Automated direct measurements of Alfvenic wave energy flux in coronal holes: constraints for solar wind acceleration models.
Abstract
A full understanding of the solar wind is critical for predicting geomagnetic storms and forecasting space weather, and so there is a need to understand the physical mechanism(s) behind solar wind acceleration. Currently, a number of models utilise Alfvenic wave turbulence to enable acceleration of the solar wind. However, results from a recent AFOSR pilot study indicate that Alfvenic waves as resolved by the Solar Dynamics Observatory/Atmospheric Imaging Assembly may not be the dominant energy source for fast solar wind acceleration in the open-field corona, potentially placing limitations on the suitability of Alfvenic wave turbulence for explaining acceleration.
Document Details
- Document Type
- DoD Grant Award
- Publication Date
- Mar 23, 2016
- Source ID
- FA95501610032
Entities
People
- James Mclaughlin
Organizations
- Air Force Office of Scientific Research
- Northumbria University
- United States Air Force