PPT-Coronal

Spectro polarimetry with the Turin Lyot Filter Silvano Fineschi INAF Astrophysical Observatory of Torino Italy Future of Polarimetry Brussels B 2123 September 2015. 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 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. quadrature. observations. Janusz Nicewicz. Introduction. ESA Model. Observations. Results. Conclusions . Introduction. . Mean distance 1AU. Mass . 1.9891×10. 30.  kg. Mean diameter 1,392,684 km. 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 . 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. . 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. Ken Phillips. Scientific Associate, Natural History Museum, and Honorary . Prof.. , QUB. 1. Solar Corona: Physical Properties. Solar corona has very . high temperatures:. . 10. 6. K – 2. ×10. 6. 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.. 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. 235 Dr. Andrea G. Drusini. Dipartimento di Scienze Medico-Diagnostiche e Terapie Speciali, Università diPadova,Via Giustiniani, 2- Padova 35128, Italia.Profesor de Antropología Física. Università