Heliophysics Events Knowledgebase Coverage Registry (HCR)
Observation Details
Overview Where Groups: Mode, FOV, # spectra in map Data Links
2016-08-16 15:26:35-16:21:54
AR 12577
Joint Observation with IRIS and BBSO/NST for Filament and Flare
x,y:445",-68"
Max FOV:267"x162"
Target:Active Region
Nearby Events
6302A Continuum Intensity267"x162"862 spectra
6302A Longitudinal Flux Density267"x162"862 spectra
6302A Transverse Flux Density267"x162"862 spectra
6302A Velocity 6301.5A267"x162"862 spectra
Level 1 Summary
Level 2 Summary
Level 1 Monthly
Level 2 Monthly
SOTSP: AR 12577
2016-08-16T15:26:35 to 2016-08-16T16:21:54
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=445 ycen=-68
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

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

Annotations:
Hits: 52
Chief Observer
Cruz (RCO)
Related Links
Cites: AR 12577     
Timeline: gif use
See also
Datasets
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wavelength: 6302A Continuum Intensity cadence: -1 min fov: 267,162 images: 862 JavaScript Landing Page
wavelength: 6302A Velocity 6301.5A cadence: -1 min fov: 267,162 images: 862 JavaScript Landing Page
wavelength: 6302A Transverse Flux Density cadence: -1 min fov: 267,162 images: 862 JavaScript Landing Page
wavelength: 6302A Longitudinal Flux Density cadence: -1 min fov: 267,162 images: 862 JavaScript Landing Page
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