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 . by Brian T. Welsch & George H. Fisher. Space Sciences Lab, UC-Berkeley. Permanent changes in . photospheric. magnetic fields have been observed to occur during solar flares (e.g., . Sudol. & Harvey 2005, Wang & Liu 2010, Petrie & . 13th May 2005 Solar Flare. William M.R. Simpson, Angela Des . Jardins. University of St. Andrews, Montana State University. Contact. :. Email:. www. : . William M. R. Simpson. wmrs2@st-and.ac.uk. http://solar.physics.montana.edu/home/www/REU/2009/wsimpson . Christopher F. . McKee. MFU V Corsica. Oct 7, 2015. With: Pak-. Shing. Li. Richard Klein. IN STAR FORMATION. Partial support provided by the National Science Foundation and NASA. OUTLINE. III. Observing interstellar magnetic fields on a computer (LMK). 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. Egidio Landi Degl’Innocenti. Dipartimento di Fisica e Astronomia. Università di Firenze, Italia. Banja Koviljaca, May 13-17, 2013. 9th Serbian Conference on Spectral Line Shapes in Astrophysics. Line shapes I. . . Their cores usually have a quite simple structure that makes them ideally suited for studies of isolated low-mass star formation (Bok . 1947, . ApJ. , 105, 255. ).. BOK GLOBULES. LARGE BOK GLOBULE CB34. . 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; . 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. . 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. Joel Allred (NASA GSFC) --Team 1. Phil Judge (HAO) & Lucia . Kleint. . (Original PI)-- Team 2 . Alexander . Kosovichev. (NJIT/Stanford) –Team 3. Chang Liu (NJIT)--Team 4. 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 .