The black lines in the solar spectrum during | vedclass

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(B) Kirchhoff's Law states that good emitters are good absorbers at a given temperature. In the solar spectrum,the dark lines known as Fraunhofer line

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Kirchhoff's law

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(B) Kirchhoff's Law states that good emitters are good absorbers at a given temperature. In the solar spectrum,the dark lines known as Fraunhofer lines are formed because the cooler gases in the Sun's outer atmosphere (chromosphere) absorb specific wavelengths of light emitted by the hotter inner layers (photosphere). During a solar eclipse,when the bright photosphere is obscured by the Moon,the chromosphere becomes visible. At this moment,the emission spectrum of the chromosphere is observed,showing bright lines at the exact same wavelengths as the dark Fraunhofer lines. This phenomenon is a direct consequence of Kirchhoff's law,which explains why the same material that absorbs light at a specific wavelength will also emit light at that same wavelength.

The black lines in the solar spectrum during a solar eclipse can be explained by

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