Coronal Heating and Solar Wind Acceleration Mechanisms
Technical Report,18 Aug 2015,17 Nov 2017
The University of New Mexico Albuquerque United States
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The project goal is to determine whether the magnetic expansion factor plays a physical role in solar wind acceleration or whether it simply serves as a proxy that can be used to distinguish between solar wind with slow 300 - 500 kms and fast 650 kms speeds. During the period of performance, a methodology has been developed, through which suitable pseudostreamers can be identified and their resulting solar wind speeds can be determined. This is done applying the existing Wang-Sheeley-Arge WSA model output produced with Air Force Data Assimilative Photospheric Flux Transport ADAPT input maps, allowing the determination of the time of arrival at the specified spacecraft of the exact parcel of solar wind that left the pseudostreamer. We have shown that the methodology outlined is useful to identify unambiguous cases where spacecrafts like ACE are magnetically connected to pseudostreamers, and it can also be used to compare the field line expansion factors with the associated terminal solar wind speed.