Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: The Effect of Asymmetric Magnetic Field Topology
In proto-neutron stars with strong magnetic fields, the cross section for $ν_e$ ($\barν_e$) 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 asymm...
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ftdatacite:10.48550/arxiv.astro-ph/9802345 2023-05-15T18:22:58+02:00 Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: The Effect of Asymmetric Magnetic Field Topology Lai, Dong Qian, Y. -Z. 1998 https://dx.doi.org/10.48550/arxiv.astro-ph/9802345 https://arxiv.org/abs/astro-ph/9802345 unknown arXiv https://dx.doi.org/10.1086/306203 Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ Astrophysics astro-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 1998 ftdatacite https://doi.org/10.48550/arxiv.astro-ph/9802345 https://doi.org/10.1086/306203 2022-04-01T17:16:38Z In proto-neutron stars with strong magnetic fields, the cross section for $ν_e$ ($\barν_e$) 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 $\nue$ and $\bnue$ 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 ($\sim 300$ 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 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 $ν_e$ and $\barν_e$. : AASTeX, 25 pages. Expanded introduction and references. This revised version was accepted by ApJ in April 1998 (to appear in the Oct 1 issue) Text South pole DataCite Metadata Store (German National Library of Science and Technology) North Pole South Pole |
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Astrophysics astro-ph FOS Physical sciences |
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Astrophysics astro-ph FOS Physical sciences Lai, Dong Qian, Y. -Z. Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: The Effect of Asymmetric Magnetic Field Topology |
topic_facet |
Astrophysics astro-ph FOS Physical sciences |
description |
In proto-neutron stars with strong magnetic fields, the cross section for $ν_e$ ($\barν_e$) 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 $\nue$ and $\bnue$ 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 ($\sim 300$ 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 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 $ν_e$ and $\barν_e$. : AASTeX, 25 pages. Expanded introduction and references. This revised version was accepted by ApJ in April 1998 (to appear in the Oct 1 issue) |
format |
Text |
author |
Lai, Dong Qian, Y. -Z. |
author_facet |
Lai, Dong Qian, Y. -Z. |
author_sort |
Lai, Dong |
title |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: The Effect of Asymmetric Magnetic Field Topology |
title_short |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: The Effect of Asymmetric Magnetic Field Topology |
title_full |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: The Effect of Asymmetric Magnetic Field Topology |
title_fullStr |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: The Effect of Asymmetric Magnetic Field Topology |
title_full_unstemmed |
Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks: The Effect of Asymmetric Magnetic Field Topology |
title_sort |
neutrino transport in strongly magnetized proto-neutron stars and the origin of pulsar kicks: the effect of asymmetric magnetic field topology |
publisher |
arXiv |
publishDate |
1998 |
url |
https://dx.doi.org/10.48550/arxiv.astro-ph/9802345 https://arxiv.org/abs/astro-ph/9802345 |
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North Pole South Pole |
geographic_facet |
North Pole South Pole |
genre |
South pole |
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South pole |
op_relation |
https://dx.doi.org/10.1086/306203 |
op_rights |
Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ |
op_doi |
https://doi.org/10.48550/arxiv.astro-ph/9802345 https://doi.org/10.1086/306203 |
_version_ |
1766202388886061056 |