PPT-SH31C-08: The Photospheric Poynting Flux and Coronal Heatin

Some models of coronal heating suppose that convective motions at the photosphere shuffle the footpoints of coronal magnetic fields and thereby inject sufficient magnetic energy upward to account for observed coronal . D.J. . Bercik. and J.G. . Luhmann. Space Sciences Lab, UC Berkeley. 1. FEW 2011, Aug 24. Introduction. The two most viable models of solar wind . energization. both ultimately appeal to convective granular flows. in Solar Disk Images . (and how to compare to models). Working Group Report. Nick Arge. .  . Rachel Hock. .  . Carl Henney. Definitions . (from our invited speakers). Coronal holes. : observable used as. with . M. ulti-wavelength. . Polarimetry. Silvano . Fineschi. INAF-Torino Astrophysical . Observatory, . Italy. 25. . May, . 2013, . Bern (CH). Coronal. . Magnetism. Line . formation. in . magnetized. e-mail: . hamrin@space.umu.se. Department of Physics, . Umeå. University, . Sweden. Nordic Cluster Meeting, Uppsala, August 2011. Hamrin, Nordic Cluster . Meeting. , 2011. . Cluster observations . Based on works by. Asaf. . Pe’er. . (ITC / Harvard University) . in collaboration with . Peter . Meszaros. . (PSU). , Martin Rees . (. IoA. ) . Christoffer. . Lundman. , Felix . Ryde. . (Stockholm. Flows . &. Flare Forecasting . tentative plans for Welsch & . Kazachenko. Topics. 0. Why do should . photospheric. electric or velocity fields . E. . or . v. matter for flares?. Previous work with B. Brian Welsch, George Fisher*, and Bill . Abbett. Space Sciences Laboratory, UC Berkeley. . *NB. : much . material presented here was borrowed from George!. 2. Links . between the interior and atmosphere?!. Dandan Ye. Contents. Paper review: . 2005 J.J. Sudol and J.W. Harvey. ‘. Longitudinal magnetic field changes accompanying . . solar flares’. My work . about. flare-related magnetic field evolutions to the X1.8 flare on 2012.10.23. Spectro. -polarimetry with the Turin . Lyot. -Filter. Silvano Fineschi . INAF – . Astrophysical. . Observatory. of . Torino, . Italy. Future . of . Polarimetry - . Brussels. (B) – 21-23 September 2015. . What Photospheric Magnetograms Can Teach Us About Solar Activity. Brian T. Welsch, Bill Abbett. 1. , Dave Bercik. 1. , . George H. Fisher. 1. , Yan Li. 1. , and Pete W. Schuck. 2 . 1. Space Sciences Lab, UC-Berkeley; . . Motivation. . The Corona is a Magnetically Dominated System. Coronal Magnetism is the Source of Space Weather. Coronal Mass Ejections. Energetic Particle Acceleration . Coronal Heating. Solar Wind Acceleration. June . 5-11. , . 2017. Cis . Verbeeck. . and SIDC forecaster team. Solar Influences. Data analysis Centre. www.sidc.be. Report of Solar Activity. Active Regions. 2. . low complexity . regions. Flaring. Alissa . N. . Oppenheimer¹. (. aoppenheimer2010@my.fit.edu. ), . A. Winebarger², S. Farid³, F. Mulu-Moore². ¹Department of Physics and Space Sciences, Florida Institute of Technology, Melbourne, FL 32907, United States. UV . Hanle. Effect . Coronal Magnetic Field & Plasma Dynamics . N.-E. . R. aouafi . Coronal Zeeman effect. Limitations. . Few . applications because of the weakness. of . the coronal magnetic field and of coronal signal.