Using a complete non-local convection theory, we carried out the theoretical calculations of 7Li depletion of the solar convective envelope models with different convective parameters c1 and C2, and got a model of the...Using a complete non-local convection theory, we carried out the theoretical calculations of 7Li depletion of the solar convective envelope models with different convective parameters c1 and C2, and got a model of the solar convection zone consistent with the observed 7Li abundance and the depth of the solar convection zone determined by helioseismic techniques. The overshooting distance of effective non-local convective mixing of 7Li is very extensive, which is about 1.07 Hp or 0.09 R. However, the super-radiation temperature zone is much narrower, and it is only 0.20 Hp or 0.01GR.展开更多
Solar atmosphere is a rotating plasma shell filled by magnetic field. The coupling between the magnetic and the movement of plasma makes a variety of magnetohydrodynamic phenomena in the solar atmosphere. After giving...Solar atmosphere is a rotating plasma shell filled by magnetic field. The coupling between the magnetic and the movement of plasma makes a variety of magnetohydrodynamic phenomena in the solar atmosphere. After giving a brief introduction on the basic theoretical regime of solar MHD, we describe mainly the magnetohydrodynamic aspects of solar flares, solar prominences (filaments) and flux tubes with different scales. Some future works are also discussd.展开更多
文摘Using a complete non-local convection theory, we carried out the theoretical calculations of 7Li depletion of the solar convective envelope models with different convective parameters c1 and C2, and got a model of the solar convection zone consistent with the observed 7Li abundance and the depth of the solar convection zone determined by helioseismic techniques. The overshooting distance of effective non-local convective mixing of 7Li is very extensive, which is about 1.07 Hp or 0.09 R. However, the super-radiation temperature zone is much narrower, and it is only 0.20 Hp or 0.01GR.
文摘Solar atmosphere is a rotating plasma shell filled by magnetic field. The coupling between the magnetic and the movement of plasma makes a variety of magnetohydrodynamic phenomena in the solar atmosphere. After giving a brief introduction on the basic theoretical regime of solar MHD, we describe mainly the magnetohydrodynamic aspects of solar flares, solar prominences (filaments) and flux tubes with different scales. Some future works are also discussd.
基金美国太空总署(NASA)支持Smithsonian Astrophysical Observatory的研究基金NAG5-11420美国空军科研办公室(Air Force Office of ScientificResearch)支持Mount Wilson Observatory的研究基金 AF49620-02-1-0194所资助.
