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Modeling of Reflective Propagating Slow-mode Wave in a Flaring Loop View all abstracts by submitter

Xia Fang   Submitted: 2015-10-28 04:24

Quasi-periodic propagating intensity disturbances have been observed in large coronal loops in extreme ultraviolet images over a decade, and are widely accepted to be slow magnetosonic waves. However, spectroscopic observations from Hinode/EIS revealed their association with persistent coronal upflows, making this interpretation debatable. We perform a 2.5D magnetohydrodynamic simulation to imitate the chromospheric evaporation and the following reflected patterns in a flare loop. Our model encompasses the corona, transition region, and chromosphere. We demonstrate that the quasi periodic propagating intensity variations captured by the synthesized Solar Dynamics Observatory/Atmospheric Imaging Assembly 131, 94 Å emission images match the previous observations well. With particle tracers in the simulation, we confirm that these quasi periodic propagating intensity variations consist of reflected slow mode waves and mass flows with an average speed of 310 km s?1 in an 80 Mm length loop with an average temperature of 9 MK. With the synthesized Doppler shift velocity and intensity maps of the Solar and Heliospheric Observatory/Solar Ultraviolet Measurement of Emitted Radiation Fe xix line emission, we confirm that these reflected slow mode waves are propagating waves.

Authors: X. Fang, D. Yuan, T. Van Doorsselaere, R. Keppens, and C. Xia
Projects: None

Publication Status: published
Last Modified: 2015-10-28 15:24
Go to main E-Print page  CORONAL RAIN IN MAGNETIC ARCADES: REBOUND SHOCKS, LIMIT CYCLES, AND SHEAR FLOWS  Fast magnetoacoustic wave trains of sausage symmetry in cylindrical waveguides of the solar corona  Edit Entry  Download Preprint  Delete Entry 

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