Linked from

The 11 pages that link to Spectral line broadening, each with the reason it gives.

• Doppler effectCompared with: Broadening can signal a distribution of motions rather than one bulk Doppler shift.

• Stellar classificationRelated: Line widths can complicate classification and also reveal conditions in stellar atmospheres.

• Astronomical spectroscopyRelated: Line widths constrain temperature, turbulence, pressure, and rotation in emitting regions.

• Atomic spectrumRelated: Motion, collisions, and finite state lifetimes give atomic lines measurable widths.

• Fraunhofer linesRelated: The shapes and widths of solar absorption lines encode temperature, pressure, and motion.

• Hydrogen spectrumRelated: Real hydrogen lines have finite widths from motion, collisions, and finite excited-state lifetimes.

• AltairRelated: Line profiles provide an independent estimate of Altair's projected rotation speed.

• Astrophysical maserRelated: Observed line widths constrain gas motions and conditions in masing regions.

• Atomic emission spectroscopyRelated: Broadening can blur nearby lines and affect measured emission intensity.

• Johannes StarkCompared with: Broadening can obscure the distinct line shifts and splittings Stark investigated.

• Absorption bandRelated: Broadening turns narrow transitions into bands with measurable width.