Talk:List of largest stars/Pending Additions

Galactic list

List of the largest known stars: galactic pending additions^[a]
Star name	Solar radii (Sun = 1)	Method^[b]	Notes
Radii that were stated in the paper
U Arietis	801±205^[1]	AD
RT Ophiuchi	801±217^[1]	AD
UU Pegasi	742±193^[1]	AD
V Camelopardalis	716±185^[1]	AD
RR Aquilae	648±169^[1]	AD
RR Persei	599±161^[1]	AD
R Cassiopeiae	593±181^[1]	AD
S Serpentis	583±172–601±159^[1]	AD
RS Virginis	577±155^[1]	AD
RU Herculis	572±147^[1]	AD
R Leonis Minoris	569±146^[1]	AD
S Orionis	545±142^[1]	AD
R Draconis	511±142^[1]	AD
DG Cygni	499±140^[1]	AD
V Cassiopeiae	472±129^[1]	AD
Mira (ο Ceti)	468±120–482±124^[1]	AD
S Coronae Borealis	457±116^[1]	AD
S Pegasi	459±135–574±154^[1]	AD
R Pegasi	455±119–476±122^[1]	AD
U Herculis	431±114–453±117^[1]	AD
T Cassiopeiae	416±108^[1]	AD
Y Cassiopeiae	413±110^[1]	AD
R Aquarii	412±106–438±114^[1]	AD
R Leonis	409±105^[1]	AD
R Aurigae	407±105^[1]	AD
U Orionis	370±96^[1]	AD
BG Serpentis	354±99^[1]	AD
S Herculis	354±124^[1]	AD
R Serpentis	328±86^[1]	AD
U Persei	325±94–352±101^[1]	AD
Z Pegasi	310±92^[1]	AD
RT Aquilae	305±79^[1]	AD
X Ophiuchi	298±78–314±81^[1]	AD
S Ursae Minoris	296±82^[1]	AD
R Canum Venaticorum	279±75–322±82^[1]	AD
R Aquilae	259±67–328±85^[1]	AD
BG Cygni	236±76^[1]	AD
Radii that were calculated manually
Stephenson 2-18	2,150^[2]	L/T_eff
MY Cephei	2,061^[3]	L/T_eff
NML Cygni (V1489 Cygni)	1,639(–2,770)^[4]	L/T_eff
RSGC1-F01	1,530^[3]	L/T_eff
RSGC1-F04	1,422^[3]	L/T_eff
RSGC1-F06	1,382^[3]	L/T_eff
Stephenson 2-3	1,301^[3]	L/T_eff
Stephenson 2-11	1,300^[3]	L/T_eff
RSGC1-F10	1,246^[3]	L/T_eff
RSGC1-F05	1,185^[3]	L/T_eff
EV Carinae	1,165^[5]	L/T_eff
RSGC1-F08	1,150^[3]	L/T_eff
RSGC1-F02	1,128^[3]	L/T_eff
S Persei	1,109^[2]	L/T_eff
W Persei	1,011^[2]	L/T_eff
RSGC1-F11	1,032^[3]	L/T_eff
RSGC1-F13	1,017^[3]	L/T_eff
RSGC1-F07	1,006^[3]	L/T_eff
RSGC1-F09	996^[3]	L/T_eff
RSGC1-F12	955^[3]	L/T_eff
RSGC1-F03	942^[3]	L/T_eff
Stephenson 2-14	911^[3]	L/T_eff
SU Persei	863^[2]	L/T_eff
Stephenson 2-4	855^[3]	L/T_eff
AD Persei	812^[2]	L/T_eff
V441 Persei	799^[2]	L/T_eff
BU Persei	795^[2]	L/T_eff
V648 Cassiopeiae	778^[2]	L/T_eff
YZ Persei	758^[2]	L/T_eff
GP Cassiopeiae	751^[2]	L/T_eff
RSGC3-3	735^[3]	L/T_eff
Stephenson 2-5	730^[3]	L/T_eff
RSGC3-15	728^[3]	L/T_eff
KK Persei	724^[2]	L/T_eff
XX Persei	710^[2]	L/T_eff
Mercer 8-6	708^[2]	L/T_eff
RSGC3-16	682^[3]	L/T_eff
RSGC1-F14	662^[3]	L/T_eff
Stephenson 2 DFK 23	661^[3]	L/T_eff	The star has a peculiar SED and is potentially not a member.
RSGC3-13	655^[3]	L/T_eff
Stephenson 2-1	635^[3]	L/T_eff
Mercer 8-1	620^[2]	L/T_eff
PR Persei	603^[2]	L/T_eff
Stephenson 2 DFK 6	592^[3]	L/T_eff
Stephenson 2-8	576^[2]	L/T_eff
RSGC3-4	575^[3]	L/T_eff
Stephenson 2-2	569^[3]	L/T_eff
V778 Cassiopeiae	549^[2]	L/T_eff
Stephenson 2 DFK 18	531^[3]	L/T_eff
NGC 7419 BNSW e	528^[3]	L/T_eff
Mercer 8-5	522^[2]	L/T_eff
FZ Persei	501^[2]	L/T_eff
RSGC3-5	500^[3]	L/T_eff
Stephenson 2 DFK 13	499^[3]	L/T_eff
Mercer 8-2	498^[2]	L/T_eff
Stephenson 2-26	496^[2]	L/T_eff
RSGC3-1	494^[3]	L/T_eff
V605 Cassiopeiae	490^[2]	L/T_eff
V439 Persei	479^[2]	L/T_eff
RSGC3-14	474^[3]	L/T_eff
Mercer 8-4	458^[2]	L/T_eff
NGC 7419 BNSW c	455^[3]	L/T_eff
Stephenson 2 DFK 17	451^[3]	L/T_eff
HD 236947	431^[2]	L/T_eff
Stephenson 2 DFK 14	422^[3]	L/T_eff
RSGC1-F15	410^[3]	L/T_eff
RSGC3-2	393^[3]	L/T_eff
RSGC3-7	393^[3]	L/T_eff
NGC 7419 BNSW d	390^[3]	L/T_eff
V403 Persei	389^[2]	L/T_eff
RSGC3-9	386^[3]	L/T_eff
BD+59 372	380^[2]	L/T_eff
V550 Persei	371^[2]	L/T_eff
Stephenson 2 DFK 52	357^[3]	L/T_eff	The star has a peculiar SED.
PP Persei	352^[2]	L/T_eff
Mercer 8-3	351^[2]	L/T_eff
RSGC3-6	342^[3]	L/T_eff
RSGC3-11	342^[3]	L/T_eff
RSGC3-8	310^[3]	L/T_eff
Stephenson 2 DFK 15	288^[3]	L/T_eff
NGC 7419 BNSW a	273^[3]	L/T_eff
RSGC3-12	271^[3]	L/T_eff
RSGC3-10	231^[3]	L/T_eff

Extragalactic list

List of the largest known stars: extragalactic pending additions^[a]
Star name	Solar radii (Sun = 1)	Method^[c]
Radii that were stated in the paper
IRAS 05280-6910	1,738^[6]	L/T_eff
WOH G64	1,540±77^[7]	L/T_eff

Notes

^ ^a ^b So far these values are very far from final and they will definetly change some time in the future.
^
Methods for calculating the radius:
- AD: radius calculated from angular diameter and distance
- AtmModel: radius determined by comparing with atmosphere models
- L/T_eff: radius calculated from bolometric luminosity and effective temperature
- SAnl: radius determined from seismic analysis
- SED: radius determined from the spectral energy distribution
^
Methods for calculating the radius:
- L/T_eff: radius calculated from bolometric luminosity and effective temperature

References

^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ ^o ^p ^q ^r ^s ^t ^u ^v ^w ^x ^y ^z ^aa ^ab ^ac ^ad ^ae ^af ^ag ^ah ^ai ^aj ^ak van Belle, G. T.; Thompson, R. R.; Creech-Eakman, M. J. (September 2002). "Angular Size Measurements of Mira Variable Stars at 2.2 Microns. II". The Astronomical Journal. 124: 1706–1715. arXiv:astro-ph/0210167. Bibcode:2002AJ....124.1706V. doi:10.1086/342282. ISSN 0004-6256.
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ ^o ^p ^q ^r ^s ^t ^u ^v ^w ^x ^y ^z ^aa ^ab ^ac ^ad Fok, Thomas K. T.; Nakashima, Jun-ichi; Yung, Bosco H. K.; Hsia, Chih-Hao; Deguchi, Shuji (November 2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal. 760: 65. arXiv:1209.6427. Bibcode:2012ApJ...760...65F. doi:10.1088/0004-637X/760/1/65. ISSN 0004-637X.
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ ^o ^p ^q ^r ^s ^t ^u ^v ^w ^x ^y ^z ^aa ^ab ^ac ^ad ^ae ^af ^ag ^ah ^ai ^aj ^ak ^al ^am ^an ^ao ^ap ^aq ^ar ^as ^at ^au ^av ^aw ^ax ^ay Humphreys, Roberta M.; Helmel, Greta; Jones, Terry J.; Gordon, Michael S. (September 2020). "Exploring the Mass-loss Histories of the Red Supergiants". The Astronomical Journal. 160: 145. arXiv:2008.01108. Bibcode:2020AJ....160..145H. doi:10.3847/1538-3881/abab15. ISSN 0004-6256.{{cite journal}}: CS1 maint: unflagged free DOI (link)
^ Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W.; Brunthaler, A. (August 2012). "The distance and size of the red hypergiant NML Cygni from VLBA and VLA astrometry". Astronomy and Astrophysics. 544: A42. arXiv:1207.1850. Bibcode:2012A&A...544A..42Z. doi:10.1051/0004-6361/201219587. ISSN 0004-6361.
^ van Loon, J. Th.; Cioni, M. -R. L.; Zijlstra, A. A.; Loup, C. (July 2005). "An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars". Astronomy and Astrophysics. 438: 273–289. arXiv:astro-ph/0504379. Bibcode:2005A&A...438..273V. doi:10.1051/0004-6361:20042555. ISSN 0004-6361.
^ Matsuura, Mikako; Sargent, B.; Swinyard, Bruce; Yates, Jeremy; Royer, P.; Barlow, M. J.; Boyer, Martha; Decin, L.; Khouri, Theo; Meixner, Margaret; van Loon, Jacco Th. (November 2016). "The mass-loss rates of red supergiants at low metallicity: detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud". Monthly Notices of the Royal Astronomical Society. 462: 2995–3005. arXiv:1608.01729. Bibcode:2016MNRAS.462.2995M. doi:10.1093/mnras/stw1853. ISSN 0035-8711.
^ Levesque, Emily M.; Massey, Philip; Plez, Bertrand; Olsen, Knut A. G. (June 2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". The Astronomical Journal. 137: 4744–4752. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744. ISSN 0004-6256.

Add topic

[not-final-1] So far these values are very far from final and they will definetly change some time in the future.

[2] Methods for calculating the radius:
AD: radius calculated from angular diameter and distance

AtmModel: radius determined by comparing with atmosphere models

L/T_eff: radius calculated from bolometric luminosity and effective temperature

SAnl: radius determined from seismic analysis

SED: radius determined from the spectral energy distribution

[3] AD: radius calculated from angular diameter and distance

[4] AtmModel: radius determined by comparing with atmosphere models

[5] L/T_eff: radius calculated from bolometric luminosity and effective temperature

[6] SAnl: radius determined from seismic analysis

[7] SED: radius determined from the spectral energy distribution

[8] Methods for calculating the radius:
L/T_eff: radius calculated from bolometric luminosity and effective temperature

[9] L/T_eff: radius calculated from bolometric luminosity and effective temperature

[van-belle-3] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ ^o ^p ^q ^r ^s ^t ^u ^v ^w ^x ^y ^z ^aa ^ab ^ac ^ad ^ae ^af ^ag ^ah ^ai ^aj ^ak van Belle, G. T.; Thompson, R. R.; Creech-Eakman, M. J. (September 2002). "Angular Size Measurements of Mira Variable Stars at 2.2 Microns. II". The Astronomical Journal. 124: 1706–1715. arXiv:astro-ph/0210167. Bibcode:2002AJ....124.1706V. doi:10.1086/342282. ISSN 0004-6256.

[fok-4] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ ^o ^p ^q ^r ^s ^t ^u ^v ^w ^x ^y ^z ^aa ^ab ^ac ^ad Fok, Thomas K. T.; Nakashima, Jun-ichi; Yung, Bosco H. K.; Hsia, Chih-Hao; Deguchi, Shuji (November 2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal. 760: 65. arXiv:1209.6427. Bibcode:2012ApJ...760...65F. doi:10.1088/0004-637X/760/1/65. ISSN 0004-637X.

[humphreys-5] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ ^o ^p ^q ^r ^s ^t ^u ^v ^w ^x ^y ^z ^aa ^ab ^ac ^ad ^ae ^af ^ag ^ah ^ai ^aj ^ak ^al ^am ^an ^ao ^ap ^aq ^ar ^as ^at ^au ^av ^aw ^ax ^ay Humphreys, Roberta M.; Helmel, Greta; Jones, Terry J.; Gordon, Michael S. (September 2020). "Exploring the Mass-loss Histories of the Red Supergiants". The Astronomical Journal. 160: 145. arXiv:2008.01108. Bibcode:2020AJ....160..145H. doi:10.3847/1538-3881/abab15. ISSN 0004-6256.{{cite journal}}: CS1 maint: unflagged free DOI (link)

[zhang-6] Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W.; Brunthaler, A. (August 2012). "The distance and size of the red hypergiant NML Cygni from VLBA and VLA astrometry". Astronomy and Astrophysics. 544: A42. arXiv:1207.1850. Bibcode:2012A&A...544A..42Z. doi:10.1051/0004-6361/201219587. ISSN 0004-6361.

[van-loon-7] van Loon, J. Th.; Cioni, M. -R. L.; Zijlstra, A. A.; Loup, C. (July 2005). "An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars". Astronomy and Astrophysics. 438: 273–289. arXiv:astro-ph/0504379. Bibcode:2005A&A...438..273V. doi:10.1051/0004-6361:20042555. ISSN 0004-6361.

[matsuura-9] Matsuura, Mikako; Sargent, B.; Swinyard, Bruce; Yates, Jeremy; Royer, P.; Barlow, M. J.; Boyer, Martha; Decin, L.; Khouri, Theo; Meixner, Margaret; van Loon, Jacco Th. (November 2016). "The mass-loss rates of red supergiants at low metallicity: detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud". Monthly Notices of the Royal Astronomical Society. 462: 2995–3005. arXiv:1608.01729. Bibcode:2016MNRAS.462.2995M. doi:10.1093/mnras/stw1853. ISSN 0035-8711.

[levesque-10] Levesque, Emily M.; Massey, Philip; Plez, Bertrand; Olsen, Knut A. G. (June 2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". The Astronomical Journal. 137: 4744–4752. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744. ISSN 0004-6256.

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