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In astronomy, absorption lines are dark lines observed in the spectrum of a hot object, resulting from the presence of absorbing materials along the line of sight. These lines are caused by atoms absorbing light emitted by the source at specific and well-defined wavelengths.
The absorption lines in a spectrum provide valuable information about the composition of the object being observed. For instance, the Sun’s spectrum exhibits numerous absorption lines known as Fraunhofer lines. These lines allow astronomers to study the composition of the Sun’s outer layers by identifying the elements that absorb light at those specific wavelengths.
Similarly, absorption lines in the spectra of stars offer insights into the composition of interstellar gas and dust. By analyzing the absorption lines in stellar spectra, astronomers can determine the types of elements present in the outer layers of stars and the intervening interstellar medium.
The study of absorption lines plays a crucial role in astrophysics, aiding in the understanding of celestial objects’ chemical composition, temperatures, and motion.