PPT-Hot Onsets of Solar Flares: GOES-R

Hugh S Hudson UC Berkeley and U of Glasgow Bibliography Bornmann P L Limits to derived flare properties ApJ 356 733 1990 Hudson HS Simoes JA Fletcher L Hayes L A and Hannah IG. 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… . RHESSI: a . statistical study. Jianxia. Cheng. . Jiong. . Qiu. , . Mingde. Ding, and . Haimin. Wang. outline. Introduction. Observations and data analysis. Properties of HXR spikes. summary. 1.Introduction. Ryan Payne. Advisor:. Dana . Longcope. Solar Flares. General. Solar flares are violent releases of matter and energy within active regions on the Sun.. Flares are identified by a sudden brightening in chromospheric and coronal emissions.. Solar Prominence. Sun Fact Sheet. The Sun is a normal G2 star, one of more than 100 billion stars in our galaxy.. . Diameter: . 1,390,000 km. (Earth 12,742 km or nearly 100 times smaller). Mass: . 1.1989 x 10. Individual . AR example: 8910. The only selection criterion imposed in this study is that the AR must be within 30 degrees of disk center. to minimize projection errors. See right for description of . Hugh Hudson. SSL, UC Berkeley and U. Of Glasgow. . 1. The Sun and its corona/wind. Solar . flares and . CMEs. Extreme events: new facts. “. Nanoflares. ”. The Sun itself. 2. It is not obvious from this sketch, but the very thin . Nick . Berkner. Goals. Develop a . Matlab. program to determine the tempo, meter and pulse of an audio file. Implement and optimize several algorithms from lectures and sources. Apply algorithm to a variety of musical pieces. detecting . flares, dimmings, and EUV waves . in near real-time on SDO/AIA images. Emil Kraaikamp. . (p), Cis Verbeeck – Royal Observatory of Belgium. 12. th. European Space Weather Week, Oostende, Belgium . M. Dominique. and I. . Dammasch. ESWW9, Brussels 2012. PROBA2: an ESA . microsat. L. aunched on November 9, 2009. 17 technology demonstrators + 4 scientific instruments. LYRA first light on January 6, 2010. SDO jEVE The EUV Variability Experiment EVE onboard the Solar Dynamics Observatory SDO has been obtaining unprecedented observations of solar variation on times scales of seconds during flares and ove Alexander Kosovichev (NJIT, U.S.A.) and Ivan Sharykin (IKI, Russia). Helioseismic response to solar flares . ("sunquakes") occurs due to localized force or/and momentum impacts observed during the flare impulsive phase in the lower atmosphere. . M. . Prijatelj. Carnegie Mellon University. Advisors: B. Chen, P. . Jibben. (SAO). Overview. Motivations. Standard Flare Model. Flux rope eruption. Magnetic reconnection. Flare emissions. Type III Radio Bursts. flares. in 2002. . B. Schmieder. 1;2. , R.-S. Kim. 2. , B. Grison. 3. , K. Bocchialini. 4. , R.-Y. Kwon. 2. . Key Points. :. . Analysis. . of the . chain. of . events. . (. flare. , CME, L1, SEP. Exoplanets. Kazunari. Shibata. . Kwasan. and . Hida. observatories, . Kyoto University. Hiroaki Isobe. Unit of Synergetic Studies for Space, Kyoto University. isobe@kwasan.kyoto. -. u.ac.jp. COSPAR2014, .