At the time of a total solar eclipse,the spec | vedclass

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(D) Fraunhofer lines are dark absorption lines observed in the solar spectrum caused by the absorption of specific wavelengths by the cooler gases in

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All Fraunhofer lines changed into brilliant colours

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(D) Fraunhofer lines are dark absorption lines observed in the solar spectrum caused by the absorption of specific wavelengths by the cooler gases in the Sun's atmosphere (the photosphere).During a total solar eclipse,the Moon blocks the bright photosphere of the Sun.This allows the light from the chromosphere,which is a hotter and thinner layer of the Sun's atmosphere,to be observed.The chromosphere emits light through emission,which produces bright emission lines at the exact same wavelengths where the dark absorption lines (Fraunhofer lines) were previously observed.Therefore,the dark Fraunhofer lines are replaced by bright,brilliant emission lines.

At the time of a total solar eclipse,the spectrum of solar radiation would be:

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