Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23a1937k&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH23A-1937
Astronomy and Astrophysics
Astrophysics
[7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections
Scientific paper
Coronal mass ejections (CMEs) are known to be deflected when ejected near a coronal hole (Gopalswamy et al. 2009). We present results from simulations of CMEs near a coronal hole (CH) using a 3D magnetohydrodymics model - the Space Weather Modeling Framework. We propose magnetic tension and pressure as a cause of the CME deflection from the disturbed magnetic field lines of the simulation coronal hole. The solar wind is driven via Alfven waves and Kolmogorov-like dissipation and surface Alfven wave damping are considered for the dissipation of the waves (Evans et al. 2011). The magnetic field at the inner boundary is specified with synoptic magnetogram data from Carrington Rotation 2029, which corresponds to April 21 to May 18, 2005. CMEs are generated by inserting an out of equilibrium modified Titov-Demoulin flux rope into active region (AR) 0758. Treating the CME as a solid body we calculate the expected deflection from the coronal hole field lines. We compare this value to the actual path of the simulated CMEs for which we define a deflection angle as the difference between the observed path and the radial vector connecting the center of the Sun and the CME launch site. Finally, we generalize the deflection by seeing how it scales with several physical parameters such as CME mass, velocity and the separation of the AR and CH as well as its intensity. We compare our simulated and estimated values with observed deflections (Gopalswamy et. al 2009)
Evans Martin R.
Gombosi Tamas I.
Kay Christina
Opher Merav
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