Physics – Plasma Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh21a1492h&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SH21A-1492
Physics
Plasma Physics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle, [7833] Space Plasma Physics / Mathematical And Numerical Techniques
Scientific paper
We will show our recent efforts on the MHD simulation of the solar corona nearby the Sun and the solar wind in the heliosphere up to 20--40 AUs. In resent years, most of our efforts had been focused on the boundary treatment to introduce the observation-based map of B_r (the radial component of the magnetic field in the heliocentric frame, normal to the boundary surface) and other plasma parameters such as the coronal temperature derived from SOHO/EIT emission at the coronal base and the solar wind speed in the interplanetary space derived from IPS (interplanetary scintillation) measurements. Because of the large differences in time-scale, the simulation region is separated into two regions; the sub/trans-Alfvenic nearby-Sun region within 50 -- 100 solar radii, and the heliospheric part from 30--50 solar radii up to 10--40 AUs. In the time-varying nonlinear MHD simulation it is a challenge to handle the time-varying normal component of the magnetic field to the computation boundary. We employed a somehow simple model (differential layer model) that allows us to avoid some computational difficulties and obtain mathematical consistency: the characteristics of the hyperbolic MHD system can be fully taken into account to treat the time-variations of the unspecified MHD variables matching those of the specified time-varying variables on the sub-Alfvenic solar surface boundary. The boundary map rotating with the Sun is applied to the heliospheric rest-frame simulations. By introducing the time-varying boundary map and adding computational treatments, we are now able to obtain the theoretically and observationally consistent MHD solutions of the solar corona and solar wind in both time and space, and thus able to examine how the global corona and interplanetary space respond to the gradual but ceaseless solar-origin variations. We have tested this MHD simulation model with various dataset in various situations and found it is very robust and can give good agreements with the other independent measurements. In this presentation, we will focus on two periods; the last solar activity maximum (around 2002) and the minimum (around 2008 and 2009).
No associations
LandOfFree
MHD simulations of the solar corona and solar wind with the observation-based time-varying boundary maps of B_r and other variables does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with MHD simulations of the solar corona and solar wind with the observation-based time-varying boundary maps of B_r and other variables, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and MHD simulations of the solar corona and solar wind with the observation-based time-varying boundary maps of B_r and other variables will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1782146