Like the solar spectrum the spectra of stars show a continuous spectrum on which dark aborption lines are superimposed. The inner layer (called the photosphere) of the star emits radiations of all wavelengthts, producing a continuous spectrum. When these radiations pass through the outer, relatively cooler, layer of the star, the radiations of certain wavelengths are selectively absorbed by this layer. This explains the dark lines in the spectrum of a star. The dark lines are charactreristic of the substances present in the outer layer of the star.The surface temperature T of a star can be estimated by measuring the wavelengths λm at which the intensity of the emitted radiation is maximum and then using Wiens displacement law which states that λm x T = b where b is a constant called Wiens constant and the above relation is called Wiens Displacement Law which states that as the temperature increases, the maximum intensity of emission shifts (or is displaced) towards the shorter wavelengths. The value of constant b has been found experimentally to be 2.89 x 10−3mK .
The dark lines in the solar spectrum are due to the
Like the solar spectrum the spectra of stars show a continuous spectrum on which dark aborption lines are superimposed. The inner layer (called the photosphere) of the star emits radiations of all wavelengthts, producing a continuous spectrum. When these radiations pass through the outer, relatively cooler, layer of the star, the radiations of certain wavelengths are selectively absorbed by this layer. This explains the dark lines in the spectrum of a star. The dark lines are charactreristic of the substances present in the outer layer of the star.The surface temperature T of a star can be estimated by measuring the wavelengths λm at which the intensity of the emitted radiation is maximum and then using Wiens displacement law which states that λm x T = b where b is a constant called Wiens constant and the above relation is called Wiens Displacement Law which states that as the temperature increases, the maximum intensity of emission shifts (or is displaced) towards the shorter wavelengths. The value of constant b has been found experimentally to be 2.89 x 10−3mK .
The dark lines in the solar spectrum are due to the
The correct option is C absorption of corresponding wavelengthts by the outer layers of the sun
The spectrum emitted by the sun is a continuous spectrum, and certain lines would be absorbed by the outer layers of the sun and the other lines would pass through unaffected.
Thus, we would obtain a continuous spectrum, with a few lines omitted (dark lines). These are the dark lines in the solar spectrum and they are due to the absorption of those wavelengths by the outer surface of the sun.
The spectrum emitted by the sun is a continuous spectrum, and certain lines would be absorbed by the outer layers of the sun and the other lines would pass through unaffected.
Thus, we would obtain a continuous spectrum, with a few lines omitted (dark lines). These are the dark lines in the solar spectrum and they are due to the absorption of those wavelengths by the outer surface of the sun.
