2024-09-24T22:22:03.000Z 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 Arikawa Arikawa Cruz (RCO)-> Oba 322 HOP 322 w/ Hida @ AR 12578 Active Region PHO PHO 12578 10 20160819_234104 373 401 402 10 70 1024 2 1 1 2 0 21 2024 513 1.001953125 -194.368 6.508 162.621 162.304 2016-08-19T23:41:04.000Z 2016-08-20T00:13:25.000Z -194.368 6.508 Dark Filament and Photospheric Magnetic Field with coordinated observations between Hida Obs, Fuxian Solar Obs and Hinode Fast map, 164x164", 1-side, Q65, no repeat abstract of observational proposal Main Objective: Dark filaments on the disk and Photospheric magnetic field Scientific Justification: The main purpose of this plan is to investigate the evolution of fine structures of filaments and their relation with velocity field and magnetic field. If we are lucky enough, we could observe the magnetic reconnection and eruption. FSO group is used to study filaments by high resolution observations combined with simulations (e.g. NLFFF). But in this process, we need very good measurement of photospheric magnetic field. Therefore, 1m NVST at FSO does high resolution H-alpha imaging and 60cm DST at Hida Obs performs spectroscopy at chromospheric lines to measure the velocity, density and temperature of filaments. HINODE is hoped to obtain the distribution and evolution of photosphericmagnetic field with high accuracy. When the filament looks stationary, Hida/DST will occasionally take spectro-polarimetric data too in He 1083nm in order to directly confirm magnetic field configuration in the filament. request to SOT SP (fast map) 164"x164" (30min) twice/hr;;abstract of observational proposal Main Objective: Dark filaments on the disk and Photospheric magnetic field Scientific Justification: The main purpose of this plan is to investigate the evolution of fine structures of filaments and their relation with velocity field and magnetic field. If we are lucky enough, we could observe the magnetic reconnection and eruption. FSO group is used to study filaments by high resolution observations combined with simulations (e.g. NLFFF). But in this process, we need very good measurement of photospheric magnetic field. Therefore, 1m NVST at FSO does high resolution H-alpha imaging and 60cm DST at Hida Obs performs spectroscopy at chromospheric lines to measure the velocity, density and temperature of filaments. HINODE is hoped to obtain the distribution and evolution of photosphericmagnetic field with high accuracy. When the filament looks stationary, Hida/DST will occasionally take spectro-polarimetric data too in He 1083nm in order to directly confirm magnetic field configuration in the filament. request to SOT SP (fast map) 164"x164" (30min) twice/hr ivo://sot.lmsal.com/VOEvent#2016-08-19T23:40:30Z