1997/12/31 by Dong Lai, Yong-Zhong Qian, Y. -Z. Qian · 31 citations
Physics and Astronomy · #Asymmetry #Magnetic field #Neutrino #Neutrino Physics Research #Neutrino oscillation #Neutron star #Parity (physics) #Pulsar #Pulsars and Gravitational Waves Research #Quantum and Classical Electrodynamics #astro-ph
paper · pdf · doi:10.1086/311228
published in The Astrophysical Journal 495(2), L103-L106 (IOP Publishing) · AASTeX, 10 pages including 2 ps figures; ApJ Letter in press (March 10, 1998). Shortened to agree with the published version
arxiv created 1998/02/24 · openalex publication_date 1998/03/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In proto-neutron stars with strong magnetic fields, the neutrino-nucleon scattering/absorption cross sections depend on the direction of neutrino momentum with respect to the magnetic field axis, a manifestation of parity violation in weak interactions. We study the deleptonization and thermal cooling (via neutrino emission) of proto-neutron stars in the presence of such asymmetric neutrino opacities. Significant asymmetry in neutrino emission is obtained because of multiple neutrino-nucleon scatterings. For an ordered magnetic field threading the neutron star interior, the fractional asymmetry in neutrino emission is about 0.006( B /10 14 G), corresponding to a pulsar kick velocity of about 200( B /10 14 G) km s −1 for a total radiated neutrino energy of 3 × 10 53 ergs.