PPT-Modelling the Effect of Magnetic Field Variation on Solar Flares

Introduction Solar flares occur when energy is converted into xrays heat amp supersonic fluid motion Energy is stored in magnetic filed lines Electric field changes connectivity of magnetic field lines and the energy is released. In addition magnetic fields create a force only on moving charges The direction the magnetic field produced by a moving charge is perpendicular to the direction of motion The direction of the force due to a magnetic field is perpendicular to the dir Flows . &. Flare Forecasting . tentative plans for Welsch & . Kazachenko. Topics. 0. Why do should . photospheric. electric or velocity fields . E. . or . v. matter for flares?. Previous work with B. The Sun and the Stars. The Sun and the Stars. Limb darkening. The surface of the sun does not have uniform brightness, it appears bright toward the centre, darker towards the edges, and the colour is redder, an effect known as Limb darkening - why?. a physical perspective . . 1. Philip Judge, . . High Altitude Observatory, NCAR. "Double, double, toil and trouble;. Fire burn, and cauldron bubble!". -- . Dandan Ye. Contents. Paper review: . 2005 J.J. Sudol and J.W. Harvey. ‘. Longitudinal magnetic field changes accompanying . . solar flares’. My work . about. flare-related magnetic field evolutions to the X1.8 flare on 2012.10.23. 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 . 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 . . What Photospheric Magnetograms Can Teach Us About Solar Activity. Brian T. Welsch, Bill Abbett. 1. , Dave Bercik. 1. , . George H. Fisher. 1. , Yan Li. 1. , and Pete W. Schuck. 2 . 1. Space Sciences Lab, UC-Berkeley; . basic concepts and magnetic topology . Anna (. Ania. ) . Malanushenko. Plasma. Is matter…. Mass is conserved. Momentum is conserved. Energy is conserved. …ionized and in magnetic field. Obeys Maxwell’s equations. Tonight's agenda . Our focus is always somewhere else. A Secure Development Lifecycle?. Threat Modelling. Taking it in your STRIDE. How . to get everyone involved. How to win at Poker. Q & A. Fin. ?. 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.