2024-09-24T22:21:07.000Z 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 DeRosa(RCO) 268 HOP268 (MMF evolution) Active Region AR AR 12187 5 20141019_120626 375 403 404 5 30 64 2 1 3 2 1 82 2030 2105 65.78125 327.168 -239.146 10.11 81.152 2014-10-19T12:06:26.000Z 2014-10-19T14:59:31.000Z 327.168 -239.146 Transition region and coronal response to MMFs Sparse dynamics, 31"x80", step=3, Q75, 1-side, repeat This is an investigation of small moving magnetic features (MMFs) that move radially outwards from a sunspot in the moat region. MMFs can have an opposite polarity to the sunspot, and an early IRIS data-set from 2013 October 22 demonstrated that such MMFs can exhibit both transition region and coronal emission as they cancel against stronger plage fields. These MMFs all show signatures in the AIA 1700 channel and the IRIS Mg II and C II lines. A subset show very strong SiIV emission, and a smaller subset show coronal emission in the AIA 171 filter. The MMFs typically have a lifetime of 20-60 minutes, and they move over distances of up to 25 arcsec. This IHOP will obtain coordinated observations between SOT, XRT, EIS and IRIS to identify the magnetic topology and evolution that determines what temperature these MMFs reach. Signatures of the (presumed) magnetic reconnection will be identified through dynamics seen in the IRIS and EIS emission lines.;;This is an investigation of small moving magnetic features (MMFs) that move radially outwards from a sunspot in the moat region. MMFs can have an opposite polarity to the sunspot, and an early IRIS data-set from 2013 October 22 demonstrated that such MMFs can exhibit both transition region and coronal emission as they cancel against stronger plage fields. These MMFs all show signatures in the AIA 1700 channel and the IRIS Mg II and C II lines. A subset show very strong SiIV emission, and a smaller subset show coronal emission in the AIA 171 filter. The MMFs typically have a lifetime of 20-60 minutes, and they move over distances of up to 25 arcsec. This IHOP will obtain coordinated observations between SOT, XRT, EIS and IRIS to identify the magnetic topology and evolution that determines what temperature these MMFs reach. Signatures of the (presumed) magnetic reconnection will be identified through dynamics seen in the IRIS and EIS emission lines. ivo://sot.lmsal.com/VOEvent#2014-10-19T12:06:00Z