MODELING OF REFLECTIVE PROPAGATING SLOW-MODE WAVE IN A FLARING LOOP

Abstract

Quasi-periodic propagating intensity disturbances have been observed in large\ncoronal loops in EUV images over a decade, and are widely accepted to be slow\nmagnetosonic waves. However, spectroscopic observations from Hinode/EIS\nrevealed their association with persistent coronal upflows, making this\ninterpretation debatable. We perform a 2.5D magnetohydrodynamic simulation to\nimitate the chromospheric evaporation and the following reflected patterns in a\nflare loop. Our model encompasses the corona, transition region, and\nchromosphere. We demonstrate that the quasi periodic propagating intensity\nvariations captured by the synthesized \\textit{Solar Dynamics\nObservatory}/Atmospheric Imaging Assembly (AIA) 131, 94~\\AA~emission images\nmatch the previous observations well. With particle tracers in the simulation,\nwe confirm that these quasi periodic propagating intensity variations consist\nof reflected slow mode waves and mass flows with an average speed of 310 km/s\nin an 80 Mm length loop with an average temperature of 9 MK. With the\nsynthesized Doppler shift velocity and intensity maps of the \\textit{Solar and\nHeliospheric Observatory}/Solar Ultraviolet Measurement of Emitted Radiation\n(SUMER) Fe XIX line emission, we confirm that these reflected slow mode waves\nare propagating waves.\n