Spectral Class |
Color |
Surface Temperature (K) |
Principal Features |
Examples |
O |
Bluish-white |
30,000-50,000+ |
Relatively few absorption lines. Lines of
ionized helium and other lines of highly ionized atoms. Hydrogen lines
appear only weakly. Peak of light in UV part of spectrum. |
Naos |
B |
Bluish-white |
10,000-30,000 |
Lines of neutral helium. Hydrogen lines more pronounced than
in O-type stars. He I lines strong, as well as C II, O II, Si III. |
Rigel, Spica |
A |
Bluish-white to white |
7,500-10,000 |
Strong lines of hydrogen. Also lines of singly ionized
magnesium, silicon, iron, titanium, calcium, and others. Lines of some
neutral metals show weakly. |
Sirius, Vega |
F |
white to yellowish-white |
6,000-7,500 |
Hydrogen lines are weaker than in A-type star but still
conspicuous. Lines of singly ionized metals are present (Ca II), as are
lines of other neutral metals. |
Canopus, Procyon |
G |
yellow to yellowish-white |
5,000-6,000 |
Lines of ionized calcium (Ca II) are the most conspicuous.
Many lines of ionized and neutral metals are present. Hydrogen lines
are weaker even than in F-type stars. |
Sun, Capella |
K |
yellowish-orange |
3,500-5,000 |
Lines of neutral metals predominate. Hydrogen very weak,
molecular bands start to appear. |
Arcturus, Aldebaran |
M |
reddish |
2,200-3,500 |
Strong lines of neutral metals and molecules. |
Betelgeuse, Antares |
L |
red |
1,400-2,200 |
Visible mainly in the infrared part of the spectrum. Strong
lines of neutral metals and molecules, including water, CO, TiO, FeH, O2. |
* |
T |
red |
Less than 1,400 |
Visible almost entirely at Infrared wavelengths, shows strong
methane features. |
* |