Star Type Classification

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Star Types[edit | edit source]

Class Image
Class Name
Details
Star0.jpg Class O An O-class (or O-type) star is a stellar classification for stars composed of ionized atoms, especially helium, emitting high amounts of ultraviolet radiation, generally referred to as being blue-violet or dark blue in color. O-type stars in the main sequence tend to be extremely hot (in the neighborhood of 28,000 to 50,000 Kelvin) and bright in terms of absolute magnitude, the "dark" and "violet" descriptors of their name are as such because of the large output of non-visible heat radiation.
Starb.jpg Class B A B-class (or B-type) star is a stellar classification for a hot blue star that is composed of neutral helium and some hydrogen. The temperature is between 10,000 and 28,000 Kelvins, generally referred to as being a blue star.
Stara.jpg Class A An A-class (or A-type) star is a stellar classification for stars composed of strong hydrogen and some ionized metals. The temperature ranges from 7,500 to 10,000 Kelvin, generally referred to as being blue-white or light blue in color.
Starf.jpg Class F A Class F star is white and is made up of hydrogen and ionized metals. Also in the star there is calcium and iron. The temperature in this type of star is between 6,000 and 7,500 K.
Starg.jpg Class G A G-class (or G-type) star is a stellar classification for stars composed of both neutral and ionized atoms of metallic substances, including ionized calcium, emitting in the neighborhood of 5,000 to 6,000 Kelvin, generally referred to as being yellow in color. G-type stars in the main sequence tend to be median in terms of absolute magnitude, and in the "cooler" half of the stellar classification system.
Stark.jpg Class K A K class (also K type or orange star) is a type of star that is made up of neutral metals. The temperature is around 3,500 through 5,000 degrees Kelvin.
Starm.jpg Class M An M-class (or M-type) star is a stellar classification for red star made up of ionized atoms, especially helium. The temperature is cool at 2,500 to 3,500 degrees K.


Other Stellar Objects[edit | edit source]

Class Image
Class Name
Details
Browndwarf.jpg Brown Dwarf A brown dwarf is a "star" whose mass is too small to have nuclear fusion based on hydrogen to occur at its core (the temperature and pressure at its core are insufficient for hydrogen fusion) though they can fuse deuterium and rarely even lithium. A brown dwarf is not very luminous. Brown Dwarfs typically appear as magenta tinted because of absorption by sodium and potassium atoms of light in the green portion of the spectrum.
Starwhited.jpg White Dwarf a small very dense star that is typically the size of a planet. A white dwarf is formed when a low-mass star has exhausted all its central nuclear fuel and lost its outer layers as a planetary nebula.
Neutronstar.jpg Neutron Star A neutron star is a type of stellar remnant that can result from the gravitational collapse of a massive star during a Type II, Type Ib or Type Ic supernova event. Such stars are composed almost entirely of neutrons, which are subatomic particles without net electrical charge and with slightly larger mass than protons. Neutron stars are very dense (the average Neutron star contains 500,000 times the mass of the Earth in a sphere with a diameter no larger than that of Brooklyn), very hot and emit vast amounts of deadly radiation.
Blackhole.jpg Black Hole A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping.


Spectral Type Characteristics[edit | edit source]

Main sequence stars (V)

Spectral Type Temperature (K) Absolute Magnitude Luminosity (in solar luminosities)
O5 54,000 -4.5 200,000
O6 45,000 -4.0 140,000
O7 43,300 -3.9 120,000
O8 40,600 -3.8 80,000
O9 37,800 -3.6 55,000
B0 29,200 -3.3 24,000
B1 23,000 -2.3 5550
B2 21,000 -1.9 3190
B3 17,600 -1.1 1060
B5 15,200 -0.4 380
B6 14,300 0 240
B7 13,500 0.3 140
B8 12,300 0.7 73
B9 11,400 1.1 42
A0 9600 1.5 24
A1 9330 1.7 20
A2 9040 1.8 17
A3 8750 2.0 14
A4 8480 2.1 12
A5 8310 2.2 11
A7 7920 2.4 8.8
F0 7350 3.0 5.1
F2 7050 3.3 3.8
F3 6850 3.5 3.2
F5 6700 3.7 2.7
F6 6550 4.0 2.0
F7 6400 4.3 1.5
F8 6300 4.4 1.4
G0 6050 4.7 1.2
G1 5930 4.9 1.1
G2 5800 5.0 1
G5 5660 5.2 0.73
G8 5440 2.6 0.51
K0 5240 6.0 0.38
K1 5110 6.2 0.32
K2 4960 6.4 0.29
K3 4800 6.7 0.24
K4 4600 7.1 0.18
K5 4400 7.4 0.15
K7 4000 8.1 0.11
M0 3750 8.7 0.080
M1 3700 9.4 0.055
M2 3600 10.1 0.035
M3 3500 10.7 0.027
M4 3400 11.2 0.022
M5 3200 12.3 0.011
M6 3100 13.4 0.0051
M7 2900 13.9 0.0032
M8 2700 14.4 0.0020
L0
2600
*
0.00029
L3
2200
*
0.00013
L8
1500
*
0.000032
T2
1400
*
0.000025
T6
1000
*
0.0000056
T8
800
*
0.0000036
  • - not visible to the human eye (for the most part)

    Giants (III)

Spectral Type Temperature (K) Absolute Magnitude Luminosity (in solar luminosities)
G5 5010 0.7 127
G8 4870 0.6 113
K0 4720 0.5 96
K1 4580 0.4 82
K2 4460 0.2 70
K3 4210 0.1 58
K4 4010 0.0 45
K5 3780 -0.2 32
M0 3660 -0.4 15
M1 3600 -0.5 13
M2 3500 -0.6 11
M3 3300 -0.7 9.5
M4 3100 -0.75 7.4
M5 2950 -0.8 5.1
M6 2800 -0.9 3.3

Supergiants (I)

Spectral Type Temperature (K) Absolute Magnitude Luminosity (in solar luminosities)
B0 21,000 -6.4 320,000
B1 16,000 -6.4 280,000
B2 14,000 -6.4 220,000
B3 12,800 -6.3 180,000
B5 11,500 -6.3 140,000
B6 11,000 -6.3 98,000
B7 10,500 -6.3 82,000
B8 10,000 -6.2 73,000
B9 9700 -6.2 61,000
A0 9400 -6.2 50,600
A1 9100 -6.2 44,000
A2 8900 -6.2 40,000
A5 8300 -6.1 36,000
F0 7500 -6 20,000
F2 7200 -6 18,000
F5 6800 -5.9 16,000
F8 6150 -5.9 12,000
G0 5800 -5.9 9600
G2 5500 -5.8 9500
G5 5100 -5.8 9800
G8 5050 -5.7 11,000
K0 4900 -5.7 12,000
K1 4700 -5.6 13,500
K2 4500 -5.6 15,200
K3 4300 -5.6 17,000
K4 4100 -5.5 18,300
K5 3750 -5.5 20,000
M0 3660 -5.3 50,600
M1 3600 -5.3 52,000
M2 3500 -5.3 53,000
M3 3300 -5.3 54,000
M4 3100 -5.2 56,000
M5 2950 -5.2 58,000