Modeling Solar Wind and Coronal Mass Ejection During Carrington Rotation 2107

Details Modeling Solar Wind and Coronal Mass Ejection During Carrington Rotation 2107 Modeling Solar Wind and Coronal Mass Ejection During Carrington Rotation 2107

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh53c..08j&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH53C-08

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[0550] Computational Geophysics / Model Verification And Validation, [2102] Interplanetary Physics / Corotating Streams, [2164] Interplanetary Physics / Solar Wind Plasma, [7509] Solar Physics, Astrophysics, And Astronomy / Corona

Scientific paper

With the starting of solar cycle 24, the Sun begins to show more activity. New observations from Solar Dynamics Observatory (SDO) give us a great opportunity to test and validate our solar corona model for space weather forecasts. During Carrington Rotation 2107, an M3.7 flare occurred in NOAA 11164 on 2011 March 7 with a fast CME (> 2000 km/s). There is also a Solar Energetic Particle (SEP) event associated with this CME. In this study, we will first model the steady state solar wind using a newly developed three-dimensional Alfven-wave-driven global solar wind model within the Space Weather Modeling Framework (SWMF), which includes counter propagating Alfven waves. The magnetic field of the inner boundary is set up using the magnetogram from SDO/HMI. The inner boundary condition for density and temperature are specified from the Differential Emission Measure Tomography (DEMT) of SDO/AIA data. A flux rope is then applied to the active region NOAA 11164 to initiate the CME event. The properties of CME-driven shocks in the model output are studied in detail, which will be used to simulate the related SEP event in the future. By using multispacecraft observations, we perform a validation study for the model results.

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