statements)

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“…Rather the microscopic rates are relevant. The mean kinetic energies per neutrino or νν-pair are about ∼ 3T or ∼ 6T , respectively [52,53]. With mean collision rates of the order of Γ ∼ π 2 T 2 /ǫ F ≪ T [54], c.f.…”

Section: Discussion and Perspectivesmentioning

confidence: 99%

Classical and Quantum Many-Body Description of Bremsstrahlung in Dense Matter

Knoll¹,

Voskresensky²

1996

Annals of Physics

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Some considerations about the importance of coherence effects for bremsstrahlung processes in non-equilibrium dense matter (Landau -Pomeranchuk -Migdal -effect) are presented. They are of particular relevance for the application to photonand di-lepton production from high energy nuclear collisions, to gluon radiation in QCD transport, or parton kinetics and to neutrino and axion radiation from supernova explosion and from hot neutron stars. The soft behavior of the bremsstrahlung from a source described by classical transport models is discussed and pocket correction formulas for the in-matter radiation cross sections are suggested in terms of standard transport coefficients. The radiation rates are also discussed within a non-equilibrium quantum field theory (Schwinger -Kadanoff -Baym -Keldysh) formulation. A classification of diagrams and corresponding resummation in physically meaningful terms is proposed, which considers the finite damping width of all source particles in matter. This way each diagram in this expansion is already free from the infra-red divergences. Both, the correct quasi-particle and quasi-classical limits are recovered from this subset of graphs. Explicit results are given for dense matter in thermal equilibrium. The diagrammatic description may suggest a formulation of a transport theory that includes the propagation of off-shell particles in non-equilibrium dense matter.

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Section: Discussion and Perspectivesmentioning

confidence: 99%

Classical and Quantum Many-Body Description of Bremsstrahlung in Dense Matter

Knoll¹,

Voskresensky²

1996

Annals of Physics

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“…The scattering rate can be rewritten in a more conventionial form as follows. Define the differential cross section (per unit volume) to be 4) where the "nucleon response function", S ss ′ (q 0 , q), is…”

Section: A the Scattering Termmentioning

confidence: 99%

“…The cutoff R max ≃ eBA/2π (the degeneracy of the Landau level) limits the guiding center to lie within the normalization volume V = AL (where A is the area). The proton energy is given by 4) where N p specifies the Landau level, s p = ±1 is the spin projection along the z-axis, µ Bp is the proton magnetic moment, and p p,z is the proton z-momentum. The summation over states for the proton takes the form…”

Section: A the Expression For Absorption Opacitymentioning

confidence: 99%

Neutrino-nucleon interactions in magnetized neutron-star matter: The effects of parity violation

Arras

Lai

1999

Phys. Rev. D

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We study neutrino-nucleon scattering and absorption in a dense, magnetized nuclear medium. These are the most important sources of neutrino opacity governing the cooling of a proto-neutron star in the first tens of seconds after its formation. Because the weak interaction is parity violating, the absorption and scattering cross-sections depend asymmetrically on the directions of the neutrino momenta with respect to the magnetic field. We develop the moment formalism of neutrino transport in the presence of such asymmetric opacities and derive explicit expressions for the neutrino flux and other angular moments of the Boltzmann transport equation. For a given neutrino species, there is a drift flux of neutrinos along the magnetic field in addition to the usual diffusive flux. This drift flux depends on the deviation of the neutrino distribution function from thermal equilibrium. Hence, despite the fact that the neutrino cross-sections are asymmetric throughout the star, asymmetric neutrino flux can be generated only in the outer region of the proto-neutron star where the neutrino distribution deviates significantly from thermal equilibrium. The deviation from equilibrium is similarly altered by the asymmetric scattering and absorption, although its magnitude will still be quite small in the interior of the star. We clarify two reasons why previous studies have led to misleading results. First, inelasticity must be included in the phase space integrals in order to satisfy detail balance. Second, nucleon recoil must be included in order to find the leading order asymmetric cross sections correctly, even though it can be ignored to leading order to get the zero field opacities. In addition to the asymmetric absorption opacity arising from nucleon polarization, we find the contribution of the electron (or positron) ground state Landau level. For neutrinos of energy less than a few times the temperature, this is the dominant source of asymmetric opacity. Lastly, we discuss the implication of our result to the origin of pulsar kicks: in order to generate kick velocity of a few hundred km s −1 from asymmetric neutrino emission using the parity violation effect, the proto-neutron star must have a dipole magnetic field of at least 10 15 − 10

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“…In particular, we focus on the collision between a neutrino and a particle in nuclear matter in the presence of a strong magnetic field and a core temperature of 20 − 40MeV. Two-baryon process are not taken into account in the present PNS calculation since they only play an important role at low temperature (∼ a few MeV) [31].…”

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confidence: 99%

Relativistic mean-field treatment of pulsar kicks from neutrino propagation in magnetized proto-neutron stars

et al. 2012

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We make a perturbative calculation of neutrino scattering and absorption in hot and dense hyperonic neutron-star matter in the presence of a strong magnetic field. We calculate that the absorption cross-sections in a fully relativistic mean-field theory. We find that there is a remarkable angular dependence, i.e. the neutrino absorption strength is reduced in a direction parallel to the magnetic field and enhanced in the opposite direction. This asymmetry in the neutrino absorption is estimated to be as much as 2.2 % of the entire neutrino momentum for an interior magnetic field of ∼ 2 × 10 17 G. The pulsar kick velocities associated with this asymmetry are shown to be comparable to observed velocities.

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Transport of neutrinos in hot neutron-star matter

Cited by 57 publications

References 0 publications

Classical and Quantum Many-Body Description of Bremsstrahlung in Dense Matter

Classical and Quantum Many-Body Description of Bremsstrahlung in Dense Matter

Neutrino-nucleon interactions in magnetized neutron-star matter: The effects of parity violation

Relativistic mean-field treatment of pulsar kicks from neutrino propagation in magnetized proto-neutron stars

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