Abstract
PRESENT estimates of the electron density in the solar corona are based on the measurements during an eclipse of the optical radiation which originates in the photosphere and is scattered in the corona1. These measurements and their interpretation present considerable difficulties, particularly when attempts are made to determine the electron density in the outermost layers of the corona2,3. In this communication a possible method of determining the electron density at different heights in the corona is suggested, which should allow the exploration of regions where the density is as low as 104 cm.−3.
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References
Baumbach, S., Astr. Nach., 263, 121 (1937).
Allen, C. W., Mon. Not. Roy. Astro. Soc., 107, 426 (1947).
Van der Hulst, H. C., Nature, 163, 24 (1949).
Stanier, H. M., Nature, 165, 354 (1950).
Machin, K. E., Nature, 167, 889 (1951).
Smith, F. G., Nature, [168, 555 (1951)].
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MACHIN, K., SMITH, F. A New Radio Method for Measuring the Electron Density in the Solar Corona. Nature 168, 599–600 (1951). https://doi.org/10.1038/168599b0
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DOI: https://doi.org/10.1038/168599b0
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