Solar wind outflow and the chromospheric magnetic network

Observations of outflow velocities in coronal holes (regions of open corona l magnetic field) have recently been obtained with the Solar and Heliospher ic Observatory (SOHO) spacecraft. Velocity maps of Ne7+ from its bright res onance line at 770 angstroms, formed at the base of the corona, show a rela tionship between outflow velocity and chromospheric magnetic network struct ure, suggesting that the solar wind is rooted at its base to this structure , emanating from localized regions along boundaries and boundary intersecti ons of magnetic network cells. This apparent relation to the chromospheric magnetic network and the relatively large outflow velocity signatures will improve understanding of the complex structure and dynamics at the base of the corona and the source region of the solar wind.