Spectral Classification of Stars

Spectral classification of stars is a grouping based on photospheric temperature and its associated spectral characteristics.

By Tim TrottSolar Physics • November 13, 2008
845 words, estimated reading time 3 minutes.
Solar Physics

This article is part of a series of articles. Please use the links below to navigate between the articles.

  1. Star Formation and Stellar Evolution
  2. Spectral Classification of Stars
  3. Hertzsprung-Russell Diagram and the Main Sequence Explained
  4. Investigating Light with Spectroscopy and Spectrometry
  5. Chandrasekhar Limit - White Dwarfs and Black Holes
  6. What is Electron Degeneracy Pressure and White Dwarfs Explained
Spectral Classification of Stars

Stellar temperatures can be classified using Wien's displacement law, which poses difficulties for distant stars. Stellar spectroscopy offers a way to classify stars according to their absorption lines; particular absorption lines can be observed only for a certain range of temperatures because only in that range are the involved atomic energy levels populated. An early scheme (from the 19th century) ranked stars from A to Q, the origin of the currently used spectral classes.

Secchi Spectral Classification

During the 1860s and 1870s, pioneering stellar spectroscopist Father Angelo Secchi created the Secchi Spectral Classification to classify observed spectra. The classifications group stars into classes as follows:

  • Class I: white and blue stars with broad, heavy hydrogen lines like Vega and Altair. This includes modern class A and early class F.
    • Class I, Orion subtype: a subtype of class I with narrow lines in place of wide bands, such as Rigel and γ Orionis. In modern terms, this corresponds to early B-type stars.
  • Class II: yellow stars - hydrogen less strong, but evident metallic lines, such as Arcturus and Capella. This includes the modern classes G and K as well as late class F.
  • Class III: orange to red stars with complex band spectra, such as Betelgeuse and Antares. This corresponds to the modern class M.
  • Class IV: red stars with significant carbon bands and lines (carbon stars.)
  • Class V: emission-line stars, such as γ Cassiopeiae and β Lyrae.

In the late 1890s, this classification began to be superseded by the Harvard classification.

Harvard Spectral Classification

The Harvard classification system is a one-dimensional classification scheme. Physically, the classes indicate the temperature of the star's atmosphere.

Star classes with the colours very close to those actually perceived by the human eye. The relative sizes are for main sequence or "dwarf" stars.
Spectral Classification star classes with colours very close to those perceived by the human eye. The relative sizes are for main sequence or 'dwarf' stars.

A popular mnemonic for remembering the order of spectral classification is "Oh Be A Fine Girl/Guy, Kiss Me", although there are many variants of this mnemonic.

The Hertzsprung-Russell diagram relates stellar classification with absolute magnitude, luminosity, and surface temperature and provides a useful tool for the analysis of stars.

The main sequence is visible as a prominent diagonal band that runs from the upper left to the lower right.
The main sequence is visible as a prominent diagonal band that runs from the upper left to the lower right.

Spectral Classification O

Spectral Classification O stars are very hot and very luminous, being bluish; most of their output is in the ultraviolet range. These are the rarest of all main sequence stars, constituting as few as 1 in 3,000,000 in the solar neighbourhood. These stars have dominant lines of absorption and sometimes emission for He II lines, prominent ionised (Si IV, O III, N III, and C-III) and neutral helium lines, strengthening from O5 to O9, and prominent hydrogen Balmer lines, although not as strong as in later types. Because they are so huge, class O stars quickly burn through their hydrogen fuel and are the first to leave the main sequence.

Examples: Zeta Orionis, Zeta Puppis, Lambda Orionis, Delta Orionis

Spectral Class B

Spectral Classification B stars are extremely luminous and blue. Their spectra have neutral helium, most prominent in the B2 subclass, and moderate hydrogen lines. Ionised metal lines include Mg II and Si II. As O and B stars are so powerful, they only live for a very short time; thus, they do not stray far from the area in which they were formed. They constitute about 1 in 800 main-sequence stars in the solar neighbourhood.

Examples: Rigel, Spica, the brighter Pleiades

Spectral Class A

Spectral Classification A stars are amongst the more common naked-eye stars and are white or bluish-white. They have strong hydrogen lines at a maximum of A0 and lines of ionised metals (Fe II, Mg II, Si II) at a maximum of A5. The presence of Ca II lines is notably strengthening by this point. They comprise about 1 in 160 of the main sequence stars in the solar neighbourhood.

Examples: Vega, Sirius, Deneb

Spectral Class F

Class F stars have strengthening H and K lines of Ca II. Neutral metals (Fe I, Cr I) begin to gain on ionised metal lines by late F. Their spectra are characterised by the weaker hydrogen lines and ionised metals. Their colour is white. These represent about 1 in 33 of the main sequence stars in the solar neighbourhood.

Examples: Arrakis, Canopus, Procyon

Spectral Class G

Class G stars are probably the best known because our Sun is of this class. Most notable are the H and K lines of Ca II, which are most prominent at G2. They have even weaker hydrogen lines than F, but along with the ionised metals, they have neutral metals. There is a prominent spike in the G band of CH molecules. G stars represent about 1 in 13 of the main sequence stars in the solar neighbourhood.

Examples: Sun, Alpha Centauri A, Capella, Tau Ceti

Spectral Class K

Class K is orange stars, which are slightly cooler than our Sun. Some K stars are giants and supergiants, such as Arcturus, while others, like Alpha Centauri B, are main-sequence stars. They have extremely weak hydrogen lines, if they are present at all, and mostly neutral metals (Mn I, Fe I, Si I).

Examples: Alpha Centauri B, Epsilon Eridani, Arcturus, Aldebaran

Spectral Class M

Class M is by far the most common class. About 76% of the main-sequence stars in the solar neighbourhood are red dwarfs. M is also hosting most giants, some supergiants such as Antares and Betelgeuse, and Mira variables. The late-M group holds hotter brown dwarfs that are above the L spectrum.

Examples: Betelgeuse, Proxima Centauri, Barnard's star, Gliese 581

About the Author

Tim Trott is an avid stargazer and astrophotographer whose passion for the cosmos fuels a lifelong journey of exploration and wonder. Through Perfect Astronomy, he shares the beauty of the night sky and the art of capturing it, blending science and creativity to inspire curious minds and aspiring astrophotographers alike. Join him as he turns every starry night into a story waiting to be told.

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