The stellar classification is based on stars’ spectra. The stellar spectrum is characterised by three basic parameters:
temperature
gas pressure,
chemical composition.
In the Morgan‑Keenan (MK) system, there are seven main spectral types of stars ordered of decreasing temperature: O, B, A, F, G, K, and M. Each type has subclasses from 0 to 9 (hottest to coolest star of certain type e.g. B4, G7). The colour of a star is determined by its surface temperature.
star type
colour
approximate surface temperature (in K)
average mass (mass of the Sun = 1)
average radius (radius of the Sun = 1)
average luminosity (luminosity of the Sun = 1)
O
blue
≥ 30000
≥ 16
≥ 6,6
≥ 30000
B
blue
from 10000 to 30000
from 2,1 to 16
from 1,8 to 6,6
from 25 to 30000
A
blue
from 7500 to 10000
from 1,4 to 2,1
from 1,4 to 1,8
from 5 to 25
F
blue to white
from 6000 to 7500
from 1,04 to 1,4
from 1,15 to 1,4
from 1,5 to 5
G
white to yellow
from 5200 to 6000
from 0,8 to 1,04
from 0,96 to 1,15
from 0,6 to 1,5
K
orange to red
from 3700 to 5200
from 0,45 to 0,8
from 0,7 to 0,96
from 0,08 to 0,6
M
red
from 2400 to 3700
from 0,08 to 0,45
≤ 0,7
≤ 0,08
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An additional parameter used in the classification is luminosityluminosityluminosity of a star (The Yerkes Luminosity Classes).
Luminosity
Definition: Luminosity
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LuminosityluminosityLuminosity describes the brightness of a star (or galaxy). Luminosity is the total amount of energy that a star radiates each second (including all wavelengths of electromagnetic radiation).
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The luminosityluminosityluminosity of stars is affected not only by their temperature, but depends also on the size of a star. The most luminous stars are these which are hot and large. For a group of stars with the same temperature, the luminosity class differentiates between their sizes (supergiants, giants, main‑sequence stars, and subdwarfs).
Luminosity class
Description
0
hipergiants
Ia
bright supergiants
Ib
supergiants
II
bright giants
III
normal giants
IV
subgiants
V
main‑sequence stars (dwarfs)
VI
subdwarfs
VII
white dwarfs
The Hertzsprung‑Russell diagram
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The relationship between the average surface temperature of stars (spectral type) and their absolute luminosity is presented by the Hertzsprung‑Russell diagram (the H‑R diagram). The absolute luminosityluminosityluminosity of stars is telling how brigth they would appear if they were all the same distance, equal to 10 parsecs.
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Main sequence stars
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Main sequencemain sequenceMain sequence stars are the central band of stars on the H‑R Diagram. They are usually young stars. Their energy comes from nuclear fusion (conversion of hydrogen into helium). About 90% stars belong to the Main Sequence Stars.
The Sun is a G2V type star – a yellow dwarf.
Dwarf stars
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Dwarf stars are relatively small stars. Their size can be up to 20 times larger than the Sun’s size and luminosityluminosityluminosity up to 20000 times higher.
Yellow dwarfs are small stars of spectral type G, a weight between 0,7 and 1 times the solar mass, and a surface temperature of about 6000°C. They are bright yellow or almost white. Yellow dwarfs are about 10% of stars in the Milky Way.
Red dwarfs are small, cool, very faint, main sequencemain sequencemain sequence stars. Their surface temperature is under 4000 K. Red dwarfs are the most common type of star.
Giant and supergiant stars
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To the giantgiantgiant and supergiant stars belong mainly the old large stars.
Red giants
A red giant is an old star with a diameter about 100 times larger than it was at its beginning. Its surface temperature is under 6500 K.
Blue giant
A blue giant is a huge, very hot, blue star.
Supergiant
Supergiants are the largest known stars. Some of them are as big as our entire Solar System. They have extreme masses and hence relatively short lifetime of only 10 to 50 million years.
Dead stars
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White dwarfs
White dwarfs are small, very dense, hot stars. They are remnants of red giantgiantgiant stars. Their size is comparable with the Earth’s size, but these stars are much denser.
Neutron star
A neutron starneutron starneutron star: is a very small, very dense star. It is composed mostly of neutrons and has a thin atmosphere consisting of hydrogen. It has a diameter of about 5‑15 km.
Pulsar
A pulsarpulsarpulsar is a rapidly spinning neutron star. Its radiation can be observed only when the beam of emission is pointing toward the Earth.
Black holes
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A black holeblack holeblack hole is a part of space where a great amount of matter is packed into a very small area. The gravitational field of black holes is so strong that nothing, no particles and no electromagnetic radiation can escape from inside it.
Evolution of stars
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The radiation emitted by stars is a result of thermonuclear reactions taking place deep in their cores. In these reactions light elements are converted into heavier and enormous energy is released. There is enough pressure due to energy flow from the core to the outer parts of the star to keep it from collapsing under its weight. When nuclear reactions slow down due to the lack of elements a star starts to collapse. The dying star expands in the giantgiantgiant or supergiant phase. The star will eventually explode and become a planetary nebula or supernova. Finally it turns into a white dwarf stardwarf stardwarf star, neutron starneutron starneutron star or is getting a black holeblack holeblack hole. The final state of a star depends of its initial mass.
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Remember
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The star classification is based on stars spectra.
The relationship between the average surface temperature of stars and their absolute magnitude is presented by the Hertzsprung‑Russell diagram.
All stars undergo an evolution.
Exercises
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Exercise 1
Exercise 2
Order the following stars according to their decreasing luminosityluminosityluminosity: the Sun, white dwarf, a blue supergiant, a red giant.
A blue supergiant, a red giant, the Sun, white dwarf.