Magnetic fields in the photosphere and heliosphere: structure, statistical parameters, turbulent state Valentyna I. Abramenko Big Bear Solar Observatory.
SADS for SADs: Semi-Automatic Detection Software for Supra-Arcade Downflows Sabrina Savage 1, David E. McKenzie 1, Letisha McLaughlin 2 1 Montana State.
1.B – Solar Dynamo 1.C – Global Circulation 1.D – Irradiance Sources 1.H – Far-side Imaging 1.F – Solar Subsurface Weather 1.E – Coronal Magnetic Field.
Calculating Magnetic Energy in Active Regions Using Coronal Loops for AR 11092 and AR 11112 Presentation by, Joseph B. Jensen.
Spatio-Temporal Dynamics of Magnetic Fields and Flaring Productivity of Active Regions
Can the coronal field’s susceptibility to emergence-induced eruption be estimated? SSPVSE Discussion Group B, Wed., 19 Oct. 2005 B. Welsch, Space Sciences.
