Global three-dimensional simulation of the interplanetary evolution of the observed geoeffective coronal mass ejection during the epoch 1-4 August 2010

Details Global three-dimensional simulation of the interplanetary evolution of the observed geoeffective coronal mass ejection during the epoch 1-4 August 2010 Global three-dimensional simulation of the interplanetary evolution of the observed geoeffective coronal mass ejection during the epoch 1-4 August 2010

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011jgra..11612103w&link_type=abstract

Journal of Geophysical Research, Volume 116, Issue A12, CiteID A12103

Physics

Interplanetary Physics: Coronal Mass Ejections (4305, 7513), Interplanetary Physics: Corotating Streams, Interplanetary Physics: Interplanetary Shocks, Space Weather: Magnetic Storms (2788), Space Weather: Models

Scientific paper

Several coronal mass ejections (CMEs) were observed during 1-4 August 2010. At ˜17:12 UT on 3 August 2010, the Wind spacecraft detected an interplanetary shock followed by two magnetic cloud-like (MCL) structures that induced geomagnetic activity. The geomagnetic index, Dst, dropped to -65 nT while one of the MCLs passed through the magnetosphere. A global, three-dimensional magnetohydrodynamic (MHD) numerical model and a kinematic model (HAFv.2), with inputs based on actual solar observations, were used to simulate the response of the three-dimensional heliosphere. HAFv.2 and MHD models were used to simulate regions from 2.5 to 18 solar radii (Rs) and 18 to 285 Rs, respectively. A velocity pulse was used to simulate the major CME on 1 August 2010. The solar disturbances were injected into the lower boundary at 2.5 Rs. It is found that the background solar wind plays an important role in the evolution of this CME on its way to Earth. We compared the derived solar wind parameters (density, velocity, magnetic field, and temperature) with in situ observations from Wind near Earth. The simulation demonstrates a useful tool to link the general case of ICME at 1 AU to their solar sources. Simulation results also show that adiabatic value of γ = 5/3 seems to be appropriate for ideal MHD simulation studies of solar wind at 1 AU.

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