stjärnspektrumet

Stjärnspektrumet refers to the continuous spectrum of light emitted by a star, which contains absorption lines at specific wavelengths. These lines are caused by the elements in the star's atmosphere absorbing photons of particular energies, corresponding to the energy differences between electron orbitals in those atoms. By analyzing the patterns and strengths of these absorption lines, astronomers can determine the chemical composition, temperature, and even the radial velocity of a star.

The spectral classification system, often represented by letters like O, B, A, F, G, K, and M, is based on the temperature of a star, which directly influences its spectrum. Hotter stars, like O and B types, exhibit strong lines of ionized helium and hydrogen, while cooler stars, like G and K types (our Sun is a G-type star), show more lines of neutral metals and molecules. M-type stars, the coolest, display prominent molecular bands.

The study of stjärnspektrumet is a fundamental tool in astrophysics, providing crucial information for understanding stellar evolution, the formation of galaxies, and the universe as a whole. It allows us to deduce properties that cannot be directly measured, such as a star's age and its magnetic field strength, indirectly through detailed spectral analysis.