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Updated: Aug 3, 2026

Surface Renewal: An Advanced Micrometeorological Method for Measuring and Processing Field-Scale Energy Flux Density Data
Published on: December 12, 2013
Solar wind outflow and the chromospheric magnetic network
1Southwest Research Institute, 1050 Walnut Street, Boulder, CO 80302, USA. Max-Planck-Institut fur Aeronomie, D-37191 Katlenburg-Lindau, Germany. Institut d'Astrophysique Spatiale, Unite Mixte CNRS- Universite Paris XI, 91405 Orsay, France. Ins.
Abstract:
Observations of outflow velocities in coronal holes (regions of open coronal magnetic field) have recently been obtained with the Solar and Heliospheric Observatory (SOHO) spacecraft. Velocity maps of Ne7+ from its bright resonance line at 770 angstroms, formed at the base of the corona, show a relationship between outflow velocity and chromospheric magnetic network structure, suggesting that the solar wind is rooted at its base to this structure, emanating from localized regions along boundaries and boundary intersections 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.
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