Slide 1 UCL DEPARTMENT OF SPACE & CLIMATE PHYSICS SPACE PLASMA PHYSICS GROUP A Potential Mission Concept for the M3 2022 Launch: Investigation of MagnetoPause Activity…

The Independency of Stellar Mass-Loss Rates on Stellar X-ray Luminosity and Activity Space Telescope Science Institute – 2012 The stellar wind determines the stellar mass…

An Introduction to the NIMROD Fusion Magnetohydrodynamics Simulation Project Prof. Carl Sovinec Department of Engineering Physics University of Wisconsin-Madison presented…

195 Ã image â behind 195 Ã image â Sun- Earth line â SOHO/ EIT image 195 Ã image â ahead SECCHI Extreme Ultraviolet Imager (EUVI) In Space Weather, you get ahead by…

The Rise of Solar Cycle 24: Magnetic Fields from the Dynamo through the Photosphere and Corona and Connecting to the Heliosphere Part 1: Interior and Photosphere Subsurface…

Observational Evidence of Post-CME Current Sheets – Mostly White Light New STEREO/SECCHI Processing for Heliospheric Transients David F. Webb ISR, Boston College, MA, USA…

Slide 1 The Photosphere & CME Initiation “We would like us to give us your views on the application of vector field and photospheric flows data to the CME initiation…

195 Ã image â behind 195 Ã image â Sun- Earth line â SOHO/ EIT image 195 Ã image â ahead SECCHI Extreme Ultraviolet Imager (EUVI) In Space Weather, you get ahead by…

Heliospheric Magnetic Field 1835-2010 Leif Svalgaard Stanford University, CA [email protected] http://www.leif.org/research http://arxiv.org/ftp/arxiv/papers/1002/1002.2934.pdf…