Intensity Oscillation in the Corona as Observed during the Total Solar Eclipse of 29 March 2006 |
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| Authors: | Jagdev Singh S S Hasan G R Gupta D Banerjee S Muneer K P Raju S P Bagare R Srinivasan |
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| Institution: | 1.Indian Institute of Astrophysics,Bangalore,India;2.Joint Astronomy Programme,Indian Institute of Science,Bangalore,India |
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| Abstract: | We obtained the images of the eastern part of the solar corona in the Fe xiv 530.3 nm (green) and Fe x 637.4 nm (red) coronal emission lines during the total solar eclipse of 29 March 2006 at Manavgat, Antalya, Turkey. The images
were obtained using a 35 cm Meade telescope equipped with a Peltier-cooled 2k × 2k CCD and 0.3 nm pass-band interference filters
at the rates of 2.95 s (exposure times of 100 ms) and 2.0 s (exposure times of 300 ms) in the Fe xiv and Fe x emission lines, respectively. The analysis of the data indicates intensity variations at some locations with period of strongest
power around 27 s for the green line and 20 s for the red line. These results confirm earlier findings of variations in the
continuum intensity with periods in the range of 5 to 56 s by Singh et al. (Solar Phys.
170, 235, 1997). The wavelet analysis has been used to identify significant intensity oscillations at all pixels within our field of view.
Significant oscillations with high probability estimates were detected for some locations only. These locations seem to follow
the boundary of an active region and in the neighborhood, rather than within the loops themselves. These intensity oscillations
may be caused by fast magneto-sonic waves in the solar corona and partly account for heating of the plasma in the corona. |
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