Heliophysics Events Knowledgebase Coverage Registry (HCR)
Observation Details
Overview Where Groups: Mode, FOV, # spectra in map Data Links
2016-08-27 15:30:06-16:42:45
HOP306 (AR12580 evol) w/IRIS
Short-term Active Region Evolution
x,y:-32",-422"
Max FOV:84"x122"
Target:Active Region
Nearby Events
6302A Continuum Intensity84"x122"799 spectra
6302A Longitudinal Flux Density84"x122"799 spectra
6302A Transverse Flux Density84"x122"799 spectra
6302A Velocity 6301.5A84"x122"799 spectra

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SOTSP: HOP306 (AR12580 evol) w/IRIS
2016-08-27T15:30:06 to 2016-08-27T16:42:45
Science Goal: Short-term Active Region Evolution
Program: HOP 306 Fast map, 60"x121", 20min cadence
Target: Active Region
xcen=-32 ycen=-422
Instrument: SOTSP
HOP/JOP: 306
Description: Main Objective: To determine the short term evolution of the magnetic field and chromosphere and transition region of an active region Scientific Justification: Chromospheric and transition region heating in active regions are strongly correlated with the magnetic field. Various theoretical models predict that heating through braiding of magnetic field lines, reconnection with newly emerged flux, or dissipation of Alfven waves may play an important role in heating the chromosphere and transition region. To properly study the correlation between the magnetic field and low-atmospheric heating and to distinguish between various heating models, studies of the evolution of active regions on timescales of minutes to hours over the course of a few days are critical. Such high-cadence studies over a longer period of time can track the evolution of both the fields and the chromospheric/transition region heating as flux emergence and large scale flow patterns change the Poynting flux input into the solar atmosphere.

Main Objective: To determine the short term evolution of the magnetic field and chromosphere and transition region of an active region Scientific Justification: Chromospheric and transition region heating in active regions are strongly correlated with the magnetic field. Various theoretical models predict that heating through braiding of magnetic field lines, reconnection with newly emerged flux, or dissipation of Alfven waves may play an important role in heating the chromosphere and transition region. To properly study the correlation between the magnetic field and low-atmospheric heating and to distinguish between various heating models, studies of the evolution of active regions on timescales of minutes to hours over the course of a few days are critical. Such high-cadence studies over a longer period of time can track the evolution of both the fields and the chromospheric/transition region heating as flux emergence and large scale flow patterns change the Poynting flux input into the solar atmosphere.

Annotations:
Hits: 57
Chief Observer
DeRosa(RCO)
Related Links
Cites: HOP306 (AR12580 evol) w/IRIS     
Timeline: gif use
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Datasets
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saaIntervals hiIntervals

wavelength: 6302A Continuum Intensity cadence: 0 min fov: 84,122 images: 799 JavaScript Landing Page
wavelength: 6302A Velocity 6301.5A cadence: 0 min fov: 84,122 images: 799 JavaScript Landing Page
wavelength: 6302A Transverse Flux Density cadence: 0 min fov: 84,122 images: 799 JavaScript Landing Page
wavelength: 6302A Longitudinal Flux Density cadence: 0 min fov: 84,122 images: 799 JavaScript Landing Page
Time Series (SP Datacubes)
JavaScript MP4