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 colour of a star depends upon its
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 colour of a star depends upon its
The correct option is A surface temperature
The peak wavelength is inversely proportional to temperature of the star. Wavelength where the intensity peaks determines the color of that the star. The distribution of color shifts toward longer wavelengths as the temperature decreases. However, the star's radiation should falls in the visible spectrum for it to be visible. Thus correct answer is A.
The peak wavelength is inversely proportional to temperature of the star. Wavelength where the intensity peaks determines the color of that the star. The distribution of color shifts toward longer wavelengths as the temperature decreases. However, the star's radiation should falls in the visible spectrum for it to be visible. Thus correct answer is A.
