TY - JOUR
T1 - A new numerical method for simulating the solar wind Alfvén waves
T2 - Development of the VlasovMHD model
AU - Nariyuki, Y.
AU - Umeda, T.
AU - Kumashiro, T.
AU - Hada, T.
N1 - Funding Information:
This work was supported by Grant-in-Aid for Young Scientists (Start-up) No. 20840042 (Y.N.) from JSPS and Grant-in-Aid for Young Scientists (B) No. 21740352 (T.U.) from MEXT of Japan. This work was also carried out by the joint research program of the Solar-Terrestrial Environment Laboratory, Nagoya, University. The hybrid simulation code was kindly provided by Dr. K. Tsubouchi, and the simulation run was performed with the KDK system of the Research Institute for Sustainable Humanosphere (RISH) at Kyoto University as a collaborative research project.
PY - 2011/6
Y1 - 2011/6
N2 - A novel scheme of plasma simulation particularly suited for computing the one-dimensional nonlinear evolution of parallel propagating solar wind Alfvén waves is presented. The scheme is based on the Vlasov and the MHD models, for solving the longitudinal and the transverse components, respectively. As long as the nonlinearity is not very large (so that the longitudinal and transverse components are well separated), our VlasovMHD model can correctly describe evolution of finite amplitude parallel Alfvén waves, which are typical in the solar wind, both in the linear and nonlinear stages. The present model can be applied to discussions of phenomena where the parallel Alfvén waves play major roles, for example, the solar coronal heating and solar wind acceleration by the Alfvén waves propagating from the photosphere.
AB - A novel scheme of plasma simulation particularly suited for computing the one-dimensional nonlinear evolution of parallel propagating solar wind Alfvén waves is presented. The scheme is based on the Vlasov and the MHD models, for solving the longitudinal and the transverse components, respectively. As long as the nonlinearity is not very large (so that the longitudinal and transverse components are well separated), our VlasovMHD model can correctly describe evolution of finite amplitude parallel Alfvén waves, which are typical in the solar wind, both in the linear and nonlinear stages. The present model can be applied to discussions of phenomena where the parallel Alfvén waves play major roles, for example, the solar coronal heating and solar wind acceleration by the Alfvén waves propagating from the photosphere.
UR - http://www.scopus.com/inward/record.url?scp=79955485124&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=79955485124&partnerID=8YFLogxK
U2 - 10.1016/j.pss.2011.02.017
DO - 10.1016/j.pss.2011.02.017
M3 - Article
AN - SCOPUS:79955485124
VL - 59
SP - 767
EP - 771
JO - Planetary and Space Science
JF - Planetary and Space Science
SN - 0032-0633
IS - 8
ER -