Solar Observer 1
HIGH-QUALITY FAST QPOs FROM MAGNETARS: AN ELECTRIC CIRCUIT MODEL A.Stepanov (Pulkovo Observatory, St.Petersburg) V.Zaitsev (Institute of Applied Physics,
II. MAGNETOHYDRODYNAMICS (Space Climate School, Lapland, March, 2009) Eric Priest (St Andrews)
Instructor Notes These images correspond to the layers of the Sun discussed in the Features of the Sun – 3D Sun lesson. Layers – Photosphere:
CH. 29.2 – Solar Activity CH. 29 - MARQUES. Terms to know… Sunspot Prominence Granules solar flare coronal mass ejection aurora.
National Science Foundation: NSF and Space Weather Rich Behnke Division of Atmospheric and Geospace Sciences June 21, 2011.
Magnetic fields in the photosphere and heliosphere: structure, statistical parameters, turbulent state Valentyna I. Abramenko Big Bear Solar Observatory.
Xu et al., ApJ 607, L131, 2004: or, how do flare footpoints work? First flare observations in the infrared 1.56 nominally is as deep as deep can be (the.
The Dynamic Evolution of Quiet Sun Magnetic Fields in the Solar Atmosphere W.P. Abbett, Space Sciences Laboratory, Univ. of California, Berkeley [email protected].
Andrea Dupree SAO/CfA New England Space Science Consortium (NESSC) March 1, 2006 Some Stellar Problems of Interest to Solar Physics Global properties.
Feb. 2006HMI/AIA Science Team Mtg.1 Heating the Corona and Driving the Solar Wind A. A. van Ballegooijen Smithsonian Astrophysical Observatory Cambridge,
