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Neutrino processes in strong magneti...

Duan, Huaiyu.

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Neutrino processes in strong magnetic fields and implications for supernova dynamics.

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	Neutrino processes in strong magnetic fields and implications for supernova dynamics./
作者:	Duan, Huaiyu.
面頁冊數:	108 p.
附註:	Source: Dissertation Abstracts International, Volume: 65-08, Section: B, page: 4089.
Contained By:	Dissertation Abstracts International65-08B.
標題:	Physics, Nuclear. -
電子資源:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3144259
ISBN:	0496023357

Neutrino processes in strong magnetic fields and implications for supernova dynamics.
Duan, Huaiyu.

Neutrino processes in strong magnetic fields and implications for supernova dynamics. - 108 p.

Source: Dissertation Abstracts International, Volume: 65-08, Section: B, page: 4089.

Thesis (Ph.D.)--University of Minnesota, 2004.

The processes nue + n &rlhar2; e- + p and nue + p &rlhar2; e+ + n provide the dominant mechanisms for heating and cooling the material between the protoneutron star and the stalled shock in a core-collapse supernova. These neutrino processes also decide the neutron to proton ratio in the neutrino-driven wind, which is one of the key parameters of r-process nucleosynthesis. Observations suggest that some neutron stars are born with magnetic fields of at least &sim;1015 G while theoretical considerations give an upper limit of &sim;1018 G for the protoneutron star magnetic fields. We derive the analytical expressions of the rates for the above neutrino processes in strong magnetic fields to the 0th order of Enu/mN (Enu and mN being the neutrino energy and nucleon mass, respectively). We also develop a numerical method to calculate those rates to the 1st order of Enu/mN, which includes the effects of weak magnetism, nucleon recoil, and nucleon thermal motion. We apply the 0th order rates to a simple supernova model, and find that the cooling rates are substantially suppressed for typical supernova conditions in the presence of a magnetic field of &sim;10 16 G, which is due to the change in the equations of state through the phase space of e- and e +. In addition, strong magnetic fields always lead to an angle-dependent heating rate by polarizing the spin of n and p. Using the 1st order rates, we find that strong magnetic fields do not help to boost the neutron to proton ratio in neutrino-driven winds.

ISBN: 0496023357Subjects--Topical Terms:

1019065
Physics, Nuclear.

Neutrino processes in strong magnetic fields and implications for supernova dynamics.
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502 $a Thesis (Ph.D.)--University of Minnesota, 2004.
520 $a The processes nue + n &rlhar2; e- + p and nue + p &rlhar2; e+ + n provide the dominant mechanisms for heating and cooling the material between the protoneutron star and the stalled shock in a core-collapse supernova. These neutrino processes also decide the neutron to proton ratio in the neutrino-driven wind, which is one of the key parameters of r-process nucleosynthesis. Observations suggest that some neutron stars are born with magnetic fields of at least &sim;1015 G while theoretical considerations give an upper limit of &sim;1018 G for the protoneutron star magnetic fields. We derive the analytical expressions of the rates for the above neutrino processes in strong magnetic fields to the 0th order of Enu/mN (Enu and mN being the neutrino energy and nucleon mass, respectively). We also develop a numerical method to calculate those rates to the 1st order of Enu/mN, which includes the effects of weak magnetism, nucleon recoil, and nucleon thermal motion. We apply the 0th order rates to a simple supernova model, and find that the cooling rates are substantially suppressed for typical supernova conditions in the presence of a magnetic field of &sim;10 16 G, which is due to the change in the equations of state through the phase space of e- and e +. In addition, strong magnetic fields always lead to an angle-dependent heating rate by polarizing the spin of n and p. Using the 1st order rates, we find that strong magnetic fields do not help to boost the neutron to proton ratio in neutrino-driven winds.
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