Solar Physics General Session
Diagnostics of the solar coronal hole plasma during the 2015 total solar eclipse observation: Temperature, electron density, and solar wind acceleration
Joe Hutton
Shadia Habbal (IfA Hawaii), Huw Morgan (Aberystwyth Uni.), Enrico Landi (Uni. Michigan), Miloslav Druckmuller (Brno Uni.), & Nathalia Alzate (Aberystwyth Uni.)
Aberystwyth University
Using data from the total solar eclipse of 2015 March 20 at 10:10:40 UT on the Norwegian archipelago of Svalbard, a temperature map of the solar corona is created, which is the first (the authors believe) of it's kind to accurately calculate the temperature of the solar corona out to two solar radii. This is achieved using ratios of the Fe XI (789.2 nm) and Fe XIV (530.3 nm) spectral lines, which are cross-calibrated with the total brightness observations of the Large Angle Spectrometric Coronagraph instrument C2 on board the Solar and Heliospheric Observatory. The electron density in the corona is also estimated by taking an inversion of the calibrated ion emissions. These are powerful tools for diagnostics of the coronal holes present during the eclipses. Through comparisons with corresponding observations by the Hinode EUV imaging spectrometer, it is possible to examine electron density as a function of height out to two solar radii in the corona, as well as calculating the acceleration of the solar wind originating from these regions.


09:00 - 10:30
EX - LT3 (320)