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High Resolution Solar Observations at Three Frequencies: 1424 MHz, 696 MHz and 408 MHz

  • D. G. Cole (a1), R. F. Mullaly (a1) and A. Watkinson (a1)


During the period 1966 July 12 to August 5 observations were made of the Sun at three radio observatories. The instruments used were the east-west arm of the Mills cross at Molonglo (408 MHz) and the Christiansen cross at Fleurs (696 MHz and 1424 MHz). The aim of these observations was to study the discrete sources of the slowly varying component of solar radio emission, while activity was comparatively quiet. The three frequencies enabled the variation of source structure with height of solar atmosphere to be studied. It has been pointed out by Swarup et al., and Christiansen et al. that the determination of the frequency dependence of these discrete sources is important for defining the physical mechanisms causing the radio emission.



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1 Swarup, G., Kakinuma, T., Covington, A. E., Harvey, G. A., Mullaly, R. F., and Rome, J., Astrophys. J., 137, 1251 (1963).
2 Christiansen, W. N., Mathewson, D. S., Pawsey, J. L., Smerd, S. F., Boischot, A., Denisse, J. F., Simon, P., Kakinuma, T., Dodson-Prince, H., and Firor, J. W., Ann. d’Astrophys., 23, 75 (1960).
3 Kundu, M. R., ‘Solar Radio Astronomy’, Interscience Publishers, New York, 1965.


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