Solar Magnetic Activity
The far-side image display the seismic signature of magnetic activity on the side of the Sun that we cannot directly see from Earth. Darker regions indicate locations where there is an accumulation of magnetic field. Credits: NSO/GONG
HMI, from SDO, measures the Sun’s magnetic field over the entire visible disk with 1 arc second resolution. Credits: the Joint Science Operations Center (JSOC)
Solar Magnetic Cycles
This plot shows time vs. solar latitude of the radial component of the solar magnetic field, averaged over successive solar rotation. Sunspot signatures are clearly visible at low latitudes. Credits: the solar group at NASA Marshall Space Flight Center (NASA/MSFC).
A plot of four categories of field lines from the Potential-Field Source-Surface Models: open positive (outward) flux, open negative flux, and the tallest closed flux trajectories in blue. Also plotted is the original synoptic magnetogram, with flux density from white (maximum-strength positive flux) to black (maximum-strength negative flux). Credits: NSO/NISP.
Coronal Mass Ejections
Coronal mass ejections (“CMEs”)
Solar Wind – L1
Fast solar wind and large negative Bz values cause geomagnetic storms. Credits: NOAA/ACE
Celias onboard SOHO measures also solar wind at L1 and may complement ACE when plasma measurements from ACE are not reliable. Credits: CELIAS/MTOF Proton Monitor