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Mira variable

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Mira, the prototype of the Mira variables

Mira variables /ˈmrə/ (named for the prototype star Mira) are a class of pulsating stars characterized by very red colours, pulsation periods longer than 100 days, and amplitudes greater than one magnitude in infrared and 2.5 magnitude at visual wavelengths.[1] They are red giants 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 dwarfs within a few million years.

Mira variables are stars massive enough that they have undergone helium fusion in their cores but are less than two solar masses,[2] stars that have already lost about half their initial mass.[citation needed] However, they can be thousands of times more 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 relationship between period and luminosity (and colour).[3][4] 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.[5]

Light curve of 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 IOTA telescope are not spherically symmetric,[6] a result which is consistent with previous images of individual Mira stars,[7][8][9] so there is now pressure to do realistic three-dimensional modelling of Mira stars on supercomputers.[10]

Mira variables may be oxygen-rich or carbon-rich. Carbon-rich stars such as R Leporis arise from a narrow set of conditions that override the normal tendency for AGB stars to maintain a surplus of oxygen over carbon at their surfaces due to dredge-ups.[11] Pulsating AGB stars such as Mira variables undergo fusion in alternating hydrogen and helium shells, which produces periodic deep convection known as dredge-ups. 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 4 M, hot bottom burning occurs. This is when the lower regions of the convective region are hot enough for significant 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.[12]

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 masers.[13]

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 thermal pulses, 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.[14] 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.[15][16]

Mira variables are popular targets for 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.[17]

Visualisation of Mira type variable
Visualisation of Mira type variable

List

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The following list contains selected Mira variables. Unless otherwise noted, the given magnitudes are in the V-band, and distances are from the Gaia DR2 star catalogue.[18]

Star
Brightest
magnitude
Dimmest
magnitude
Period
(in days)
Distance
(in parsecs)
Reference
Mira 2.0 10.1 332 92 12
−9
[19]
[1]
Chi Cygni 3.3 14.2 408 180 45
−30
[2]
R Hydrae 3.5 10.9 380 224 56
−37
[3]
R Carinae 3.9 10.5 307 387 81
−57
[4]
R Leonis 4.4 11.3 310 71 5
−4
[5]
S Carinae 4.5 9.9 149 497 22
−20
[6]
R Cassiopeiae 4.7 13.5 430 187 9
−8
[7]
R Horologii 4.7 14.3 408 313 40
−32
[8]
U Orionis 4.8 13.0 377 216 19
−16
[9]
RR Scorpii 5.0 12.4 281 277 18
−16
[10]
R Serpentis 5.2 14.4 356 285 26
−22
[11]
T Cephei 5.2 11.3 388 176 13
−12
[12]
R Aquarii 5.2 12.4 387 320 31
−26
[13]
R Centauri 5.3 11.8 502 385 159
−87
[19]
[14]
RR Sagittarii 5.4 14 336 386 48
−38
[15]
R Trianguli 5.4 12.6 267 933 353
−201
[16]
S Sculptoris 5.5 13.6 367 1078 1137
−366
[17]
R Aquilae 5.5 12.0 271 238 27
−22
[18]
R Leporis 5.5 11.7 445 419 15
−14
[19]
W Hydrae 5.6 9.6 390 164 25
−19
[20]
R Andromedae 5.8 15.2 409 242 30
−24
[21]
S Coronae Borealis 5.8 14.1 360 431 60
−47
[22]
U Cygni 5.9 12.1 463 767 34
−31
[23]
X Ophiuchi 5.9 8.6 338 215 15
−13
[24]
RS Scorpii 6.0 13.0 319 709 306
−164
[25]
RT Sagittarii 6.0 14.1 306 575 48
−41
[26]
RU Sagittarii 6.0 13.8 240 1592 1009
−445
[27]
RT Cygni 6.0 13.1 190 888 47
−43
[28]
R Geminorum 6.0 14.0 370 1514 1055
−441
[29]
S Gruis 6.0 15.0 402 671 109
−82
[30]
V Monocerotis 6.0 13.9 341 426 50
−41
[31]
R Cancri 6.1 11.9 357 226 32
−25
[32]
R Virginis 6.1 12.1 146 530 28
−25
[33]
R Cygni 6.1 14.4 426 674 47
−41
[34]
R Boötis 6.2 13.1 223 702 60
−52
[35]
T Normae 6.2 13.6 244 1116 168
−129
[36]
R Leonis Minoris 6.3 13.2 372 347 653
−137
[19]
[37]
S Virginis 6.3 13.2 375 729 273
−156
[38]
R Reticuli 6.4 14.2 281 1553 350
−241
[39]
S Herculis 6.4 13.8 304 477 27
−24
[40]
U Herculis 6.4 13.4 404 572 53
−45
[41]
R Octantis 6.4 13.2 407 504 46
−39
[42]
S Pictoris 6.5 14.0 422 574 74
−59
[43]
R Ursae Majoris 6.5 13.7 302 489 54
−44
[44]
R Canum Venaticorum 6.5 12.9 329 661 65
−54
[45]
R Normae 6.5 12.8 496 581 10000
−360
[19]
[46]
T Ursae Majoris 6.6 13.5 257 1337 218
−164
[47]
R Aurigae 6.7 13.9 458 227 21
−17
[48]
RU Herculis 6.7 14.3 486 511 53
−44
[49]
R Draconis 6.7 13.2 246 662 58
−49
[50]
V Coronae Borealis 6.9 12.6 358 843 43
−39
[51]
T Cassiopeiae 6.9 13.0 445 374 37
−31
[52]
R Pegasi 6.9 13.8 378 353 35
−29
[53]
V Cassiopeiae 6.9 13.4 229 298 15
−14
[54]
T Pavonis 7.0 14.4 244 1606 340
−239
[55]
RS Virginis 7.0 14.6 354 616 81
−64
[56]
Z Cygni 7.1 14.7 264 654 36
−33
[57]
S Orionis 7.2 13.1 434 538 120
−83
[58]
T Draconis 7.2 13.5 422 783 48
−43
[59]
UV Aurigae 7.3 10.9 394 1107 83
−72
[60]
W Aquilae 7.3 14.3 490 321 22
−20
[61]
S Cephei 7.4 12.9 487 531 23
−21
[62]
R Fornacis 7.5 13.0 386 633 44
−38
[63]
RZ Pegasi 7.6 13.6 437 1117 88
−76
[64]
RT Aquilae 7.6 14.5 327 352 24
−21
[65]
V Cygni 7.7 13.9 421 458 36
−31
[66]
RR Aquilae 7.8 14.5 395 318 33
−28
[67]
S Boötis 7.8 13.8 271 2589 552
−387
[68]
WX Cygni 8.8 13.2 410 1126 86
−75
[69]
W Draconis 8.9 15.4 279 6057 4469
−1805
[70]
R Capricorni[20] 8.9 14.9 343 1407 178
−142
[71]
UX Cygni 9.0 17.0 569 5669 10000
−2760
[72]
LL Pegasi 9.6 K 11.6 K 696 1300[21] [73]
TY Cassiopeiae 10.1 19.0 645 1328 502
−286
[74]
IK Tauri 10.8 16.5 470 285 36
−29
[75]
CW Leonis 11.0 R 14.8 R 640 95 22
−15
[22]
[76]
TX Camelopardalis 11.6 B 17.7 B 557 333 42
−33
[77]
LP Andromedae 15.1 17.3 614 400 68
−51
[78]

See also

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References

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  1. ^ Mattei, Janet Akyuz (1997). "1997JAVSO..25...57M Page 57". Journal of the American Association of Variable Star Observers (Jaavso). 25 (2): 57. Bibcode:1997JAVSO..25...57M. Retrieved 2023-02-23.
  2. ^ Ireland, M.J.; Scholz, M.; Tuthill, P.G.; Wood, P.R. (December 2004). "Pulsation of M-type Mira variables with moderately different mass: search for observable mass effects". Monthly Notices of the Royal Astronomical Society. 355 (2): 444–450. arXiv:astro-ph/0408540. Bibcode:2004MNRAS.355..444I. doi:10.1111/j.1365-2966.2004.08336.x. S2CID 12395165.
  3. ^ Glass, I.S.; Lloyd Evans, T. (1981). "A period-luminosity relation for Mira variables in the Large Magellanic Cloud". Nature. 291 (5813). Macmillan: 303–4. Bibcode:1981Natur.291..303G. doi:10.1038/291303a0. S2CID 4262929.
  4. ^ Bedding, Timothy R.; Zijlstra, Albert A. (1998). "Hipparcos Period-Luminosity Relations for Mira and Semiregular variables". The Astrophysical Journal. 506 (1): L47–L50. arXiv:astro-ph/9808173. Bibcode:1998ApJ...506L..47B. doi:10.1086/311632. S2CID 14529151.
  5. ^ Smith, Beverly J.; Leisawitz, David; Castelaz, Michael W.; Luttermoser, Donald (2002). "Infrared Light Curves of Mira Variable Stars from COBE DIRBE Data". The Astronomical Journal. 123 (2): 948. arXiv:astro-ph/0111151. Bibcode:2002AJ....123..948S. doi:10.1086/338647. S2CID 16934459.
  6. ^ Ragland, S.; Traub, W. A.; Berger, J.-P.; Danchi, W. C.; Monnier, J. D.; Willson, L. A.; Carleton, N. P.; Lacasse, M. G.; Millan-Gabet, R.; Pedretti, E.; Schloerb, F. P.; Cotton, W. D.; Townes, C. H.; Brewer, M.; Haguenauer, P.; Kern, P.; Labeye, P.; Malbet, F.; Malin, D.; Pearlman, M.; Perraut, K.; Souccar, K.; Wallace, G. (2006). "First Surface-resolved Results with the Infrared Optical Telescope Array Imaging Interferometer: Detection of Asymmetries in Asymptotic Giant Branch Stars". The Astrophysical Journal. 652 (1): 650–660. arXiv:astro-ph/0607156. Bibcode:2006ApJ...652..650R. doi:10.1086/507453. S2CID 30825403.
  7. ^ Haniff, C. A.; Ghez, A. M.; Gorham, P. W.; Kulkarni, S. R.; Matthews, K.; Neugebauer, G. (1992). "Optical aperture synthetic images of the photosphere and molecular atmosphere of Mira" (PDF). Astronomical Journal. 103: 1662. Bibcode:1992AJ....103.1662H. doi:10.1086/116182.
  8. ^ Karovska, M.; Nisenson, P.; Papaliolios, C.; Boyle, R. P. (1991). "Asymmetries in the atmosphere of Mira". Astrophysical Journal. 374: L51. Bibcode:1991ApJ...374L..51K. doi:10.1086/186069.
  9. ^ Tuthill, P. G.; Haniff, C. A.; Baldwin, J. E. (1999). "Surface imaging of long-period variable stars". Monthly Notices of the Royal Astronomical Society. 306 (2): 353. Bibcode:1999MNRAS.306..353T. doi:10.1046/j.1365-8711.1999.02512.x.
  10. ^ Freytag, B.; Höfner, S. (2008). "Three-dimensional simulations of the atmosphere of an AGB star". Astronomy and Astrophysics. 483 (2): 571. Bibcode:2008A&A...483..571F. doi:10.1051/0004-6361:20078096.
  11. ^ Feast, Michael W.; Whitelock, Patricia A.; Menzies, John W. (2006). "Carbon-rich Mira variables: Kinematics and absolute magnitudes". Monthly Notices of the Royal Astronomical Society. 369 (2): 791–797. arXiv:astro-ph/0603506. Bibcode:2006MNRAS.369..791F. doi:10.1111/j.1365-2966.2006.10324.x. S2CID 12805849.
  12. ^ Stancliffe, Richard J.; Izzard, Robert G.; Tout, Christopher A. (2004). "Third dredge-up in low-mass stars: Solving the Large Magellanic Cloud carbon star mystery". Monthly Notices of the Royal Astronomical Society: Letters. 356 (1): L1–L5. arXiv:astro-ph/0410227. Bibcode:2005MNRAS.356L...1S. doi:10.1111/j.1745-3933.2005.08491.x. S2CID 17425157.
  13. ^ Wittkowski, M.; Boboltz, D. A.; Ohnaka, K.; Driebe, T.; Scholz, M. (2007). "The Mira variable S Orionis: Relationships between the photosphere, molecular layer, dust shell, and SiO maser shell at 4 epochs". Astronomy and Astrophysics. 470 (1): 191–210. arXiv:0705.4614. Bibcode:2007A&A...470..191W. doi:10.1051/0004-6361:20077168. S2CID 14200520.
  14. ^ Zijlstra, A. A.; Bedding, T. R.; Mattei, J. A. (2002). "The evolution of the Mira variable R Hydrae". Monthly Notices of the Royal Astronomical Society. 334 (3): 498. arXiv:astro-ph/0203328. Bibcode:2002MNRAS.334..498Z. doi:10.1046/j.1365-8711.2002.05467.x. S2CID 16663228.
  15. ^ Templeton, M. R.; Mattei, J. A.; Willson, L. A. (2005). "Secular Evolution in Mira Variable Pulsations". The Astronomical Journal. 130 (2): 776–788. arXiv:astro-ph/0504527. Bibcode:2005AJ....130..776T. doi:10.1086/431740. S2CID 359940.
  16. ^ Zijlstra, Albert A.; Bedding, Timothy R. (2002). "Period Evolution in Mira Variables". Journal of the American Association of Variable Star Observers. 31 (1): 2. Bibcode:2002JAVSO..31....2Z.
  17. ^ Mattei, Janet Akyuz (1997). "Introducing Mira Variables". The Journal of the American Association of Variable Star Observers. 25 (2): 57. Bibcode:1997JAVSO..25...57M.
  18. ^ Gaia Collaboration (2018), Gaia DR2, VizieR, retrieved 20 April 2019
  19. ^ a b c d van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  20. ^ Discovered in 1848 by Hind. Patrick Moore and Robin Rees (2011). Patrick Moore's Data Book of Astronomy (second ed.). Cambridge University Press. p. 323. ISBN 978-1139495226.
  21. ^ Lombaert, R.; De Vries, B. L.; De Koter, A.; Decin, L.; Min, M.; Smolders, K.; Mutschke, H.; Waters, L. B. F. M. (2012). "Observational evidence for composite grains in an AGB outflow. MgS in the extreme carbon star LL Pegasi". Astronomy & Astrophysics. 544: L18. arXiv:1207.1606. Bibcode:2012A&A...544L..18L. doi:10.1051/0004-6361/201219782. S2CID 119022145.
  22. ^ Sozzetti, A.; Smart, R. L.; Drimmel, R.; Giacobbe, P.; Lattanzi, M. G. (2017). "Evidence for orbital motion of CW Leonis from ground-based astrometry". Monthly Notices of the Royal Astronomical Society: Letters. 471 (1): L1–L5. arXiv:1706.04391. Bibcode:2017MNRAS.471L...1S. doi:10.1093/mnrasl/slx082.
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