PPT-Free Magnetic Energy and Flare Productivity of Active Regions

Jing et al ApJ 2010 April 20 v713 issue in press Eq 1 Free Magnetic Energy E free Soft Xray Flare Index FI Eq 2 where is the length of time window measured in days and I. 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 & . Frank Hill. NSO. SPRING Workshop. Nov. 26, 2013. Science drivers. Understand dynamics below active regions – vorticity, divergence. Continue observations of large-scale zonal and meridional flows underlying the dynamo and solar activity. 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 . . Observed, estimated, and predicted daily geomagnetic . AFr. -indices (A-indices from Fredericksburg, VA), and daily AP-indices (planetary A-indices). . Ap. indices are estimated in near-real time using a network of up to 12 North American stations. . 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 . Yingna. Su. Bernhard . Kliem. , . Adriaan. van . Ballegooijen. , Vincent Surges, Edward Deluca. Presentation at Hinode-5 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. . 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. . Let’s start with a reminder and a . word of caution. : . Goal: Using magnetic model systems to study interaction phenomena . We know from thermodynamics that Gibbs free energy:. G=G(T,H). and. If, without further thought, we use our standard approach . . Observed, estimated, and predicted daily geomagnetic . AFr. -indices (A-indices from Fredericksburg, VA), and daily AP-indices (planetary A-indices). . Ap. indices are estimated in near-real time using a network of up to 12 North American stations. . —a measure of X-ray absorption at several positions around the head, maps tissue density. Magnetic resonance imaging (MRI). gives higher resolution images in three steps:. Strong magnets cause protons in brain tissue to line up in parallel. A pulse of radio waves knocks protons over. Protons reconfigure themselves, emitting radio waves that differ by tissue density.. 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. Magnetic . Energy. . once an ancient mystery, is now recognized as the strongest natural force in the universe. . . Our Earth. . is a giant magnet and all life developed under the influence of the earth’s magnetic field. . current. area enclosed by current loop. Orbiting electrons form a current loop which give rise to a magnetic field.. For the electron, the Bohr . magneton is the simplest model . possible . to the smallest possible current to the smallest possible . 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.