Physics
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh13a..05r&link_type=abstract
American Geophysical Union, Spring Meeting 2004, abstract #SH13A-05
Physics
2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma
Scientific paper
Following the lead of K. Shatten in work done for Solar Wind 2, we use the assumption of a stationary heliospheric structure to find the magnetic field pattern over significant regions of the ecliptic plane under quiet solar conditions. A measured dataset is time lagged to form sets for different heliolongitudes, and each of these sets is then kinematically projected to yield radial coverage. This can be done with one spacecraft (or OMNI data), but at times data from two Helios spacecraft can be combined with the 1 AU data to yield a richer set that also checks the consistency of the assumption of stationarity. The resulting pictures will be qualitatively compared to simulations. We will also examine to what extent these methods can be applied to Ulysses data to get a better view of fields over the solar poles, as well as combining that data with measurements from constellations near the Earth (including Cluster, Wind, ACE, and Geotail) for a more global view. This work will help us to sort out spatial and temporal effects in the heliosphere, and will be relevant to predicting the geoeffectiveness of solar events.
Eastwood Jonathan
Goldstein Michel L.
Roberts Dale
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