Like the solar spectrum the spectra of stars show a continuous spectrum on which dark absorption lines are superimposed. The inner layer (called the photosphere) of the star emits radiations of all wavelengths, producing a continuous spectrum. When these radiations pass through the outer, relatively cooler, layer of the star, the radiation of certain wavelengths are selectively absorbed by this layer. This explains the dark lines in the spectrum of a star. The dark lines are characteristic 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 Wien's 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 2.89×10−3mK .
The spectrum of light received from a star is a
Like the solar spectrum the spectra of stars show a continuous spectrum on which dark absorption lines are superimposed. The inner layer (called the photosphere) of the star emits radiations of all wavelengths, producing a continuous spectrum. When these radiations pass through the outer, relatively cooler, layer of the star, the radiation of certain wavelengths are selectively absorbed by this layer. This explains the dark lines in the spectrum of a star. The dark lines are characteristic 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 Wien's 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 2.89×10−3mK .
The spectrum of light received from a star is a
The correct option is D absorption line spectrum
The received radiation is in lines and not in bands, because specific wavelengths are obtained and not a continuous range of wavelengths. Hence it is a radiation line spectrum, not a radiation band spectrum.
Since certain lines of the continuous spectra are absorbed by the photosphere of star, the spectrum obtained is an absorption spectrum, not an emission spectrum. (only certain lines are absorbed). Hence it is an absorption spectrum.
The received radiation is in lines and not in bands, because specific wavelengths are obtained and not a continuous range of wavelengths. Hence it is a radiation line spectrum, not a radiation band spectrum.
Since certain lines of the continuous spectra are absorbed by the photosphere of star, the spectrum obtained is an absorption spectrum, not an emission spectrum. (only certain lines are absorbed). Hence it is an absorption spectrum.
