SOTSP: AR 12577
2016-08-16T15:26:30 to 2016-08-16T18:10:00
Science Goal: Joint Observation with IRIS and BBSO/NST for Filament and Flare
Program: Fast map, 280"x164", Q65, 1-side CCD
Target: Active Region
xcen=435 ycen=-75
Instrument: SOTSP
HOP/JOP: 317
Description:
Main Objective: Filament formation and the relationship between flare and filament in different levels Scientific Justification: Solar flares are one of the most energetic phenomenon that are closely related with the eruption of filaments (Aulanier et al. 2010). A huge amount of free magnetic energy (10^28 ? 10^32 erg) would be released into other kinds of energy, such as the thermal energy and kinetic energy of solar plasma and that of energetic particles. Theoretically, many ideal magneto-hydrodynamic (MHD) instabilities have been proposed to explain the solar eruption (Torok et al. 2004
Kilem and Torok 2006). While the realistic conditions are usually much more complex, thus detailed observation of the dynamic evolution of solar flare is important for understanding its physical nature. request to SOT SP, Fast map mode, 82" ? 82" , 4 min cadence
