Volume 33 Issue 3
May  2013
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Article Navigation >  Chinese Journal of Space Science  > 2013  >  33(3): 231-239
Chen Wenlei, He Jiansen, WU S T, Yang Liping, Wang Aihua, Zhang Lei, Tu Chuanyi. Study of magnetic reconnection between closed loops and open magnetic field driven by horizontal flows on solar surface[J]. Chinese Journal of Space Science, 2013, 33(3): 231-239. doi: 10.11728/cjss2013.03.231
Citation: Chen Wenlei, He Jiansen, WU S T, Yang Liping, Wang Aihua, Zhang Lei, Tu Chuanyi. Study of magnetic reconnection between closed loops and open magnetic field driven by horizontal flows on solar surface[J]. Chinese Journal of Space Science, 2013, 33(3): 231-239. doi: 10.11728/cjss2013.03.231
shu

Study of magnetic reconnection between closed loops and open magnetic field driven by horizontal flows on solar surface

doi: 10.11728/cjss2013.03.231 cstr: 32142.14.cjss2013.03.231
  • 1.

    School of Earth and Space Sciences, Peking University, Beijing 100871

  • 2.

    Center for Space Plasma and Aeronomic Research, University of Alabama, Huntsville, AL 35899, USA

  • Received Date: 2012-04-11
  • Rev Recd Date: 2012-10-11
  • Publish Date: 2013-05-15
    Abstract
  • Numerous observational events in the solar atmosphere (e.g., solar flares and jets) are attributed to be the energy conversion due to magnetic reconnection. Magnetic reconnection is also involved in a new scenario of solar wind origin to play a crucial role in opening the closed loop and releasing its mass into the open funnel. In the scenario, closed loop are moved towards the supergranular boundary by the supergranular advection, colliding with open magnetic funnel there and triggerring magnetic reconnection between each other. This work aims at studying the occurrence and effect of magnetic reconnection in the scenario in details. Magnetohydrodynamic (MHD) numerical simulation is an important approach to investigate the magnetic reconnection process in the solar atmosphere. A 2D MHD numerical model in supergranular scale is established, which starts from the solar atmosphere with stratified layers of temperature and density. Based on quantitative analysis of the simulation result, the conclusion that the mass flow in the open funnel can be supplied from the closed loop aside through magnetic reconnection as driven by supergranular advection is suggested. Our results lay the foundation for future modeling of solar wind origin.

     

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