Coordinated Observations

1. Determine empirical constraints on theoretical models of the solar wind from particular coronal structures from coordinated UVCS, LASCO and CELIAS observations.
2. For various coronal structures, derive observational constraints on models describing the freezing-in temperature, ionization state and abundance of hydrogen, oxygen, silicon, magnesium and iron. Compare the results with those obtained from CELIAS ``in situ" measurements.
3. Derive the geometry of coronal structures from 2D scans with the UVCS white light channel and LASCO observations.
4. Map different solar wind streams from their source region into interplanetary space through coordinated and simultaneous ground and space based observations.
5. Perform coordinated observations with UVCS, MDI magnetograms and ground based magnetograms; for example, determine the magnetic fields in polar coronal holes and plumes.
6. Used coordinated observations with UVCS, CDS, EIT and SUMER to trace the evolution of coronal structures.