TY - JOUR

T1 - Neutrino processes in strong magnetic fields and implications for supernova dynamics

AU - Duan, Huaiyu

AU - Qian, Yong Zhong

PY - 2004/1/1

Y1 - 2004/1/1

N2 - The processes [Formula Presented] and [Formula Presented] provide the dominant mechanisms for heating and cooling the material between the protoneutron star and the stalled shock in a core-collapse supernova. Observations suggest that some neutron stars are born with magnetic fields of at least [Formula Presented] while theoretical considerations give an upper limit of [Formula Presented] for the protoneutron star magnetic fields. We calculate the rates for the above neutrino processes in strong magnetic fields of [Formula Presented] We find that the main effect of such magnetic fields is to change the equations of state through the phase space of [Formula Presented] and [Formula Presented] which differs from the classical case due to quantization of the motion of [Formula Presented] and [Formula Presented] perpendicular to the magnetic field. As a result, the cooling rate can be greatly reduced by magnetic fields of [Formula Presented] for typical conditions below the stalled shock and a nonuniform protoneutron star magnetic field (e.g., a dipole field) can introduce a large angular dependence of the cooling rate. In addition, strong magnetic fields always lead to an angle-dependent heating rate by polarizing the spin of n and p. The implications of our results for the neutrino-driven supernova mechanism are discussed.

AB - The processes [Formula Presented] and [Formula Presented] provide the dominant mechanisms for heating and cooling the material between the protoneutron star and the stalled shock in a core-collapse supernova. Observations suggest that some neutron stars are born with magnetic fields of at least [Formula Presented] while theoretical considerations give an upper limit of [Formula Presented] for the protoneutron star magnetic fields. We calculate the rates for the above neutrino processes in strong magnetic fields of [Formula Presented] We find that the main effect of such magnetic fields is to change the equations of state through the phase space of [Formula Presented] and [Formula Presented] which differs from the classical case due to quantization of the motion of [Formula Presented] and [Formula Presented] perpendicular to the magnetic field. As a result, the cooling rate can be greatly reduced by magnetic fields of [Formula Presented] for typical conditions below the stalled shock and a nonuniform protoneutron star magnetic field (e.g., a dipole field) can introduce a large angular dependence of the cooling rate. In addition, strong magnetic fields always lead to an angle-dependent heating rate by polarizing the spin of n and p. The implications of our results for the neutrino-driven supernova mechanism are discussed.

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U2 - 10.1103/PhysRevD.69.123004

DO - 10.1103/PhysRevD.69.123004

M3 - Article

AN - SCOPUS:3843106818

VL - 69

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

SN - 1550-7998

IS - 12

ER -