SOTSP: AR obs (with HOP 409 from 14UT)
2023-03-17T14:00:04 to 2023-03-17T14:47:28
Science Goal: Energetics of solar eruptions from the chromosphere to the inner heliosphere
Program: Fast map, 230"x164", Q65, 1-side CCD
Target: Active Region
xcen=-733 ycen=422
Instrument: SOTSP
HOP/JOP: 409
Description:
Scientific Justification: In order to determine the global energy budget of solar eruptions, we will focus on every part of the erupting system with applicable remote-sensing and/or in situ data. Magnetic field observations used to determine the magnetic energy will come from SDO/HMI, Hinode/SOT, and DKIST. Spectroscopic measurements of flare ribbons to measure energy input into the chromosphere will come from Hinode/EIS, IRIS, and DKIST. Measurements of DEMs to determine the thermal energy in the corona will come from SDO/AIA, Hinode/EIS, Hinode/XRT, and GOES/SUVI. Measurements of the energy in non-thermal electrons in flares will be obtained using EOVSA, the JVLA, Fermi/GBM, and Solar Orbiter/STIX, if available. CME trajectories and kinetic energy will be determined using GOES/SUVI, PROBA-2/SWAP and coronagraphs and HI instruments on STEREO, SoHO, Solar Orbiter, and PSP. Solar energetic particles will be detected by PSP, ACE, STEREO, and Wind. This IHOP is a coordinated request from the three groups selected through NASA?s Heliophysics System Observatory Connect program and who plan to coordinate and make use of a wide range of remote-sensing observations. The requested observations will be shared among the projects to address multiple scientific questions. A second IHOP request will also be submitted by these same groups for observations when activity levels are higher during an encounter and the source region is predicted to be in or near an active region.
Scientific Justification: In order to determine the global energy budget of solar eruptions, we will focus on every part of the erupting system with applicable remote-sensing and/or in situ data. Magnetic field observations used to determine the magnetic energy will come from SDO/HMI, Hinode/SOT, and DKIST. Spectroscopic measurements of flare ribbons to measure energy input into the chromosphere will come from Hinode/EIS, IRIS, and DKIST. Measurements of DEMs to determine the thermal energy in the corona will come from SDO/AIA, Hinode/EIS, Hinode/XRT, and GOES/SUVI. Measurements of the energy in non-thermal electrons in flares will be obtained using EOVSA, the JVLA, Fermi/GBM, and Solar Orbiter/STIX, if available. CME trajectories and kinetic energy will be determined using GOES/SUVI, PROBA-2/SWAP and coronagraphs and HI instruments on STEREO, SoHO, Solar Orbiter, and PSP. Solar energetic particles will be detected by PSP, ACE, STEREO, and Wind. This IHOP is a coordinated request from the three groups selected through NASA?s Heliophysics System Observatory Connect program and who plan to coordinate and make use of a wide range of remote-sensing observations. The requested observations will be shared among the projects to address multiple scientific questions. A second IHOP request will also be submitted by these same groups for observations when activity levels are higher during an encounter and the source region is predicted to be in or near an active region.
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 237,162 images: 749 JavaScript Landing Page
