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Additionally, if you want to make a new article on a star, just simply copy the markup below and add references just to save time: {{Star|name|other name(s)|constellation|distance in light years|size in solar diameters|planet whose orbit this star is roughly the size of|spectral class|temperature|dwarf? main sequence? giant? supergiant? hypergiant?|elements this star burns within its core|luminosity in suns|12=other information|13=references}}

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{| class="wikitable"
 
{| class="wikitable"
 
|-
 
|-
! Class
+
!Class
! Surface temperature<ref name="calib">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, [http://adsabs.harvard.edu/abs/1981A&AS...46..193H]. Luminosities are derived from M<sub>bol</sub> figures, using M<sub>bol</sub>(☉)=4.75.</ref><br>([[kelvin]])
+
!Surface temperature<ref name="calib" />([[kelvin]])
! abbr="color" | Conventional<br/>color description
+
! abbr="color" |Conventional color
! abbr="color" |Actual apparent color
+
! abbr="color" |Apparent color<ref name="möre">The Guinness book of astronomy facts & feats, Patrick Moore, 1992, 0-900424-76-1</ref><ref>{{cite web
!Mass(solar masses)
+
| date = 2004-12-21
!Radius(solar radii)
+
| url = http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html
!Luminosity<br/>(bolometric)
+
| title = The Colour of Stars
! Hydrogen<br>lines
+
| publisher = Australia Telescope Outreach and Education
! Fraction of all<br>[[main sequence|main-sequence]] stars<ref name="LeDrew2001"> LeDrew G. 2001. The real starry sky. ''Journal of the Royal Astronomical Society of Canada''. '''95''', 1, 32–33. [http://adsabs.harvard.edu/abs/2001JRASC..95...32L] Note: Table 2 has an error and so this article will use 824 as the assumed correct total of main-sequence stars.</ref>
+
| accessdate = 2007-09-26
|- style="background:#9db4ff;"
+
}}&nbsp;— Explains the reason for the difference in colour perception.</ref><ref>[http://www.vendian.org/mncharity/dir3/starcolor/ What color are the stars?], Mitchell Charity. Accessed online March 19, 2008.</ref>
!style="background:#9db4ff;"| [[#Class O|O]]
+
!Mass<ref name="calib">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 M<sub>bol</sub> figures, using M<sub>bol</sub>(☉)=4.75.</ref>([[solar masses]])
| ≥&nbsp;33,000&nbsp;K
+
!Radius<ref name="calib" />([[solar radius]])
| style="background:#9db4ff;" | blue
+
!Luminosity<ref name="calib" />(bolometric)
| blue
+
!Hydrogen
| ≥&nbsp;16 [[solar mass|M<sub>☉</sub>]]
+
lines
| ≥&nbsp;6.6 [[solar radius|R<sub>☉</sub>]]
+
!Fraction of all
| ≥&nbsp;30,000 [[solar luminosity|L<sub>☉</sub>]]
+
[[main sequence|main-sequence]] stars<ref name="LeDrew2001" />
| Weak
+
|- style="background:#9bb0ff;"
| ~0.00003%
+
! style="background:#9bb0ff;" |[[#Class O|O]]
 +
|≥&nbsp;33,000&nbsp;K
 +
| style="background:#9aafff;" |blue
 +
| style="background:#9bb0ff;" |blue
 +
|≥&nbsp;16 [[solar mass|M<sub>☉</sub>]]
 +
|≥&nbsp;6.6 [[solar radius|R<sub>☉</sub>]]
 +
|≥&nbsp;30,000 [[solar luminosity|L<sub>☉</sub>]]
 +
|Weak
 +
|~0.00003%
 
|- style="background:#aabfff;"
 
|- style="background:#aabfff;"
!style="background:#aabfff;"| [[#Class B|B]]
+
! style="background:#abbfff;" |[[#Class B|B]]
| 10,000–33,000&nbsp;K
+
|10,000–33,000&nbsp;K
| style="background:#aabfff;" | blue white
+
| style="background:#cad7ff;" |white to blue white
| deep blue white
+
| style="background:#aabfff;" |blue white
| 2.1–16 [[solar mass|M<sub>☉</sub>]]
+
|2.1–16 [[solar mass|M<sub>☉</sub>]]
| 1.8–6.6 [[solar radius|R<sub>☉</sub>]]
+
|1.8–6.6 [[solar radius|R<sub>☉</sub>]]
| 25–30,000 [[solar luminosity|L<sub>☉</sub>]]
+
|25–30,000 [[solar luminosity|L<sub>☉</sub>]]
| Medium
+
|Medium
| 0.13%
+
|0.13%
|- style="background:#cad8ff;"
+
|- style="background:#cad7ff;"
!style="background:#cad8ff;"| [[#Class A|A]]
+
! style="background:#cad7ff;" |[[#Class A|A]]
| 7,500–10,000&nbsp;K
+
|7,500–10,000&nbsp;K
| style="background:#cad8ff;" | white
+
| style="background:#f8f7ff;" |white
| blue white
+
| style="background:#cad7ff;" |white to blue white
| 1.4–2.1 [[solar mass|M<sub>☉</sub>]]
+
|1.4–2.1 [[solar mass|M<sub>☉</sub>]]
| 1.4–1.8 [[solar radius|R<sub>☉</sub>]]
+
|1.4–1.8 [[solar radius|R<sub>☉</sub>]]
| 5–25 [[solar luminosity|L<sub>☉</sub>]]
+
|5–25 [[solar luminosity|L<sub>☉</sub>]]
| Strong
+
|Strong
| 0.6%
+
|0.6%
 
|- style="background:#f8f7ff;"
 
|- style="background:#f8f7ff;"
!style="background:#f8f7ff;"| [[#Class F|F]]
+
! style="background:#f8f7ff;" |[[#Class F|F]]
| 6,000–7,500&nbsp;K
+
|6,000–7,500&nbsp;K
| style="background:#f8f7ff;" | yellow white
+
| style="background:#Fff4ea;" |yellowish white
| white
+
| style="background:#f8f7ff;" |white
| 1.04–1.4 [[solar mass|M<sub>☉</sub>]]
+
|1.04–1.4 [[solar mass|M<sub>☉</sub>]]
| 1.15–1.4 [[solar radius|R<sub>☉</sub>]]
+
|1.15–1.4 [[solar radius|R<sub>☉</sub>]]
| 1.5–5 [[solar luminosity|L<sub>☉</sub>]]
+
|1.5–5 [[solar luminosity|L<sub>☉</sub>]]
| Medium
+
|Medium
| 3%
+
|3%
 
|- style="background:#fff4ea;"
 
|- style="background:#fff4ea;"
!style="background:#fff4ea;"| [[#Class G|G]]
+
! style="background:#fff4ea;" |[[#Class G|G]]
| 5,200–6,000&nbsp;K
+
|5,200–6,000&nbsp;K
| style="background:#fff2a1;" | yellow
+
| style="background:#fff2a1;" |yellow
| yellowish white
+
| style="background:#Fff4ea;" |yellowish white
| 0.8–1.04 [[solar mass|M<sub>☉</sub>]]
+
|0.8–1.04 [[solar mass|M<sub>☉</sub>]]
| 0.96–1.15 [[solar radius|R<sub>☉</sub>]]
+
|0.96–1.15 [[solar radius|R<sub>☉</sub>]]
| 0.6–1.5 [[solar luminosity|L<sub>☉</sub>]]
+
|0.6–1.5 [[solar luminosity|L<sub>☉</sub>]]
| Weak
+
|Weak
| 7.6%
+
|7.6%
|- style="background:#FFEECC;"
+
|- style="background:#ffc133;"
!style="background:#FFEECC;"| [[#Class K|K]]
+
! style="background:#ffc149;" |[[#Class K|K]]
| 3,700–5,200&nbsp;K
+
|3,700–5,200&nbsp;K
| style="background:#FFEECC;" | orange
+
| style="background:#ff9833;" |orange
| pale yellow orange
+
| style="background:#ffc133;" |yellow orange
| 0.45–0.8 [[solar mass|M<sub>☉</sub>]]
+
|0.45–0.8 [[solar mass|M<sub>☉</sub>]]
| 0.7–0.96 [[solar radius|R<sub>☉</sub>]]
+
|0.7–0.96 [[solar radius|R<sub>☉</sub>]]
| 0.08–0.6 [[solar luminosity|L<sub>☉</sub>]]
+
|0.08–0.6 [[solar luminosity|L<sub>☉</sub>]]
| Very weak
+
|Very weak
| 12.1%
+
|12.1%
|- style="background:#ffd2a1;"
+
|- style="background:#ff7d33;"
!style="background:#ffd2a1;"| [[#Class M|M]]
+
! style="background:#ff7d33;" |[[#Class M|M]]
| 2,000–3,700&nbsp;K
+
|2,000–3,700&nbsp;K
| style="background:#ffd2a1;"| red
+
| style="background:#ff0000; color:#fff;" |red
| light orange red
+
| style="background:#ff7d33;" |orange red
| ≤&nbsp;0.45 [[solar mass|M<sub>☉</sub>]]
+
|≤&nbsp;0.45 [[solar mass|M<sub>☉</sub>]]
| ≤&nbsp;0.7 [[solar radius|R<sub>☉</sub>]]
+
|≤&nbsp;0.7 [[solar radius|R<sub>☉</sub>]]
| ≤&nbsp;0.08 [[solar luminosity|L<sub>☉</sub>]]
+
|≤&nbsp;0.08 [[solar luminosity|L<sub>☉</sub>]]
| Very weak
+
|Very weak
| 76.45%
+
|76.45%
|- style="background:#FFBBAA;"
+
|- style="background:#ff0000;"
!style="background:#FFBBAA;"|R
+
! style="background:#ff0000;" |[[Brown dwarf#Class L|L]]
| 1,300–2,000&nbsp;K
+
|1,300–2,000&nbsp;K
| style="background:#FFBBAA;"| red{{citation needed|date=November 2012}}
+
| style="background:#cc0099;" |purple-red
| style="background:#FFBBAA;"| red{{citation needed|date=November 2012}}
+
| style="background:#ff0000; color:#fff;" |red
| Unknown
 
| Unknown
 
| Unknown
 
| Very weak
 
 
|Unknown
 
|Unknown
|- style="background:#FFBBAA;"
 
!style="background:#FFBBAA;"|N
 
| 1,300–2,000&nbsp;K
 
| style="background:#FFBBAA;"| red{{citation needed|date=November 2012}}
 
| style="background:#FFBBAA;"| red{{citation needed|date=November 2012}}
 
| Unknown
 
| Unknown
 
| Unknown
 
| Very weak
 
 
|Unknown
 
|Unknown
|- style="background:#FFBBAA;"
+
|Unknown
!style="background:#FFBBAA;"|S
+
|Extremely weak
| 1,300–2,000&nbsp;K
+
|≥&nbsp;100.00%
| style="background:#FFBBAA;"| red{{citation needed|date=November 2012}}
+
|- style="background:#cc0099;"
| style="background:#FFBBAA;"| red{{citation needed|date=November 2012}}
+
! style="background:#cc0099;" |[[Brown dwarf#Class T|T]]
| Unknown
+
|700-1,300&nbsp;K
| Unknown
+
| style="background:#996633;" |brown
| Unknown
+
| style="background:#cc0099; color:#fff;" |purple-red
| Very weak
+
|Unknown
| Unknown
+
|Unknown
 +
|Unknown
 +
|Extremely weak
 +
|≥&nbsp;100.00%
 +
|- style="background:#996633;"
 +
! style="background:#996633;" |[[Brown dwarf#Class Y|Y]]
 +
|≤&nbsp;700&nbsp;K
 +
| style="background:#663300;" |dark brown
 +
| style="background:#996633; color:#fff;" |brown
 +
|Unknown
 +
|Unknown
 +
|Unknown
 +
|Extremely weak
 +
|≥&nbsp;100.00%
 
|}
 
|}
 
{| class="wikitable article-table"
 
{| class="wikitable article-table"

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