PPT-X-ray Spectroscopy of Coronal Plasmas

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. Steven R. Spangler, University of Iowa. Division of Plasma Physics, American Physical Society. To gain a perspective on gaseous media in space, first consider a more familiar gaseous medium….the Earth’s atmosphere. 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. Spectro. -polarimetry with the Turin . Lyot. -Filter. Silvano Fineschi . INAF – . Astrophysical. . Observatory. of . Torino, . Italy. Future . of . Polarimetry - . Brussels. (B) – 21-23 September 2015. “Topics in Solar Observation Techniques”. Lecture . 9:. Collisional lines: diagnostics & results. Spring 2016, Part . 1 . of 3: Off-limb coronagraphy & spectroscopy. Lecturer: Prof. Steven R. Cranmer. . 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. Fall . 2017. First Order Spectra. For a spectrum to be 1. st. order, the . D. n. between the chemical shifts of any given pair of nuclei must be much larger than the value of the coupling constant . 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. Piet Van Duppen. ISOLDE CERN, Switzerland. IKS-. K.U.Leuven. , Belgium. K.U. Leuven. University of Western Scotland, U.K. - . K.U.Leuven. , Belgium - SCK-CEN-Mol, Belgium - . U.Gent. , Belgium - . Commenius. 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. 2. Nuclear Magnetic Resonance Spectroscopy. After hydrogen, the most useful atom providing information is carbon-13.. The . overall intensity of a . 13. C signal is about 6400 . times . less than the intensity of an . MSSL, March 17-18, 2009. Frits Paerels. Columbia Astrophysics Laboratory. Columbia University, New York. cgs. units throughout!. Hα. Hβ. Hγ. Hδ. Wavelength (Å). NB: 1 Å = 10. -8. cm. E = . hc/λ. P. lasma . P. roperties (. ZAPP. ) Collaboration. Abstract. Astrophysically. -relevant laboratory plasmas with energy densities, volumes, and durations far beyond what was . previously possible . are being investigated using .