SOTSP: HOP306 (w/IRIS) AR12599
2016-10-13T19:00:06 to 2016-10-13T19:32:27
Science Goal: Short-term Active Region Evolution
Program: Fast map, 160"x123", 1-side CCD
Target: Active Region
xcen=760 ycen=-332
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.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 162,122 images: 512 JavaScript Landing Page
