Can parity violation in neutrino transport lead to pulsar kicks?

In magnetized proto-neutron stars, neutrino cross sections depend asymmetri cally on the neutrino momenta because of parity violation. However, these a symmetric opacities do not induce any asymmetric flux in the bulk interior of the star where neutrinos are nearly in thermal equilibrium. Consequently , parity violation in neutrino absorption and scattering can only give rise to asymmetric neutrino flux above the neutrino-matter decoupling layer. We estimate that a dipole field of B similar to 10(15)-10(16) G is necessary to produce kick velocity of order of a few hundred km s(-1) using this mech anism.