In astronomy, stellar classification is a way of grouping stars by temperature and luminosity. A star is a ball of superheated gas called plasma. Star temperature can be measured by looking at its spectrum, the type of light that the star shines. Stars are also grouped into spectral types or classes by color. In general, a star's temperature determines its color, from red to blue-white. Blue-white stars are the hottest, while Red ones are the coolest. Each class has their own subclass as well, with Hindu-Arabic Numerals. A G0 star would be the hottest type G and G9 with be the coolest type G.
Life Cycle of a Star
Stars are born in clouds of gas called a Nebula (plural: Nebulae) Nebulae are pulled together and become Protostars. Clouds of gas orbiting these stars then condense to form Planets, like how the Solar System was formed. The Star is then born and becomes a Main-Sequence Star. These stars live for up to 10 billion years and start to fuse hydrogen into the other elements of the Periodic Table. But as they reach heavier elements like Oxygen, they start cooling in temperature and become Red Giant stars, pushing their outer layers outward. Some stars expand even further into Red Supergiants by fusing metals. If the original post-giant star is more than 7 times larger than the Sun, then it will explode as a supernova for its death. Then it will become either a Neutron Star or a Black Hole, a bottomless pit that nothing can escape. If the original post-giant star is less than 7 times the size of the sun, it will become a white dwarf. White Dwarfs are small stars about the size of Earth, but they are hotter and were once the core of the progenitor star. Neutron Stars are the cores of original stars that have been crushed to the size of a city and they are packed up with Neutrons, the part of the atom that has no electrical charge. One 1 cm x 1 cm x 1 cm cube of their material would weigh as much as 5 fully-loaded cargo ships.
|Stellar evolution phase||
|Diameter (D☉, or other when specified)|
|Nebula||~0||1 to 2,000 ly|
|Main Sequence Star||3,000 to 50,000||0.08 to 20|
|Red Giant||3,000 to 5,000||20 to 200|
|Red Supergiants||200 to 2,600|
|White Dwarf||<4,000 to 150,000||8,000 to 100,000 km|
|Neutron Star||600,000||5 to 50 km|
Stars are also organized into another classification, this time for luminosity. This tells if the star is illegible to be called a dwarf, giant, supergiant, or hypergiant. It is also called the Yerkes spectral classification.
The stellar classification used to classify stars by color or temperature has seven main classes and four other ones. It is called the Morgan-Keenan stellar classification. It was originally proposed by Italian astronomer Angelo Secchi, but has been improved by Harvard professors William Morgan and Philip Keenan.
|Class||Surface temperature(kelvin)||Conventional color||Apparent color||Mass(solar masses)||Radius(solar radius)||Luminosity(bolometric)||Hydrogen
|Fraction of all|
|O||≥ 33,000 K||blue||blue||≥ 16 M☉||≥ 6.6 R☉||≥ 30,000 L☉||Weak||~0.00003%|
|B||10,000–33,000 K||white to blue white||blue white||2.1–16 M☉||1.8–6.6 R☉||25–30,000 L☉||Medium||0.13%|
|A||7,500–10,000 K||white||white to blue white||1.4–2.1 M☉||1.4–1.8 R☉||5–25 L☉||Strong||0.6%|
|F||6,000–7,500 K||yellowish white||white||1.04–1.4 M☉||1.15–1.4 R☉||1.5–5 L☉||Medium||3%|
|G||5,200–6,000 K||yellow||yellowish white||0.8–1.04 M☉||0.96–1.15 R☉||0.6–1.5 L☉||Weak||7.6%|
|K||3,700–5,200 K||orange||yellow orange||0.45–0.8 M☉||0.7–0.96 R☉||0.08–0.6 L☉||Very weak||12.1%|
|M||2,000–3,700 K||red||orange red||≤ 0.45 M☉||≤ 0.7 R☉||≤ 0.08 L☉||Very weak||76.45%|
|L||1,300–2,000 K||purple-red||red||Unknown||Unknown||Unknown||Extremely weak||≥ 100.00%|
|T||700-1,300 K||brown||purple-red||Unknown||Unknown||Unknown||Extremely weak||≥ 100.00%|
|Y||≤ 700 K||dark brown||brown||Unknown||Unknown||Unknown||Extremely weak||≥ 100.00%|
||Secchi's original classification||Temperature
|Percentage (%) of known stars||Possible color appearance|
|LBV (luminous blue variable)||n/a||7,500 to 50,000||0.000033|
||30,000 to 50,000|
|B||I (Orion subtype), V||10,000 to 30,000||0.13|
|A||I||7,500 to 10,000||0.7|
||6,000 to 7,500||3|
|G||II||5,000 to 6,000||7|
|K||4,000 to 5,000||12.1|
|M||III||2,400 to 4,000||77|
||n/a||200 to 3,000||> 100|
||IV||1,000 to 3,000||unknown|
|Wolf-Rayet Stars||n/a||30,000 to 200,000||unknown|
Star types are arranged in the Hertzsprung-Russell Diagram. This scattergraph was invented by Danish and American astronomers Ejnar Hertzsprung and Henry Russell in 1908. Stars farther away on the right are cooler in temperature, while stars that are near the top are more luminous and bright.
The line going from the top left-hand side down to the bottom right-hand side contains all of the main-sequence stars. The giant branch, containing yellow, orange, red giants, supergiants, hypergiants, and Mira variables, is located just above and right of the main sequence stars. Blue and white supergiants are directly above the central main sequence. Brown dwarfs are at the very bottom of the main sequence, with white dwarfs directly below the central main-sequence. The yellow evolutionary void is located between the blue-white supergiants and the giant branch.
B-V Color Index
In astronomy, the B-V color index is a numerical expression that determines the exact "color" of a certain star. The smaller the color index, the more the star appears blue. For comparison, our Sun has an approximate B-V color index of 0.656, while Rigel has a color index of -0.03. Red Giants have color indexes from 0.81 to 1.4 .
- ISBN 0-333-75088-8
- ISBN 1-61233-765-1
- ISBN 0-387-33543-9
- A neutron star's density increases as its mass increases, and its radius decreases non-linearly. (archived image: https://web.archive.org/web/20111017230141/http://ixo.gsfc.nasa.gov/old_conx_pages/science/neutron_star/index.html) A newer page is here: https://heasarc.gsfc.nasa.gov/docs/xte/Greatest_Hits/khz.qpo.html (specifically the image https://heasarc.gsfc.nasa.gov/docs/xte/Greatest_Hits/cole.miller.plot.2.ps.gif)
- Tables VII, VIII, Empirical bolometric corrections for the main-sequence, G. M. H. J. Habets and J. R. W. Heinze, Astronomy and Astrophysics Supplement Series 46 (November 1981), pp. 193–237, Bibcode: 1981A&AS...46..193H. Luminosities are derived from Mbol figures, using Mbol(☉)=4.75.
- The Guinness book of astronomy facts & feats, Patrick Moore, 1992, 0-900424-76-1
- Lua error in Module:Citation/CS1 at line 379: attempt to call method 'match' (a nil value). — Explains the reason for the difference in colour perception.
- What color are the stars?, Mitchell Charity. Accessed online March 19, 2008.
- Cite error: Invalid
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- ISBN 0-521-25548-1
- pp. 62–63, Hearnshaw 1986.
- p. 60, Hearnshaw 1986.
- ISBN 0-521-34787-4
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