Three-dimensional global simulation of CME/ICME/Shock propagation from Sun to the heliosphere

Details Three-dimensional global simulation of CME/ICME/Shock propagation from Sun to the heliosphere Three-dimensional global simulation of CME/ICME/Shock propagation from Sun to the heliosphere

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh14a..03w&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH14A-03

Physics

2101 Coronal Mass Ejections (7513), 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2139 Interplanetary Shocks, 2169 Solar Wind Sources, 7959 Models

Scientific paper

This study performs simulations of the propagation of coronal mass ejections from the Sun to the Earth through a realistic 3D solar wind structure. The famous solar event of 12 May 1997, described observationally by Thompson et al. [1998, 1999] and theoretically by Wu et al. [2001], is used as motivation for this simulation. The newly developed code, HAF+3DMHD combines two simulation codes, Hakamada-Akasofu-Fry code (HAF) version 2 (HAFv.2) [Fry et al., 2001] and a fully three-dimensional, time-dependent MHD simulation code [Han et al, 1988]. The solar wind structure is simulated, using the HAF code, out to 0.08 AU from source surface maps derived from solar magnetograms. The HAF simulation is then used as input for the lower boundary of a 3D MHD code to calculate the evolution of solar wind plasma beyond 18 solar radii (0.08 AU). A dynamic disturbance is delivered to this non-uniform structure to model the evolution and interplanetary propagation of a coronal mass ejection (ICME, including its shock). We also integrate the changing line-of-sight heliospheric density to compare to data observed by the LASCO instrument on SOHO, and we compare the derived ICME and shock structure at 1 AU to WIND solar wind data for this 12 May 1997 event. This new code provides a tool to link the general cases of ICME at 1 AU to their solar sources, as well as to identify the possible origins of shock formation due to CMEs and CME/CIR interactions. In the case of complex or interacting ejecta, model interpretation is often required to accurately determine the solar sources of the ejecta observed at 1 AU. Because this newly developed model incorporates 3D MHD, its results can be extended to simulate coronal and heliospheric observations, including the ambient medium's non-uniformity provided by the HAFv.2 model, from the upcoming STEREO mission. Reference: Fry et al., JGR, 106, 20985-21001, 2001. Han et al., Comp. and Fluids, 16, 81-103, 1988. Thompson et al., GRL, 25, 2465-2468, 1998. Thompson et al., AP. J. Lett., 517, L151-L155, 1999. Wu et al., JGR, 106, 25089-25102, 2001.

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