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 [key, pdf]


Page maintained by Dr Peter R Young.