Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: I. The Effect of Parity Violation in Weak Interactions, Astrophys
In proto-neutron stars with strong magnetic fields, the cross section for νe (¯νe) absorption on neutrons (protons) depends on the local magnetic field strength due to the quantization of energy levels for the e − (e +) produced in the final state. If the neutron star possesses an asymmetric magneti...
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ftciteseerx:oai:CiteSeerX.psu:10.1.1.256.1127 2023-05-15T18:22:58+02:00 Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: I. The Effect of Parity Violation in Weak Interactions, Astrophys Dong Lai The Pennsylvania State University CiteSeerX Archives 1998 application/pdf http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.256.1127 http://arxiv.org/pdf/astro-ph/9802345v1.pdf en eng http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.256.1127 http://arxiv.org/pdf/astro-ph/9802345v1.pdf Metadata may be used without restrictions as long as the oai identifier remains attached to it. http://arxiv.org/pdf/astro-ph/9802345v1.pdf text 1998 ftciteseerx 2016-01-07T19:56:38Z In proto-neutron stars with strong magnetic fields, the cross section for νe (¯νe) absorption on neutrons (protons) depends on the local magnetic field strength due to the quantization of energy levels for the e − (e +) produced in the final state. If the neutron star possesses an asymmetric magnetic field topology in the sense that the magnitude of magnetic field in the north pole is different from that in the south pole, then asymmetric neutrino emission may be generated. We calculate the absorption cross sections of νe and ¯νe in strong magnetic fields as a function of the neutrino energy. These cross sections exhibit oscillatory behaviors which occur because new Landau levels for the e − (e +) become accessible as the neutrino energy increases. By evaluating the appropriately averaged neutrino opacities, we demonstrate that the change in the local neutrino flux due to the modified opacities is rather small. To generate appreciable kick velocity ( ∼ 300 km s −1) to the newly-formed neutron star, the difference in the field strengths at the two opposite poles of the star must be at least 10 16 G. We conclude that this is a much less efficient mechanism to produce pulsar kicks than the one based on parity violation effect in weak interactions. We also consider the magnetic field effect on the spectral neutrino energy fluxes. The oscillatory features in the absorption opacities give rise to modulations in the emergent spectra of νe and ¯νe. Text South pole Unknown South Pole North Pole |
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In proto-neutron stars with strong magnetic fields, the cross section for νe (¯νe) absorption on neutrons (protons) depends on the local magnetic field strength due to the quantization of energy levels for the e − (e +) produced in the final state. If the neutron star possesses an asymmetric magnetic field topology in the sense that the magnitude of magnetic field in the north pole is different from that in the south pole, then asymmetric neutrino emission may be generated. We calculate the absorption cross sections of νe and ¯νe in strong magnetic fields as a function of the neutrino energy. These cross sections exhibit oscillatory behaviors which occur because new Landau levels for the e − (e +) become accessible as the neutrino energy increases. By evaluating the appropriately averaged neutrino opacities, we demonstrate that the change in the local neutrino flux due to the modified opacities is rather small. To generate appreciable kick velocity ( ∼ 300 km s −1) to the newly-formed neutron star, the difference in the field strengths at the two opposite poles of the star must be at least 10 16 G. We conclude that this is a much less efficient mechanism to produce pulsar kicks than the one based on parity violation effect in weak interactions. We also consider the magnetic field effect on the spectral neutrino energy fluxes. The oscillatory features in the absorption opacities give rise to modulations in the emergent spectra of νe and ¯νe. |
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The Pennsylvania State University CiteSeerX Archives |
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Dong Lai |
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Dong Lai Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: I. The Effect of Parity Violation in Weak Interactions, Astrophys |
author_facet |
Dong Lai |
author_sort |
Dong Lai |
title |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: I. The Effect of Parity Violation in Weak Interactions, Astrophys |
title_short |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: I. The Effect of Parity Violation in Weak Interactions, Astrophys |
title_full |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: I. The Effect of Parity Violation in Weak Interactions, Astrophys |
title_fullStr |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: I. The Effect of Parity Violation in Weak Interactions, Astrophys |
title_full_unstemmed |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: I. The Effect of Parity Violation in Weak Interactions, Astrophys |
title_sort |
neutrino transport in strongly magnetized proto-neutron stars and the origin of pulsar kicks: i. the effect of parity violation in weak interactions, astrophys |
publishDate |
1998 |
url |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.256.1127 http://arxiv.org/pdf/astro-ph/9802345v1.pdf |
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op_source |
http://arxiv.org/pdf/astro-ph/9802345v1.pdf |
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http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.256.1127 http://arxiv.org/pdf/astro-ph/9802345v1.pdf |
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Metadata may be used without restrictions as long as the oai identifier remains attached to it. |
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1766202392363139072 |