Abstract
An experiment to search for short-period oscillations in the solar corona was conducted during the total solar eclipse of 1995 October 24 at Kalpi, India. The intensity in the continuum, centred around 5500 Å and with a passband having a half-width of 240 Å, was recorded at a counting rate of 20 Hz using a thermoelectric-liquid cooled photomultiplier. The power-spectrum analysis of the data reveals that most of the power is contained in 6 frequencies below 0.2 Hz. A least-square analysis gives the periods of the 6 frequency components to be 56.5, 19.5, 13.5, 8.0, 6.1, and 5.3 s. These oscillations are found to be sinusoidal, and their amplitudes are found to lie in the rangełinebreak 0.2–1.3% of the coronal brightness. Assuming these oscillations to be fast magnetosonic modes, the calculations indicate the availability of enough flux for the heating of the active regions in the solar corona.
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Singh, J., Cowsik, R., Raveendran, A.V. et al. DETECTION OF SHORT-PERIOD CORONAL OSCILLATIONS DURING THE TOTAL SOLAR ECLIPSE OF 24 OCTOBER, 1995. Solar Physics 170, 235–252 (1997). https://doi.org/10.1023/A:1004943924584
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DOI: https://doi.org/10.1023/A:1004943924584