PPT-Techniques for Measuring Coronal Magnetic Fields

Motivation The Corona is a Magnetically Dominated System Coronal Magnetism is the Source of Space Weather Coronal Mass Ejections Energetic Particle Acceleration Coronal Heating Solar Wind Acceleration. 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 D.J. . Bercik. and J.G. . Luhmann. Space Sciences Lab, UC Berkeley. 1. FEW 2011, Aug 24. Introduction. The two most viable models of solar wind . energization. both ultimately appeal to convective granular flows. in Solar Disk Images . (and how to compare to models). Working Group Report. Nick Arge. .  . Rachel Hock. .  . Carl Henney. Definitions . (from our invited speakers). Coronal holes. : observable used as. 8.5 – Applications of Electric and Magnetic Fields. Agenda. Quiz. Lesson on Section on 8.5. Lots of Video’s. Story Time. Cyclotron Particle Accelerator. http://. www.youtube.com/watch?v=cNnNM2ZqIsc. Dayal Wickramasinghe and Lilia . Ferrario. Australian National University. Canberra. . . The chemically peculiar . Ap. , Bp stars ( ~ 1.8 -5 . M. sun. ) are magnetic, and . have ordered large. scale fields, . Andrii Neronov. University of Geneva. Durrer. & AN, . A&ARev. , 21, 62 (2013) . Overview . Magnetic fields in astronomy and cosmology. Characterization. of cosmological magnetic fields. Generation. to . their CME . progenitors (Wed AM). Two major efforts are under way to address the structure of CMEs that hit the Earth, and . B. z. in particular, with the long-term goal of better forecasting geomagnetic storms:. Some models of coronal heating suppose that convective motions at the photosphere shuffle the . footpoints. of . coronal magnetic fields and thereby inject sufficient magnetic energy upward to account for observed coronal . . 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; . at HIMAC synchrotron. Hiroshi Uchiyama . #,A). , Masahiro Kawashima . A). , . Shunsuke. Saito . A). , Izumi Kobayashi . A). , . Tadahiro. . Shiraishi. . A). ,. Chihiro. Kobayashi . A). , Eiichi . all magnets have magnetic poles – . . points at the ends of a magnet that have opposing magnetic qualities. all magnets have a north pole and south pole that are magnetically opposite. like poles repel and unlike poles attract. Systems. Frank Barnes.  . Department of Electrical, Computer, and Energy Engineering, University of Colorado, Boulder, Colorado. Acknowledgement. Ben Greenebaum. . Lucas Portelli . Carlos Martino . UV . Hanle. Effect . Coronal Magnetic Field & Plasma Dynamics . N.-E. . R. aouafi . Coronal Zeeman effect. Limitations. . Few . applications because of the weakness. of . the coronal magnetic field and of coronal signal. the Earth's magnetic field at a given location. Objetive. The . objective of the activity is to measure the magnetic field of the Earth . an . a given . area. The relation . between . maximum . and minimum .