PPT-Coronal Magnetometry ISSI Feb. 25 – Mar. 01, 2013

UV Hanle Effect Coronal Magnetic Field amp Plasma Dynamics NE R aouafi Coronal Zeeman effect Limitations Few applications because of the weakness of the coronal magnetic field and of coronal signal. The genesis of solar coronal mass ejections CMEs is both an intellectually intriguing fundamental unsolved problem in plasma astrophysics and a societally relevant subject critical to space weather prediction and mitigation Understanding the preerup The material ejected is sent into interplanetary space where it eventually dissipates Should the material collide with a planet then that planets electromagnetic 64257eld would be temporarily disrupted If the Earths electromagnetic 64257eld were dis uk www sea rc o uk ea ed pd t on wwwsoftwarepartnerscouk brPage 2br d b t ea Nat Su 05 N0 142 Pre re d r ET A nu 20 6 ON NT e NT ON 3 MS S 4 VE 5 as fun li ow es t t p li ea ed pd t on wwwsoftwarepartnerscouk brPage 3br d b t ea Nat Su 05 N0 142 P 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. Automatic Detection of EUV Coronal Loops from SDO-AIA Data. 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. with . M. ulti-wavelength. . Polarimetry. Silvano . Fineschi. INAF-Torino Astrophysical . Observatory, . Italy. 25. . May, . 2013, . Bern (CH). Coronal. . Magnetism. Line . formation. in . magnetized. A.B. Galvin with contributions by C. . Farrugia. and L. Ellis. 1. Telemetry Losses - STA. 2. Telemetry Losses - STB. 3. Operations. In order to meet reduced telemetry we have been eliminating some . Condensation: . T. he . Origin of Coronal/Heliospheric Structure. S.. K. Antiochos, C. R. . DeVore. , et al . NASA/GSFC. Key features of the corona and wind. Laminar loops. Sheared filament channels. Spectro. -polarimetry with the Turin . Lyot. -Filter. Silvano Fineschi . INAF – . Astrophysical. . Observatory. of . Torino, . Italy. Future . of . Polarimetry - . Brussels. (B) – 21-23 September 2015. . 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. P. F. Chen. ，. China. Moreton wave. P. F. Chen . @ISSI-Beijing. Moreton et al. (1961). Moreton. . waves are associated with big flares . Propagation velocity: ~1. 000 km/s . Propagation distance: . 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. MoteMarineLaboratoryandAquarium-ReciprocalListUpdated09/22/2020MembershipDepartment941388-4441Ext373STATECITYINSTITUTIONRECIPROCITYCanadaCalgary -AlbertaCalgary Zoo50OffAdmissionTicketCanadaQuebec-Gra Nishu Karna. Mentor: Dr. William Dean . Pesnell. Code: 671. SESI Program-2010. Goddard Space Flight Center. Date: August 4, 2010. Coronal Hole :- . Large dark regions in the Sun’s corona that are cooler and have lower density plasma than average..