中国物理B ›› 2008, Vol. 17 ›› Issue (3): 1147-1151.doi: 10.1088/1674-1056/17/3/066

• • 上一篇    

Re-research on the size of proto-neutron star in core-collapse supernova

罗志全, 刘门全   

  1. Institute of Theoretical Physics, China West Normal University, Nanchong 637002, China
  • 收稿日期:2007-05-23 修回日期:2007-08-09 出版日期:2008-03-04 发布日期:2008-03-04
  • 基金资助:
    Project supported by the National Natural Science Foundation of China (Grant No 10778719); the Scientific Research and Fund of Sichuan Provincial Education Department of China (Grant No 2006A079) and the Science and Technological Foundation of China West Normal University.

Re-research on the size of proto-neutron star in core-collapse supernova

Luo Zhi-Quan(罗志全)† and Liu Men-Quan(刘门全)   

  1. Institute of Theoretical Physics, China West Normal University, Nanchong 637002, China
  • Received:2007-05-23 Revised:2007-08-09 Online:2008-03-04 Published:2008-03-04
  • Supported by:
    Project supported by the National Natural Science Foundation of China (Grant No 10778719); the Scientific Research and Fund of Sichuan Provincial Education Department of China (Grant No 2006A079) and the Science and Technological Foundation of China West Normal University.

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摘要： The electron capture timescale may be shorter than hydrodynamic timescale in inner iron core of core-collapse supernova according to a recent new idea. Based on the new idea, this paper carries out a numerical simulation on supernova explosion for the progenitor model Ws15M$_{\odot}$. The numerical result shows that the size of proto-neutron star has a significant change (decrease about 20{\%}), which may affects the propagation of the shock wave and the final explosion energy.

关键词: supernova explosion, proto-neutron star, shock wave

Abstract: The electron capture timescale may be shorter than hydrodynamic timescale in inner iron core of core-collapse supernova according to a recent new idea. Based on the new idea, this paper carries out a numerical simulation on supernova explosion for the progenitor model Ws15M$_{\odot}$. The numerical result shows that the size of proto-neutron star has a significant change (decrease about 20%), which may affects the propagation of the shock wave and the final explosion energy.

Key words: supernova explosion, proto-neutron star, shock wave

中图分类号:  (Supernovae)

  • 97.60.Bw
97.21.+a (Pre-main sequence objects, young stellar objects (YSO's) and protostars (T Tauri stars, Orion population, Herbig-Haro objects, Bok globules, bipolar outflows, cometary nebulae, etc.)) 97.60.Jd (Neutron stars)