Modeling Super-fast Magnetosonic Waves Observed by SDO in Active Region Funnels

Details Modeling Super-fast Magnetosonic Waves Observed by SDO in Active Region Funnels Modeling Super-fast Magnetosonic Waves Observed by SDO in Active Region Funnels

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...740l..33o&link_type=abstract

The Astrophysical Journal Letters, Volume 740, Issue 2, article id. L33 (2011).

Astronomy and Astrophysics

Astronomy

2

Magnetohydrodynamics: Mhd, Sun: Activity, Sun: Corona, Sun: Coronal Mass Ejections: Cmes, Sun: Flares, Sun: Oscillations, Sun: Uv Radiation, Waves

Scientific paper

Recently, quasi-periodic, rapidly propagating waves have been observed in extreme ultraviolet by the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA) instrument in about 10 flare/coronal mass ejection (CME) events thus far. A typical example is the 2010 August 1 C3.2 flare/CME event that exhibited arc-shaped wave trains propagating in an active region (AR) magnetic funnel with ~5% intensity variations at speeds in the range of 1000-2000 km s-1. The fast temporal cadence and high sensitivity of AIA enabled the detection of these waves. We identify them as fast magnetosonic waves driven quasi-periodically at the base of the flaring region and develop a three-dimensional MHD model of the event. For the initial state we utilize the dipole magnetic field to model the AR and include gravitationally stratified density at coronal temperature. At the coronal base of the AR, we excite the fast magnetosonic wave by periodic velocity pulsations in the photospheric plane confined to a funnel of magnetic field lines. The excited fast magnetosonic waves have similar amplitude, wavelength, and propagation speeds as the observed wave trains. Based on the simulation results, we discuss the possible excitation mechanism of the waves, their dynamical properties, and the use of the observations for coronal MHD seismology.

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