PPT-Polar Coronal Hole Variations Over Solar Cycle 23

Nishu Karna Mentor Dr William Dean Pesnell Code 671 SESI Program2010 Goddard Space Flight Center Date August 4 2010 Coronal Hole Large dark regions in the Suns corona that are cooler and have lower density plasma than average. J. . Todd . Hoeksema, . Solar Observatories Group @ H.E.P.L., Stanford University. SH13C-2278. Heliospheric Current Sheet. Image Courtesy . Keiji. Hayashi. hmi.stanford.edu/MHD. LASCO Corona With Polar Activity. 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. Louise Harra. lkh. @mssl.ucl.ac.uk. UCL Department of Space and Climate Physics. Mullard Space Science Laboratory. Extended solar minimum. Hinode X-ray corona. 2007 Oct. – 2009 Apr.. The solar wind is weaker… . 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. J. . Todd . Hoeksema, . Solar Observatories Group @ H.E.P.L., Stanford University. SH13C-2278. Heliospheric Current Sheet. Image Courtesy . Keiji. Hayashi. hmi.stanford.edu/MHD. LASCO Corona With Polar Activity. . 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. James A. . Klimchuk. . NASA Goddard Space Flight Center . Hinode. / SOT. Disclaimer:. This discussion concerns spicules as observationally distinct features.. Spicules may by just one manifestation of a larger sequence of events that generates waves and creates electric currents that could potentially give rise to substantial coronal heating.. 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. 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. . Zharkova V.V.. 1. , Shepherd S.J.. 2. and Popova E.. 3. 1 – . Northumbria. University, Newcastle, UK. 2 – Le Sorbonne . Universite. , France. 3 - . Skolkovo. Institute of Science and Technology, Russia . on. Stratospheric Circulation Patterns. Yonatan Givon. Chaim . Garfinkel. The Hebrew University of Jerusalem. Freddy and Nadine Hartman Institute of Earth Sciences. Solar variability. Well . understood impacts on climate:. Multipole. . Components. The figures show the solar magnetic field from May 1976 to the present, covering nearly 4 solar cycles. Cycle 24 was weak.. (Top): The. mean field. (MF) shows the Sun viewed as a star, where all magnetic signals from the visible disk are integrated. The MF typically peaks during solar maximum or a little later. Cycle 24 was relatively weak, but the peak was comparable to or larger than recent cycles and was reached 2015 as a consequence of the development of a large low-latitude unipolar region over several months. .