Spectroscopic Observation of Oscillations in the Corona During the Total Solar Eclipse of 22 July 2009

Details Spectroscopic Observation of Oscillations in the Corona During the Total Solar Eclipse of 22 July 2009 Spectroscopic Observation of Oscillations in the Corona During the Total Solar Eclipse of 22 July 2009

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011soph..270..213s&link_type=abstract

Solar Physics, Volume 270, Issue 1, pp.213-233

Physics

2

Coronal Heating, Emission Lines, Mhd Waves, Oscillations, Solar Corona

Scientific paper

We performed high resolution spectroscopy of the solar corona during the total solar eclipse of 22 July 2009 in two emission lines: the green line at 5303 Å due to Fe xiv and the red line at 6374 Å due to Fe x, simultaneously from Anji (latitude 30°28.1' N; longitude 119°35.4' E; elevation 890 m), China. A two-mirror coelostat with 100 cm focal length lens produced a 9.2 mm image of the Sun. The spectrograph using 140 cm focal length lens in Littrow mode and a grating with 600 lines per millimeter blazed at 2 μm provided a dispersion of 30 mÅ and 43 mÅ per pixel in the fourth order around the green line and third order around the red line, respectively. Two Peltier cooled 1k × 1k CCD cameras, with a pixel size of 13 μm square and 14-bit readout at 10 MHz operated in frame transfer mode, were used to obtain the time sequence spectra in two emission lines simultaneously. The duration of totality was 341 s, but we could get spectra for 270 s after a trial exposure at an interval of 5 s. We report here on the detection of intensity, velocity, and line width oscillations with periodicity in the range of 25 - 50 s. These oscillations can be interpreted in terms of the presence of fast magnetoacoustic waves or torsional Alfvén waves. The intensity ratios of green to red emission lines indicate the temperature of the corona to be 1.65 MK in the equatorial region and 1.40 MK in the polar region, relatively higher than the expected temperature during the low activity period. The width variation of the emission lines in different coronal structures suggests different physical conditions in different structures.

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