2024-09-24T22:21:19.000Z 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 Arai Arai Cruz (RCO) 420 HOP 420 @ AR 13397 Active Region AR AR 13397 1 20230815_180106 608 630 606 1 96 1024 2 1 1 2 0 21 2017 508 0.9921875 697.192 249.491 161.036 121.728 2023-08-15T18:01:06.000Z 2023-08-15T18:33:27.000Z 697.192 249.491 tudy of MHD Waves in the Chromosphere Related to the Variation of Solar Abundances Fast map, 164"x123", 1-side CCD abstract of observational proposal Main Objective: Examine the effect of the waves propagating in the lower solar atmosphere on the abundance variation (First Ionization Potential (FIP) fractionation) Scientific Justification: The various structures in solar atmosphere have different solar abundances, photospheric or coronal. Our goal is to understand how the solar abundances changes in different plasma structures along the solar atmosphere. So far, several theoretical models propose that the waves in the lower solar atmosphere preferentially effect on the ionized particles more than neutral ones depending on their magnetic field configurations and environmental plasma characteristics, which are the main causes for the abundance variations (Laming 2012, 2017). request to SOT SOT observations are optional. If telemetry allows, we request SP maps covering the target region, active region or quiet region (at least FOV needs to be larger than 60 arcsec x 60 arcsec).;;abstract of observational proposal Main Objective: Examine the effect of the waves propagating in the lower solar atmosphere on the abundance variation (First Ionization Potential (FIP) fractionation) Scientific Justification: The various structures in solar atmosphere have different solar abundances, photospheric or coronal. Our goal is to understand how the solar abundances changes in different plasma structures along the solar atmosphere. So far, several theoretical models propose that the waves in the lower solar atmosphere preferentially effect on the ionized particles more than neutral ones depending on their magnetic field configurations and environmental plasma characteristics, which are the main causes for the abundance variations (Laming 2012, 2017). request to SOT SOT observations are optional. If telemetry allows, we request SP maps covering the target region, active region or quiet region (at least FOV needs to be larger than 60 arcsec x 60 arcsec). ivo://sot.lmsal.com/VOEvent#2023-08-15T18:01:00Z