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During the total solar eclipse at Akademgorodok, Siberia, Russia, in 1 August2008, we imaged the flash spectrum with a slitless spectrograph. We havespectroscopically determined the duration of totality, the epoch of the 2nd and3rd contacts and the duration of the flash spectrum (63 s during ingress and 48s during egress). Here we compare the 2008 flash spectra with those that wesimilarly obtained from the total solar eclipse of 29 March 2006, atKastellorizo, Greece. Any changes of the intensity of the corona emissionlines, in particularly those of [Fe X] and [Fe XIV], could give us valuableinformation about the energy content of the solar corona and the temperaturedistribution of the corona. The results show that the high-ionization state,the [Fe XIV] emission line, was much weaker during the 2008 eclipse, indicatingthat following the long, inactive period during the solar minimum, there was adrop in the overall temperature of the solar corona.

solar physics

A Comparison of the Red and Green Coronal Line Intensities at the 29  March 2006 and the 1 August 2008 Total Solar Eclipses: Considerations of the  Temperature of the Solar Corona