SOTSP: AR12974 and HOP436
2022-03-25T23:45:59 to 2022-03-26T00:18:21
Science Goal: AR long-term monitoring at high resolution with Hinode and Solar Orbiter
Program: Fast map, 164x164", 1-side, Q65, no repeat
Target: Active Region
xcen=-429 ycen=-239
Instrument: SOTSP
HOP/JOP: 436
Description:
During the third remote sensing window of the nominal mission phase (RSW3), Solar Orbiter will perform a continuous 4-day monitoring of an active region to study its decay throughout the atmosphere, focusing on dynamics, magnetic flux evolution and moving magnetic features. Specific questions to be addressed are: - What is the main mechanism of AR decay? Sunspot fragmentation by light bridges? Flux erosion by convective flows? MMFs? - How is the AR flux dispersed? - What is the fate of the dispersed flux? These observations will allow the sources of the slow solar wind at the boundaries of the AR to be studied as well. At the time of the measurements, Solar Orbiter and the Earth will be almost in quadrature, so the AR can be observed from very different vantage points. Ideally, the AR will be located on the western hemisphere, approaching the limb as seen from Earth. It will be observed with Hinode and IRIS for a few days before it disappears beyond the limb and then Solar Orbiter will take over. The coordinated observations will allow the intrinsic flux evolution of the AR to be disentangled from projection effects for the first time, without the need to resort to assumptions on the orientation of the vector magnetic field- It is expected that Solar Orbiter and Hinode will perform simultaneous observations of the target for at least a fraction of the time. These data will be used for magnetic stereoscopy of the AR.
During the third remote sensing window of the nominal mission phase (RSW3), Solar Orbiter will perform a continuous 4-day monitoring of an active region to study its decay throughout the atmosphere, focusing on dynamics, magnetic flux evolution and moving magnetic features. Specific questions to be addressed are: - What is the main mechanism of AR decay? Sunspot fragmentation by light bridges? Flux erosion by convective flows? MMFs? - How is the AR flux dispersed? - What is the fate of the dispersed flux? These observations will allow the sources of the slow solar wind at the boundaries of the AR to be studied as well. At the time of the measurements, Solar Orbiter and the Earth will be almost in quadrature, so the AR can be observed from very different vantage points. Ideally, the AR will be located on the western hemisphere, approaching the limb as seen from Earth. It will be observed with Hinode and IRIS for a few days before it disappears beyond the limb and then Solar Orbiter will take over. The coordinated observations will allow the intrinsic flux evolution of the AR to be disentangled from projection effects for the first time, without the need to resort to assumptions on the orientation of the vector magnetic field- It is expected that Solar Orbiter and Hinode will perform simultaneous observations of the target for at least a fraction of the time. These data will be used for magnetic stereoscopy of the AR.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 162,162 images: 512 JavaScript Landing Page
