PPT-Observations and Magnetic Field Modeling of the Flare/CME E

Yingna Su Bernhard Kliem Adriaan van Ballegooijen Vincent Surges Edward Deluca Presentation at Hinode5 on Oct 13 2011 Cambridge USA Overview Part I We construct static magnetic field models using the flux rope insertion method to compare with observations prior to and at the onset of the event . Martin Luther King Jr Day Monday Jan 2 Unaffected and will run on a normal schedule IRU57347WKH57347QHW57347GD57526V57347WUDGH57347GDWH 3UHVLGHQWV5752657347D Mo nday Feb 1 Unaffected and will run on a normal schedule IRU57347WKH57347QHW57347GD57526V 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. 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. Abstract. We observed a filament eruption, whose shape is like a dandelion, associated with the solar flare that occurred on 2011 February 16 at the active region NOAA 11158. The H. a. . full disk images of the flare were taken by FMT. of . Magnetic. Setting in . Flare. Productive Active . Regions. Yixuan. Li. Space Weather Research Lab. New Jersey Institute of Technology. Introduction. March 10, 2010. In recent years, it has been widely reported that photosphere magnetic fields can experience some rapid, significant and permanent changes during X-and M-class flares. . THREE PHASES OF PARTICLE ACCELERATION. FLARE IMPULSIVE PHASE (. FIRST. ) FLARE LATE PHASE (. SECOND. ) . CME. SHOCK. IMPULSIVE SEP EVENT. GRADUAL SEP EVENT. FLARE. CME SHOCK. NOTE: NO Flare. NO/very little scattering except near shock. HMI Observations of Solar Flares in Solar Cycle . 24. . Todd Hoeksema, Monica . Bobra. , . Sebastien. . Couvidat. , . and . Xudong. Sun. . Stanford University. SHARP Parameter Table. HMI Data Series: hmi.sharp_720s. in . the Houston Region. Wenxian. Zhang, Erin E. . Tullos. , . Yongtao. . Hu. , . Athanasios. . Nenes. , Armistead G. Russell. CMAS Annual Meeting. Oct 29, 2014. Acknowledgements. Funding Support:. Crusoe Energy Systems Inc. Cully Cavness Co - Founder, President and COO 200 - 500 million cubic feet of gas flared daily in North Dakota NEW TECHNOLOGY CONVERTS WASTED NATURAL GAS INTO COMPUTING ▪ 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. N. Gopalswamy, H. Xie, S. Yashiro, and S. Akiyama. NASA/GSFC. SPD Meeting July 8 -11, 2013 Bozeman, Montana. ribbons. . r. . P. Longcope et . al. 2007. Longcope & Beveridge, 2007. Qiu et al. 2007. Jing et al. . ApJ. , 2010, April 20 v713 issue, in press. Eq. (1). Free Magnetic Energy . E. free. Soft X-ray Flare Index FI. Eq. (2). where . . is the length of time window (measured in days), and I. quasi-periodic . pulsations in solar flares. Dong Li. lidong@pmo.ac.cn. Purple Mountain Observatory, CAS. O. utlines. 4-minute QPPs detected from spectra and images (Li et al., 2015, . ApJ. ). 1-minute QPPs . revealing the pre-eruption flux ropes?. Louise Harra, Sarah Matthews, Len Culhane, Mark Cheung, E. Kontar and Hiro Hara. Non-thermal velocity - what does it tell us?. FWHM. 2. = (instr. fwhm. ). 2 .