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

Tomoyuki Maruyama1,2,3, Nobutoshi Yasutake4, Myung-Ki Cheoun5,3, Jun Hidaka3, Toshitaka Kajino3,6, Grant J. Mathews7, and Chung-Yeol Ryu5

  • 1College of Bioresource Sciences, Nihon University, Fujisawa 252-8510, Japan
  • 2Advanced Science Research Center, Japan Atomic Energy Research Institute, Tokai 319-1195, Japan
  • 3National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
  • 4Research Institute for the Early Universe, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, Japan
  • 5Department of Physics, Soongsil University, Seoul 156-743, Korea
  • 6Department of Astronomy, Graduate School of Science, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, Japan
  • 7Department of Physics, Center of Astrophysics, University of Notre Dame, Notre Dame, Indiana 46556, USA

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Phys. Rev. D 86, 123003 – Published 4 December, 2012

DOI: https://doi.org/10.1103/PhysRevD.86.123003

Abstract

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 ∼2×1017  G. The pulsar kick velocities associated with this asymmetry are shown to be comparable to observed velocities.

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Phys. Rev. D 86, 123003– Published 4 December, 2012
  • Received 17 January 2012
Article part of CHORUS

© 2012 American Physical Society

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