Connecting the Corona to the Solar Wind
NASA ISFM (PI: Dr. N.M. Viall)
I am a co-Investigator on this project, which has been funded
for four years from 2017 through the NASA Individual Science
Funding Model program. My role is principally to analyze
datasets from the Hinode/EIS instrument, obtaining quantities
such as temperature, velocity and element abundance ratios that
can be compared to in situ measurements of the solar wind.
EIS mapper results
I wrote the "EIS Mapper" software in order
to graphically show the locations of EIS rasters on solar
full-disk images. For this project, I used EIS mapper to pick
out all EIS rasters that observed the Si X and S X coronal
emission lines that are needed to obtain the Si/S abundance
ratio (a good diagnostic of the FIP bias). In addition, the
rasters are required to have centers within solar-X positions
-200 to 200 arcsec since these have the best chance of showing
a connection to solar wind measurements.
EIS Mapper results for ISFM
Based on these results, the ISFM team identified key
observation days that should have a good connection to the solar
wind. On the team we refer to these as the "EIS events". I give
some notes on these data-sets below.
The EIS events
ISFM Team Presentations
Overview of EIS active region abundance results, 31-May-2008 [key, pdf]
EIS analysis update, 26-Sep-2019 [key, pdf]
EIS analysis update, 21-May-2020
5-minute flash talk for ISFM Showcase, 16-Mar-2021
Page maintained by Dr Peter R Young.