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{{short description|Type of variable star}}
[[File:A Wide-field view of the sky around a field studied in the MASSIV survey.jpg|300px|thumb|Mira, the prototype of the Mira variables]]
'''Mira variables''' {{IPAc-en|ˈ|m|aɪ|r|ə}} (named for the prototype star [[Mira]]) are a class of [[pulsating star]]s characterized by very red colours, pulsation periods longer than 100 days, and amplitudes greater than one [[Apparent magnitude|magnitude]] in [[infrared]] and 2.5 magnitude at visual wavelengths.<ref>{{Cite journal |title=Introducing Mira Variables | journal=Journal of the American Association of Variable Star Observers (Jaavso) | bibcode=1997JAVSO..25...57M | last=Mattei | first=Janet Akyuz | date=1997 | volume=25 | issue=2 | pages=57–62 }}</ref> They are [[red giant]]s in the very late stages of [[stellar evolution]], on the [[asymptotic giant branch]] (AGB), that will expel their outer envelopes as [[planetary nebulae]] and become [[white dwarf]]s within a few million years.

Mira variables are stars massive enough that they have undergone [[Triple-alpha process|helium fusion]] in their cores but are less than two [[solar masses]],<ref>{{cite journal |last1=Ireland |first1=M.J. |last2=Scholz |first2=M. |last3=Tuthill |first3=P.G. |last4=Wood |first4=P.R. |title=Pulsation of M-type Mira variables with moderately different mass: search for observable mass effects |journal=Monthly Notices of the Royal Astronomical Society |date=December 2004 |volume=355 |issue=2 |pages=444–450 |doi=10.1111/j.1365-2966.2004.08336.x |doi-access=free |arxiv=astro-ph/0408540 |bibcode=2004MNRAS.355..444I |s2cid=12395165 }}</ref> stars that have already lost about half their initial mass.{{citation needed|date=July 2016}} However, they can be thousands of times more [[luminosity|luminous]] than the [[Sun]] due to their very large distended envelopes. They are pulsating due to the entire star expanding and contracting. This produces a change in temperature along with radius, both of which factors cause the variation in [[luminosity]]. The pulsation depends on the mass and radius of the star and there is a well-defined [[period-luminosity relation|relationship]] between period and luminosity (and colour).<ref name=plrel>{{cite journal|last1=Glass|first1=I.S.|last2=Lloyd Evans|first2=T. | author2-link=Tom Lloyd-Evans |year=1981|title=A period-luminosity relation for Mira variables in the Large Magellanic Cloud|journal=Nature| publisher=Macmillan|volume=291|issue=5813|pages=303–4|bibcode = 1981Natur.291..303G |doi = 10.1038/291303a0 |s2cid=4262929}}</ref><ref name=pl>{{cite journal|doi=10.1086/311632|title=''Hipparcos'' Period-Luminosity Relations for Mira and Semiregular variables|journal=The Astrophysical Journal|volume=506|issue=1|pages=L47–L50|year=1998|last1=Bedding|first1=Timothy R.|last2=Zijlstra|first2=Albert A.|bibcode=1998ApJ...506L..47B|arxiv = astro-ph/9808173 |s2cid=14529151 }}</ref> The very large visual amplitudes are not due to large luminosity changes, but due to a shifting of energy output between infra-red and visual wavelengths as the stars change temperature during their pulsations.<ref>{{cite journal|doi=10.1086/338647|title=Infrared Light Curves of Mira Variable Stars from ''COBE'' DIRBE Data|journal=The Astronomical Journal|volume=123|issue=2|pages=948|year=2002|last1=Smith|first1=Beverly J.|last2=Leisawitz|first2=David|last3=Castelaz|first3=Michael W.|last4=Luttermoser|first4=Donald|bibcode=2002AJ....123..948S|arxiv = astro-ph/0111151 |s2cid=16934459}}</ref>

[[File:Chi Cygni light curve.png|thumb|left|Light curve of [[Chi Cygni|χ Cygni]].]]
Early models of Mira stars assumed that the star remained spherically symmetric during this process (largely to keep the computer modelling simple, rather than for physical reasons). A recent survey of Mira variable stars found that 75% of the Mira stars which could be resolved using the [[Infrared Optical Telescope Array|IOTA]] telescope are not spherically symmetric,<ref>{{cite journal|bibcode=2006ApJ...652..650R|title=First Surface-resolved Results with the Infrared Optical Telescope Array Imaging Interferometer: Detection of Asymmetries in Asymptotic Giant Branch Stars|journal=The Astrophysical Journal|volume=652|issue=1|pages=650–660|last1=Ragland|first1=S.|last2=Traub|first2=W. A.|last3=Berger|first3=J.-P.|last4=Danchi|first4=W. C.|last5=Monnier|first5=J. D.|last6=Willson|first6=L. A.|last7=Carleton|first7=N. P.|last8=Lacasse|first8=M. G.|last9=Millan-Gabet|first9=R.|last10=Pedretti|first10=E.|last11=Schloerb|first11=F. P.|last12=Cotton|first12=W. D.|last13=Townes|first13=C. H.|last14=Brewer|first14=M.|last15=Haguenauer|first15=P.|last16=Kern|first16=P.|last17=Labeye|first17=P.|last18=Malbet|first18=F.|last19=Malin|first19=D.|last20=Pearlman|first20=M.|last21=Perraut|first21=K.|last22=Souccar|first22=K.|last23=Wallace|first23=G.|year=2006|doi=10.1086/507453|arxiv = astro-ph/0607156 |s2cid=30825403 }}</ref> a result which is consistent with previous images of individual Mira stars,<ref>{{cite journal|bibcode=1992AJ....103.1662H|title=Optical aperture synthetic images of the photosphere and molecular atmosphere of Mira|journal=Astronomical Journal|volume=103|pages=1662|last1=Haniff|first1=C. A.|last2=Ghez|first2=A. M.|last3=Gorham|first3=P. W.|last4=Kulkarni|first4=S. R.|last5=Matthews|first5=K.|last6=Neugebauer|first6=G.|year=1992|doi=10.1086/116182|url=https://authors.library.caltech.edu/74624/1/1992AJ____103_1662H.pdf}}</ref><ref>{{cite journal|bibcode=1991ApJ...374L..51K|title=Asymmetries in the atmosphere of Mira|journal=Astrophysical Journal|volume=374|pages=L51|last1=Karovska|first1=M.|last2=Nisenson|first2=P.|last3=Papaliolios|first3=C.|last4=Boyle|first4=R. P.|year=1991|doi=10.1086/186069|doi-access=free}}</ref><ref>{{cite journal|bibcode=1999MNRAS.306..353T|title=Surface imaging of long-period variable stars|journal=Monthly Notices of the Royal Astronomical Society|volume=306|issue=2|pages=353|last1=Tuthill|first1=P. G.|last2=Haniff|first2=C. A.|last3=Baldwin|first3=J. E.|year=1999|doi=10.1046/j.1365-8711.1999.02512.x|doi-access=free}}</ref> so there is now pressure to do realistic three-dimensional modelling of Mira stars on supercomputers.<ref>{{cite journal|bibcode=2008A&A...483..571F|title=Three-dimensional simulations of the atmosphere of an AGB star|journal=Astronomy and Astrophysics|volume=483|issue=2|pages=571|last1=Freytag|first1=B.|last2=Höfner|first2=S.|year=2008|doi=10.1051/0004-6361:20078096|doi-access=free}}</ref>

Mira variables may be oxygen-rich or carbon-rich. Carbon-rich stars such as [[Hind's Crimson Star|R Leporis]] arise from a narrow set of conditions that override the normal tendency for [[Asymptotic giant branch|AGB]] stars to maintain a surplus of oxygen over carbon at their surfaces due to [[dredge-up]]s.<ref>{{cite journal|doi=10.1111/j.1365-2966.2006.10324.x|title=Carbon-rich Mira variables: Kinematics and absolute magnitudes|journal=Monthly Notices of the Royal Astronomical Society|volume=369|issue=2|pages=791–797|year=2006|last1=Feast|first1=Michael W.|last2=Whitelock|first2=Patricia A.|last3=Menzies|first3=John W.|doi-access=free |bibcode=2006MNRAS.369..791F|arxiv = astro-ph/0603506 |s2cid=12805849}}</ref> Pulsating AGB stars such as Mira variables undergo fusion in alternating hydrogen and helium shells, which produces periodic deep convection known as [[dredge-up]]s. These dredge-ups bring carbon from the helium burning shell to the surface and would result in a carbon star. However, in stars above about {{solar mass|4}}, hot bottom burning occurs. This is when the lower regions of the convective region are hot enough for significant [[CNO cycle#CNO-I|CNO cycle]] fusion to take place which destroys much of the carbon before it can be transported to the surface. Thus more massive AGB stars do not become carbon-rich.<ref>{{cite journal|doi=10.1111/j.1745-3933.2005.08491.x|title=Third dredge-up in low-mass stars: Solving the Large Magellanic Cloud carbon star mystery|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=356|issue=1|pages=L1–L5|year=2004|last1=Stancliffe|first1=Richard J.|last2=Izzard|first2=Robert G.|last3=Tout|first3=Christopher A.|doi-access=free |bibcode=2005MNRAS.356L...1S|arxiv = astro-ph/0410227 |s2cid=17425157 }}</ref>

Mira variables are rapidly losing mass and this material often forms [[dust]] shrouds around the star. In some cases conditions are suitable for the formation of natural [[Astrophysical maser|maser]]s.<ref>{{cite journal|doi=10.1051/0004-6361:20077168 |title=The Mira variable S Orionis: Relationships between the photosphere, molecular layer, dust shell, and SiO maser shell at 4 epochs |journal=Astronomy and Astrophysics |volume=470 |issue=1 |pages=191–210 |year=2007 |last1=Wittkowski |first1=M. |last2=Boboltz |first2=D. A. |last3=Ohnaka |first3=K. |last4=Driebe |first4=T. |last5=Scholz |first5=M. |bibcode=2007A&A...470..191W |arxiv = 0705.4614 |s2cid=14200520 }}</ref>

A small subset of Mira variables appear to change their period over time: the period increases or decreases by a substantial amount (up to a factor of three) over the course of several decades to a few centuries. This is believed to be caused by [[Asymptotic giant branch#AGB stage|thermal pulse]]s, where the [[helium]] shell reignites the outer [[hydrogen]] shell. This changes the structure of the star, which manifests itself as a change in period. This process is predicted to happen to all Mira variables, but the relatively short duration of thermal pulses (a few thousand years at most) over the [[asymptotic giant branch]] lifetime of the star (less than a million years), means we only see it in a few of the several thousand Mira stars known, possibly in [[R Hydrae]].<ref>{{cite journal|doi=10.1046/j.1365-8711.2002.05467.x|title=The evolution of the Mira variable R Hydrae|journal=Monthly Notices of the Royal Astronomical Society|volume=334|issue=3|pages=498|year=2002|last1=Zijlstra|first1=A. A.|last2=Bedding|first2=T. R.|last3=Mattei|first3=J. A.|doi-access=free |bibcode=2002MNRAS.334..498Z|arxiv = astro-ph/0203328 |s2cid=16663228 }}</ref> Most Mira variables do exhibit slight cycle-to-cycle changes in period, probably caused by nonlinear behaviour in the stellar envelope including deviations from spherical symmetry.<ref>{{cite journal|doi=10.1086/431740|title=Secular Evolution in Mira Variable Pulsations|journal=The Astronomical Journal|volume=130|issue=2|pages=776–788|year=2005|last1=Templeton|first1=M. R.|last2=Mattei|first2=J. A.|last3=Willson|first3=L. A.|bibcode=2005AJ....130..776T|arxiv = astro-ph/0504527 |s2cid=359940}}</ref><ref>{{cite journal|bibcode=2002JAVSO..31....2Z|title=Period Evolution in Mira Variables|journal=Journal of the American Association of Variable Star Observers|volume=31|issue=1|pages=2|last1=Zijlstra|first1=Albert A.|last2=Bedding|first2=Timothy R.|year=2002}}</ref>

Mira variables are popular targets for [[amateur astronomy|amateur astronomers]] interested in [[variable star]] observations, because of their dramatic changes in brightness. Some Mira variables (including [[Mira]] itself) have reliable observations stretching back well over a century.<ref>{{cite journal|bibcode=1997JAVSO..25...57M|title=Introducing Mira Variables|journal=The Journal of the American Association of Variable Star Observers|volume=25|issue=2|pages=57|last1=Mattei|first1=Janet Akyuz|year=1997}}</ref>
[[File:Mira variable visualisation based on χ Cygni pulsations.gif|alt=Visualisation of Mira type variable|center|thumb|500x500px|Visualisation of Mira type variable]]

==List==
The following list contains selected Mira variables. Unless otherwise noted, the given magnitudes are in the [[Apparent magnitude#Standard reference values|V-band]], and distances are from the [[Gaia_(spacecraft)#Data_releases|Gaia DR2 star catalogue]].<ref>{{Citation|url=http://webviz.u-strasbg.fr/viz-bin/VizieR-3?-source=I/345/gaia2|title=Gaia DR2|author=Gaia Collaboration|publisher=VizieR|year=2018|access-date=20 April 2019}}</ref>
{| border="1" class="wikitable sortable" style="text-align:center;"
|-
! Star 
! Brightest [[Apparent Magnitude|magnitude]] 
! Dimmest magnitude 
! Period (in days) 
! Distance (in [[parsec]]s)
! Reference
|-
| [[Mira]]
| 2.0
| 10.1
| 332
| {{val|92|12|9}}<ref name=aaa474_2_653>{{Cite journal| first1=F. | last1=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 |arxiv = 0708.1752| s2cid=18759600 }}</ref>
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=9237]
|-
| [[Chi Cygni]]
| 3.3
| 14.2
| 408
| {{val|180|45|30}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=13285]
|-
| [[R Hydrae]]
| 3.5
| 10.9
| 380
| {{val|224|56|37}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=15960]
|-
| [[R Carinae]]
| 3.9
| 10.5
| 307
| {{val|387|81|57}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=5754]
|-
| [[R Leonis]]
| 4.4
| 11.3
| 310
| {{val|71|5|4}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=17032]
|-
| [[S Carinae]]
| 4.5
| 9.9
| 149
| {{val|497|22|20}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=5755]
|-
| [[R Cassiopeiae]]
| 4.7
| 13.5
| 430
| {{val|187|9|8}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=6331]
|-
| [[R Horologii]]
| 4.7
| 14.3
| 408
| {{val|313|40|32}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=15900]
|-
| [[U Orionis]]
| 4.8
| 13.0
| 377
| {{val|216|19|16}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=23067]
|-
| [[RR Scorpii]]
| 5.0
| 12.4
| 281
| {{val|277|18|16}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=32826]
|-
| [[R Serpentis]]
| 5.2
| 14.4
| 356
| {{val|285|26|22}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=34592]
|-
| [[T Cephei]]
| 5.2
| 11.3
| 388
| {{val|176|13|12}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=8355]
|-
| [[R Aquarii]]
| 5.2
| 12.4
| 387
| {{val|320|31|26}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=846]
|-
| [[R Centauri]]
| 5.3
| 11.8
| 502
| {{val|385|159|87}}<ref name="aaa474_2_653" />
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=7298]
|-
| [[RR Sagittarii]]
| 5.4
| 14
| 336
| {{val|386|48|38}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=27710]
|-
| [[R Trianguli]]
| 5.4
| 12.6
| 267
| {{val|933|353|201}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=36594]
|-
| [[S Sculptoris]]
| 5.5
| 13.6
| 367
| {{val|1078|1137|366}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=34011]
|-
| [[R Aquilae]]
| 5.5
| 12.0
| 271
| {{val|238|27|22}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=1140]
|-
| [[R Leporis]]
| 5.5
| 11.7
| 445
| {{val|419|15|14}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=17280]
|-
| [[W Hydrae]]
| 5.6
| 9.6
| 390
| {{val|164|25|19}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=15965]
|-
| [[R Andromedae]]
| 5.8
| 15.2
| 409
| {{val|242|30|24}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=1]
|-
| [[S Coronae Borealis]]
| 5.8
| 14.1
| 360
| {{val|431|60|47}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=106019]
|-
| [[U Cygni]]
| 5.9
| 12.1
| 463
| {{val|767|34|31}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=10924]
|-
| [[X Ophiuchi]]
| 5.9
| 8.6
| 338
| {{val|215|15|13}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=20493]
|-
| [[RS Scorpii]]
| 6.0
| 13.0
| 319
| {{val|709|306|164}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=32827]
|-
| [[RT Sagittarii]]
| 6.0
| 14.1
| 306
| {{val|575|48|41}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=27712]
|-
| [[RU Sagittarii]]
| 6.0
| 13.8
| 240
| {{val|1592|1009|445}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=27713]
|-
| [[RT Cygni]]
| 6.0
| 13.1
| 190
| {{val|888|47|43}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=10932]
|-
| [[R Geminorum]]
| 6.0
| 14.0
| 370
| {{val|1514|1055|441}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=14295]
|-
| [[S Gruis]]
| 6.0
| 15.0
| 402
| {{val|671|109|82}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=14671]
|-
| [[V Monocerotis]]
| 6.0
| 13.9
| 341
| {{val|426|50|41}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=18833]
|-
| [[R Cancri]]
| 6.1
| 11.9
| 357
| {{val|226|32|25}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=4805]
|-
| [[R Virginis]]
| 6.1
| 12.1
| 146
| {{val|530|28|25}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=37809]
|-
| [[R Cygni]]
| 6.1
| 14.4
| 426
| {{val|674|47|41}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=10921]
|-
| [[R Boötis]]
| 6.2
| 13.1
| 223
| {{val|702|60|52}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=4304]
|-
| [[T Normae]]
| 6.2
| 13.6
| 244
| {{val|1116|168|129}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=19963]
|-
| [[R Leonis Minoris]]
| 6.3
| 13.2
| 372
| {{val|347|653|137}}<ref name="aaa474_2_653" />
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=17234]
|-
| [[S Virginis]]
| 6.3
| 13.2
| 375
| {{val|729|273|156}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=37810]
|-
| [[R Reticuli]]
| 6.4
| 14.2
| 281
| {{val|1553|350|241}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=27299]
|-
| [[S Herculis]]
| 6.4
| 13.8
| 304
| {{val|477|27|24}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=14813]
|-
| [[HD 148206|U Herculis]]
| 6.4
| 13.4
| 404
| {{val|572|53|45}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=14815]
|-
| [[R Octantis]]
| 6.4
| 13.2
| 407
| {{val|504|46|39}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=20343]
|-
| [[S Pictoris]]
| 6.5
| 14.0
| 422
| {{val|574|74|59}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=26335]
|-
| [[R Ursae Majoris]]
| 6.5
| 13.7
| 302
| {{val|489|54|44}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=37105]
|-
| [[R Canum Venaticorum]]
| 6.5
| 12.9
| 329
| {{val|661|65|54}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=5018]
|-
| [[R Normae]]
| 6.5
| 12.8
| 496
| {{val|581|10000|360}}<ref name="aaa474_2_653" />
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=19961]
|-
| [[T Ursae Majoris]]
| 6.6
| 13.5
| 257
| {{val|1337|218|164}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=37107]
|-
| [[R Aurigae]]
| 6.7
| 13.9
| 458
| {{val|227|21|17}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=3763]
|-
| [[RU Herculis]]
| 6.7
| 14.3
| 486
| {{val|511|53|44}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=14824]
|-
| [[R Draconis]]
| 6.7
| 13.2
| 246
| {{val|662|58|49}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=13673]
|-
| [[V Coronae Borealis]]
| 6.9
| 12.6
| 358
| {{val|843|43|39}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=10604]
|-
| [[T Cassiopeiae]]
| 6.9
| 13.0
| 445
| {{val|374|37|31}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=6333]
|-
| [[R Pegasi]]
| 6.9
| 13.8
| 378
| {{val|353|35|29}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=25123]
|-
| [[V Cassiopeiae]]
| 6.9
| 13.4
| 229
| {{val|298|15|14}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=6335]
|-
| [[T Pavonis]]
| 7.0
| 14.4
| 244
| {{val|1606|340|239}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=24723]
|-
| [[RS Virginis]]
| 7.0
| 14.6
| 354
| {{val|616|81|64}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=37819]
|-
| [[Z Cygni]]
| 7.1
| 14.7
| 264
| {{val|654|36|33}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=10929]
|-
| [[S Orionis]]
| 7.2
| 13.1
| 434
| {{val|538|120|83}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=23065]
|-
| [[T Draconis]]
| 7.2
| 13.5
| 422
| {{val|783|48|43}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=13675]
|-
| [[UV Aurigae]]
| 7.3
| 10.9
| 394
| {{val|1107|83|72}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=3797]
|-
| [[W Aquilae]]
| 7.3
| 14.3
| 490
| {{val|321|22|20}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=1145]
|-
| [[S Cephei]]
| 7.4
| 12.9
| 487
| {{val|531|23|21}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=8354]
|-
| [[R Fornacis]]
| 7.5
| 13.0
| 386
| {{val|633|44|38}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=14224]
|-
| [[RZ Pegasi]]
| 7.6
| 13.6
| 437
| {{val|1117|88|76}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=25140]
|-
| [[RT Aquilae]]
| 7.6
| 14.5
| 327
| {{val|352|24|21}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=1151]
|-
| [[V Cygni]]
| 7.7
| 13.9
| 421
| {{val|458|36|31}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=10925]
|-
| [[RR Aquilae]]
| 7.8
| 14.5
| 395
| {{val|318|33|28}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=1149]
|-
| [[S Boötis]]
| 7.8
| 13.8
| 271
| {{val|2589|552|387}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=4305]
|-
| [[WX Cygni]]
| 8.8
| 13.2
| 410
| {{val|1126|86|75}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=10966]
|-
| [[W Draconis]]
| 8.9
| 15.4
| 279
| {{val|6057|4469|1805}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=13678]
|-
| [[R Capricorni]]<ref>Discovered in 1848 by Hind. {{Cite book|page=[https://archive.org/details/patrickmooresdat00moor/page/n334 323]|title=Patrick Moore's Data Book of Astronomy|url=https://archive.org/details/patrickmooresdat00moor|url-access=limited|author=Patrick Moore and Robin Rees|edition=second|publisher=Cambridge University Press|date=2011|isbn=978-1139495226}}</ref>
| 8.9
| 14.9
| 343
| {{val|1407|178|142}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=5639]
|-
| [[UX Cygni]]
| 9.0
| 17.0
| 569
| {{val|5669|10000|2760}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=10957]
|-
| [[LL Pegasi]]
| 9.6 K
| 11.6 K
| 696
| {{val|1300}}<ref name="lombaert">{{cite journal|bibcode=2012A&A...544L..18L|title=Observational evidence for composite grains in an AGB outflow. MgS in the extreme carbon star LL Pegasi|journal=Astronomy & Astrophysics|volume=544|pages=L18|last1=Lombaert|first1=R.|last2=De Vries|first2=B. L.|last3=De Koter|first3=A.|last4=Decin|first4=L.|last5=Min|first5=M.|last6=Smolders|first6=K.|last7=Mutschke|first7=H.|last8=Waters|first8=L. B. F. M.|year=2012|doi=10.1051/0004-6361/201219782|arxiv = 1207.1606 |s2cid=119022145 }}</ref>
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=25383]
|-
| [[TY Cassiopeiae]]
| 10.1
| 19.0
| 645
| {{val|1328|502|286}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=6362]
|-
| [[IK Tauri]]
| 10.8
| 16.5
| 470
| {{val|285|36|29}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=35245]
|-
| [[CW Leonis]]
| 11.0 R
| 14.8 R
| 640
| {{val|95|22|15}}<ref name="sozetti">{{cite journal|arxiv=1706.04391|bibcode=2017MNRAS.471L...1S|title=Evidence for orbital motion of CW Leonis from ground-based astrometry|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=471|issue=1|pages=L1–L5|last1=Sozzetti|first1=A.|last2=Smart|first2=R. L.|last3=Drimmel|first3=R.|last4=Giacobbe|first4=P.|last5=Lattanzi|first5=M. G.|year=2017|doi=10.1093/mnrasl/slx082|doi-access=free }}</ref>
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=17154]
|-
| [[TX Camelopardalis]]
| 11.6 B
| 17.7 B
| 557
| {{val|333|42|33}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=4564]
|-
| [[LP Andromedae]]
| 15.1
| 17.3
| 614
| {{val|400|68|51}}
| [https://www.aavso.org/vsx/index.php?view=detail.top&oid=264]
|}

==See also==
* [[Long period variable]]
* [[Semiregular variable star]]

==References==
{{Reflist}}

==External links==
* [http://ogle.astrouw.edu.pl/atlas/Miras.html OGLE Atlas of Variable Star Light Curves - Mira Variables]

{{Variable star topics}}

{{Authority control}}

{{DEFAULTSORT:Mira Variable}}
[[Category:Mira variables| ]]

Mira variable - Revision history

imported>Praemonitus: Link author