SOTSP: HOP 317 w/ IRIS, BBSO
2016-08-17T19:25:01 to 2016-08-17T20:37:56
Science Goal: Joint Observation with IRIS and BBSO/NST for Filament and Flare
Program: Fast map 82x82", 1 side Q65
Target: Active Region
xcen=652 ycen=-51
Instrument: SOTSP
HOP/JOP: 317
Description:
abstract of observational proposal 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. Solar filaments are cold and dense plasma suspending in the solar corona (Tandberg-Hanssen 1995). On one hand, they could be very steady and have a lifetime of days or weeks. On the other hand, their eruptions could be the trigger of solar flares (Mackey et al. 2010). High resolution observations revealed that they are composed of a collection of separate threads which have a typical length of only 2-20 Mm (Lin et al. 2005). Although the fortuitously eruption of filaments is an attractive topic, more attentions should be paid to the formation and oscillation of the filaments, or more specificly, these motions in threads, which are important for us to understand the physics process of plasma in the solar corona. With the help of high-resolution images and spectrograms from NST, a better knowledge of the solar flare and filament, and hopefully their relationship would be achieved. request to SOT SP, Fast map mode, 82" ? 82" , 4 min cadence
abstract of observational proposal 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. Solar filaments are cold and dense plasma suspending in the solar corona (Tandberg-Hanssen 1995). On one hand, they could be very steady and have a lifetime of days or weeks. On the other hand, their eruptions could be the trigger of solar flares (Mackey et al. 2010). High resolution observations revealed that they are composed of a collection of separate threads which have a typical length of only 2-20 Mm (Lin et al. 2005). Although the fortuitously eruption of filaments is an attractive topic, more attentions should be paid to the formation and oscillation of the filaments, or more specificly, these motions in threads, which are important for us to understand the physics process of plasma in the solar corona. With the help of high-resolution images and spectrograms from NST, a better knowledge of the solar flare and filament, and hopefully their relationship would be achieved. request to SOT SP, Fast map mode, 82" ? 82" , 4 min cadence
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 85,81 images: 1082 JavaScript Landing Page
