Spectral Classification

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(From Memory Alpha's Article: Star)
H-R diagram.png

A star (or "sun") is a massive energy-producing sphere of plasma and gas located in space. The region around a star that is held by its gravity, including any planets, moons, comets, and asteroids, is called a star system.

Spectral classification is the classification of stars based upon the temperature of the photosphere. Each spectral class is further divided into 10 subclasses, ranging from 0 (hottest) to 9 (coolest). Stars are also placed into one of sevaral categories based upon luminosity:

  • 0 (hypergiants)
  • 1a (luminous supergiants)
  • 1ab (intermediate luminous supergiants
  • 1b (less luminous supergiants)
  • II (bright giants)
  • III (normal giants)
  • IV (subgiants)
  • V (main sequence and dwarf stars)
  • VI (subdwarfs)
  • VII (uncommon white dwarfs)

For example, Sol is classified as type G2V. This indicates that is a Spectral Class G star of considerable temperature, and that it is a part of the main sequence.

Data borrowed from Wikipedia Article: Stellar Classification


Spectral Class O Spectral Class B Spectral Class A Spectral Class F
Spectral Class G Spectral Class K Spectral Class M

Spectral Class O

Class O stars are very hot and extremely luminous, with most of their radiated output in the ultraviolet range. These are the rarest of all main-sequence stars. About 1 in 3,000,000 (0.00003%) of the main-sequence stars in the solar neighborhood are class O stars. Some of the most massive stars lie within this spectral class. Class O stars frequently have complicated surroundings which make measurement of their spectra difficult

COMPOSITION Ionized atoms, helium
MASS ≥ 16 sols
RADIUS ≥ sols
ABUNDANCE ~0.00003% of all stars
LIFETIME 10 million years
EXAMPLES Mintaka, Kalidar, Zeta Puppis

Spectral Class B

Class B stars are very luminous and blue. Their spectra have neutral helium, which are most prominent at the B2 subclass, and moderate hydrogen lines. Ionized metal lines include Mg II and Si II. As O and B stars are so powerful, they only live for a relatively short time. Thus, due to the low probability of kinematic interaction during their lifetime, they do not, and are unable to, stray far from the area in which they were formed.

COLOR Blue White AST SC B.png
SURFACE TEMP 10,000 - 30,000 K
COMPOSITION Neutral helium, some hydrogen
MASS 2.1 - 16 sols
RADIUS 1.8 - 6.6 sols
LUMINOSITY 25,000 - 30,000
ABUNDANCE 0.13% of stars
LIFETIME 100 Million Years
EXAMPLES Rigel, Alpha Eridani

Spectral Class A

Class A stars are among the more common naked eye stars, and are white or bluish-white. They have strong hydrogen lines, at a maximum by A0, and also lines of ionized metals (Fe II, Mg II, Si II) at a maximum at A5. The presence of Ca II lines is notably strengthening by this point. About 1 in 160 (0.625%) of the main-sequence stars in the solar neighborhood are class A stars.

COLOR White AST SC A.png
SURFACE TEMP 7,500 - 10,000 K
COMPOSITION Strong hydrogen and ionized metals
MASS 1.4 - 2.1 sols
RADIUS 1.4 - 1.8 sols
ABUNDANCE 0.6% of stars
LIFETIME 1 billion years
EXAMPLES Vega, Sirius

Spectral Class F

Class F stars have strengthening H and K lines of Ca II. Neutral metals (Fe I, Cr I) beginning to gain on ionized metal lines by late F. Their spectra are characterized by the weaker hydrogen lines and ionized metals. Their color is white. About 1 in 33 (3.03%) of the main-sequence stars in the solar neighborhood are class F stars.

COLOR Yellow White AST SC F.png
SURFACE TEMP 6,000 - 7,500 K
COMPOSITION Hydrogen and ionized metals, calcium and iron
MASS 1.04 - 1.4 sols
RADIUS 1.15 - 1.4 sols
ABUNDANCE 3% of stars
LIFETIME 3 billion years
EXAMPLES Canopus, Procyon

Spectral Class G

Class G stars are probably the best known, if only for the reason that the Sun is of this class. They make up about 7.5%, nearly one in thirteen, of the main-sequence stars in the solar neighborhood.

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 ionized metals, they have neutral metals. There is a prominent spike in the G band of CH molecules. G is host to the "Yellow Evolutionary Void". Supergiant stars often swing between O or B (blue) and K or M (red). While they do this, they do not stay for long in the yellow supergiant G classification as this is an extremely unstable place for a supergiant to be.

COLOR Yellow AST SC G.png
SURFACE TEMP 5,200 - 6,000 K
COMPOSITION Ionized calcium, neutral and ionized metals
MASS 0.8 - 1.04 sols
RADIUS 0.96 - 1.15 sols
LUMINOSITY 0.6 - 1.5
ABUNDANCE 7.6% of stars
LIFETIME 10 billion years
EXAMPLES Sol, Ka'Tula, Capella

Spectral Class K

Class K stars are orangish stars that are slightly cooler than the Sun. They make up about 12%, nearly one in eight, of the main-sequence stars in the solar neighborhood. There are also giant K-type stars, which range from hypergiants like RW Cephei, to giants and supergiants, such as Arcturus, whereas orange dwarfs, 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). By late K, molecular bands of titanium oxide become present. There is a suggestion that K Spectrum stars may potentially increase the chances of life developing on orbiting planets that are within the habitable zone.

COLOR Orange AST SC K.png
SURFACE TEMP 3,700 - 5,200 K
COMPOSITION Neutral Metals
MASS 0.45 – 0.8 sols
RADIUS 0.7 – 0.96 sols
LUMINOSITY 0.08 – 0.6
ABUNDANCE 12.1% of stars
LIFETIME 50 billion years
EXAMPLES Arcturus, Aldebaran, Alpha Centauri

Spectral Class M

Class M stars are by far the most common. About 76% of the main-sequence stars in the Solar neighborhood are class M stars. However, because main-sequence stars of spectral class M have such low luminosities, none are bright enough to be visible to see with the unaided eye. The brightest known M-class main-sequence star is M0V Lacaille 8760 at magnitude 6.6 (the fractionally brighter Groombridge 1618 was once considered to be class M0 but is now considered to be as K5) and it is extremely unlikely that any brighter examples will be found.

Although most class M stars are red dwarfs, the class also hosts most giants and some supergiants such as VY Canis Majoris, Antares and Betelgeuse. Furthermore, the late-M group holds hotter brown dwarfs that are above the L spectrum. This is usually in the range of M6.5 to M9.5. The spectrum of a class M star shows lines belonging to oxide molecules, TiO in particular, in the visible and all neutral metals, but absorption lines of hydrogen are usually absent. TiO bands can be strong in class M stars, usually dominating their visible spectrum by about M5. Vanadium monoxide bands become present by late M.

SURFACE TEMP 2,400 - 3,700 K
COMPOSITION Ionized Atoms, helium
MASS 0.08 – 0.45 sols
RADIUS ≤ 0.3 sols
ABUNDANCE 76.45% of stars
LIFETIME 200 billion years
EXAMPLES Betelgeuse, Proxima Centauri, Wolf 359