2024-09-24T22:21:16.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null HINODE SOTSP Kotanagi Brooks Tiwari (RCO) 409 HOP 409 with PSP Active Region AR AR unnamed 7 20230315_125404 383 410 411 7 7 1500 2 1 1 2 0 21 2017 746 0.9946666666666667 -308.242 461.466 236.482 162.304 2023-03-15T12:54:04.000Z 2023-03-15T13:41:28.000Z -308.242 461.466 Energetics of solar eruptions from the chromosphere to the inner heliosphereEnergetics of solar eruptions from the chromosphere to the inner heliosphere Fast map, 230"x164", Q65, 1-side CCD 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. ivo://sot.lmsal.com/VOEvent#2023-03-15T12:54:00Z