PPT-Simulating Shocks in Solar Flares

Daniel Gordon Adviser Dana Longcope Introduction Magnetic reconnection is a significant mechanism for phenomenon involving high energy release such as solar flares Postreconnection field lines act like elastic bands under tension. 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 . Rami Vainio. University of Helsinki, Department of Physics, Finland. University of Turku, Department of Physics and Astronomy, Finland. SPACECAST . Stakeholder Meeting. , . BAS, 7 February 2014. Solar energetic particle events. 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 . 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. . ?. R. . Mochkovitch. , F. Daigne, R. . Hascoët. (IAP). Basic properties of flares:. from a few 10 s to a few 10. 5. s, superimposed . . to underlying AG light curve. shape and spectral evolution comparable to that of prompt pulses . 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.