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UY Scuti

January 06, 2023

For the album, see UY Scuti (album).

UY Scuti (BD-12°5055) is an extreme red hypergiant[3] or red supergiant star in the constellation Scutum. It is considered one of the largest known stars by radius and is also a pulsating variable star, with a maximum brightness of magnitude 8.29 and a minimum of magnitude 10.56. It has an estimated radius of 1,708 solar radii (1.188×109 kilometres; 7.94 astronomical units), thus a volume nearly 5 billion times that of the Sun. It is approximately 2.9 kiloparsecs (9,500 light-years) from Earth. If placed at the center of the Solar System, its photosphere would at least engulf the orbit of Jupiter.

UY Scuti

DSS2 image of red supergiant star UY Scuti (brightest star in the image), surrounded by a dense starfield.
Observation data
Epoch J2000      Equinox J2000
Constellation Scutum
Right ascension 18h 27m 36.5334s[1]
Declination −12° 27′ 58.866″[1]
Apparent magnitude (V) 8.29 - 10.56[2]
Characteristics
Evolutionary stage Red hypergiant[3]
Spectral type M2-M4Ia-Iab[2]
U−B color index +3.29[4]
B−V color index +3.00[5]
Variable type SRc[6]
Astrometry
Radial velocity (Rv)18.33±0.82[7] km/s
Proper motion (μ) RA: 1.3[8] mas/yr
Dec.: −1.6[8] mas/yr
Parallax (π)0.5166 ± 0.0494 mas[9]
Distance9,500±1,030[10] ly
(2,900±317[10] pc)
Absolute magnitude (MV)−6.2[10]
Details
Mass7–10[4] M☉
Radius1,708±192[4] R☉
Luminosity340,000+290,000
−160,000[4] L☉
Surface gravity (log g)−0.5[4] cgs
Temperature3,365±134[4] K
Other designations
UY Sct, BD−12°5055, IRC −10422, RAFGL 2162, HV 3805
Database references
SIMBADdata

Nomenclature and history

 
A visual band light curve for UY Scuti, plotted from ASAS data[11]

UY Scuti was first catalogued in 1860 by German astronomers at the Bonn Observatory, who were completing a survey of stars for the Bonner Durchmusterung Stellar Catalogue.[12] It was designated BD-12°5055, the 5,055th star between 12°S and 13°S counting from 0h right ascension.

On detection in the second survey, the star was found to have changed slightly in brightness, suggesting that it was a new variable star. In accordance with the international standard for designation of variable stars, it was called UY Scuti, denoting it as the 38th variable star of the constellation Scutum.[13]

UY Scuti is located a few degrees north of the A-type star Gamma Scuti and northeast of the Eagle Nebula. Although the star is very luminous, it is, at its brightest, only 9th magnitude as viewed from Earth, due to its distance and location in the Zone of Avoidance within the Cygnus rift.[14]

Characteristics

 
An illustration of the approximate size of UY Scuti compared to the Sun
 
Relative sizes of the planets in the Solar System and several stars, including UY Scuti:
1. Mercury < Mars < Venus < Earth
2. Earth < Neptune < Uranus < Saturn < Jupiter
3. Jupiter < Proxima Centauri < Sun < Sirius
4. Sirius < Pollux < Arcturus < Aldebaran
5. Aldebaran < Rigel < Antares < Betelgeuse
6. Betelgeuse < NML Cygni < VV Cephei A < VY Canis Majoris (Wittkowski et al. 2012 estimate) < UY Scuti.

UY Scuti is a dust-enshrouded bright red supergiant[15] and is classified as a semiregular variable with an approximate pulsation period of 740 days.[6][16][17] Based on a radius of 1,708 R☉, this pulsation would be an overtone of the fundamental pulsation period, or it may be a fundamental mode corresponding to a smaller radius.[18]

In the summer of 2012, AMBER interferometry with the Very Large Telescope (VLT) in the Atacama Desert in Chile was used to measure the parameters of three red supergiants near the Galactic Center region:[4] UY Scuti, AH Scorpii, and KW Sagittarii. They determined that all three stars are over 1,000 times bigger than the Sun and over 100,000 times more luminous than the Sun. The stars' sizes were calculated using the Rosseland radius, the location at which the optical depth is 2⁄3,[19] with distances adopted from earlier publications. UY Scuti was found to be the largest and the most luminous of the three stars measured, at 1,708 ± 192 R☉ (1.188×109 ± 134,000,000 km; 7.94 ± 0.89 AU) based on an angular diameter of 5.48±0.10 mas and an assumed distance of 2.9±0.317 kiloparsecs (kpc) (about 9,500±1,030 light-years) which was originally derived in 1970 based on the modelling of the spectrum of UY Scuti.[10] The luminosity is then calculated to be 340,000 L☉ at an effective temperature of 3,365 ± 134 K, giving an initial mass of 25 M☉ (possibly up to 40 M☉ for a non-rotating star).[4]

A hypothetical object travelling at the speed of light would be observed to take about seven hours to travel along UY Scuti's great circle whereas it would take 14.5 seconds to circle the Sun.[20]

Direct measurements of the parallax of UY Scuti published in the Gaia Data Release 2 give a parallax of 0.6433±0.1059 mas,[7] implying a closer distance of approximately 1.5 kiloparsecs (4,900 ly),[21] and consequently much lower luminosity and radius values of around 86,300–87,100 L☉ and 755 R☉ respectively.[22] However, the Gaia parallax might be unreliable, at least until further observations, due to a very high level of astrometric noise.[7] Gaia Early Data Release 3 has published a parallax of 0.5166±0.0494 mas for this star, again with a large value for astrometric noise, rated at a significance of 122 where anything over 2 is "probably significant".[9]

UY Scuti has no known companion star and so its mass is uncertain. However, it is expected on theoretical grounds to be between 7 and 10 M☉.[4] Mass is being lost at 5.8×10−5 M☉ per year, leading to an extensive and complex circumstellar environment of gas and dust.[23]

Supernova

Based on current models of stellar evolution, UY Scuti has begun to fuse helium, and continues to fuse hydrogen in a shell around the core. The location of UY Scuti deep within the Milky Way disc suggests that it is a metal-rich star.[24]

After fusing heavy elements, its core will begin to produce iron, disrupting the balance of gravity and radiation in its core and resulting in a core collapse supernova. It is expected that stars like UY Scuti should evolve back to hotter temperatures to become a yellow hypergiant, luminous blue variable, or a Wolf–Rayet star, creating a strong stellar wind that will eject its outer layers and expose the core, before exploding as a type IIb, IIn, or type Ib/Ic supernova.[25]

See also

References

  1. ^ a b Hog, E.; Kuzmin, A.; Bastian, U.; Fabricius, C.; Kuimov, K.; Lindegren, L.; Makarov, V. V.; Roeser, S. (1998). "The TYCHO Reference Catalogue". Astronomy and Astrophysics. 335: L65. Bibcode:1998A&A...335L..65H.
  2. ^ a b "VSX: Detail for UY Sct". American Association of Variable Star Observers. Retrieved 2018-09-20.
  3. ^ a b Tabernero, H. M.; Dorda, R.; Negueruela, I.; Marfil, E. (2021). "The nature of VX Sagitarii". Astronomy & Astrophysics. 646: A98. arXiv:2011.09184. doi:10.1051/0004-6361/202039236. S2CID 227013580.
  4. ^ a b c d e f g h i Arroyo-Torres, B.; Wittkowski, M.; Marcaide, J. M.; Hauschildt, P. H. (2013). "The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii". Astronomy & Astrophysics. 554: A76. arXiv:1305.6179. Bibcode:2013A&A...554A..76A. doi:10.1051/0004-6361/201220920. S2CID 73575062.
  5. ^ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  6. ^ a b Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Perova, N. B. (1985). "The 67th Name-List of Variable Stars". Information Bulletin on Variable Stars. 2681: 1. Bibcode:1985IBVS.2681....1K.
  7. ^ a b c Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  8. ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). The Tycho-2 catalogue of the 2.5 million brightest stars. Astronomy and Astrophysics. Vol. 355. pp. L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862. ISBN 978-0333750889.
  9. ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  10. ^ a b c d Lee, T. A. (1970). "Photometry of high-luminosity M-type stars". Astrophysical Journal. 162: 217. Bibcode:1970ApJ...162..217L. doi:10.1086/150648.
  11. ^ "ASAS All Star Catalogue". The All Sky Automated Survey. Retrieved 8 December 2021.
  12. ^ "UY Scuti - Universe Guide". Universe Guide. Retrieved 15 January 2016.
  13. ^ Prager, R. (1927). "Katalog und Ephemeriden veraenderlicher Sterne fuer 1927". Kleine Veroeffentlichungen der Universitaetssternwarte zu Berlin Babelsberg. 1: 1.i. Bibcode:1927KVeBB...1....1P.
  14. ^ "UY Sct (UY Scuti)". kusastro. Retrieved 15 January 2016.
  15. ^ Van Loon, J. Th.; Cioni, M.-R. L.; Zijlstra, A. A.; Loup, C. (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 (1): 273–289. arXiv:astro-ph/0504379. Bibcode:2005A&A...438..273V. doi:10.1051/0004-6361:20042555. S2CID 16724272.
  16. ^ Whiting, Wendy A. (1978). "Observations of Three Variable Stars in Scutum". The Journal of the American Association of Variable Star Observers. 7 (2): 71. Bibcode:1978JAVSO...7...71W.
  17. ^ Jura, M.; Kleinmann, S. G. (1990). "Mass-losing M supergiants in the solar neighborhood". The Astrophysical Journal Supplement Series. 73: 769. Bibcode:1990ApJS...73..769J. doi:10.1086/191488.
  18. ^ Joyce, Meridith; Leung, Shing-Chi; Molnár, László; Ireland, Michael; Kobayashi, Chiaki; Nomoto, Ken'Ichi (2020). "Standing on the Shoulders of Giants: New Mass and Distance Estimates for Betelgeuse through Combined Evolutionary, Asteroseismic, and Hydrodynamic Simulations with MESA". The Astrophysical Journal. 902 (1): 63. arXiv:2006.09837. Bibcode:2020ApJ...902...63J. doi:10.3847/1538-4357/abb8db. S2CID 221507952.
  19. ^ Wehrse, R.; Scholz, M.; Baschek, B. (June 1991). "The parameters R and Teff in stellar models and observations". Astronomy and Astrophysics. 246 (2): 374–382. Bibcode:1991A&A...246..374B.
  20. ^ . NASA. Archived from the original on January 2, 2008. Retrieved 15 January 2016.
  21. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Mantelet, G.; Andrae, R. (2018). "Estimating Distance from Parallaxes. IV. Distances to 1.33 Billion Stars in Gaia Data Release 2". The Astronomical Journal. 156 (2): 58. arXiv:1804.10121. Bibcode:2018AJ....156...58B. doi:10.3847/1538-3881/aacb21. S2CID 119289017.
  22. ^ Messineo, M.; Brown, A. G. A. (2019). "A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2". The Astronomical Journal. 158 (1): 20. arXiv:1905.03744. Bibcode:2019AJ....158...20M. doi:10.3847/1538-3881/ab1cbd. S2CID 148571616.
  23. ^ Sylvester, R. J.; Skinner, C. J.; Barlow, M. J. (1998). "Silicate and hydrocarbon emission from Galactic M supergiants". Monthly Notices of the Royal Astronomical Society. 301 (4): 1083–1094. Bibcode:1998MNRAS.301.1083S. doi:10.1046/j.1365-8711.1998.02078.x.
  24. ^ Meynet, Georges (2008). Israelian, Garik (ed.). The metal-rich universe. Cambridge: Cambridge University Press. ISBN 9780521879989. Retrieved 15 January 2016.
  25. ^ Groh, Jose H.; Meynet, Georges; Georgy, Cyril; Ekström, Sylvia (2013). "Fundamental properties of core-collapse supernova and GRB progenitors: Predicting the look of massive stars before death". Astronomy & Astrophysics. 558: A131. arXiv:1308.4681. Bibcode:2013A&A...558A.131G. doi:10.1051/0004-6361/201321906. S2CID 84177572.

January 06, 2023
scuti, album, album, 5055, extreme, hypergiant, supergiant, star, constellation, scutum, considered, largest, known, stars, radius, also, pulsating, variable, star, with, maximum, brightness, magnitude, minimum, magnitude, estimated, radius, solar, radii, kilo. For the album see UY Scuti album UY Scuti BD 12 5055 is an extreme red hypergiant 3 or red supergiant star in the constellation Scutum It is considered one of the largest known stars by radius and is also a pulsating variable star with a maximum brightness of magnitude 8 29 and a minimum of magnitude 10 56 It has an estimated radius of 1 708 solar radii 1 188 109 kilometres 7 94 astronomical units thus a volume nearly 5 billion times that of the Sun It is approximately 2 9 kiloparsecs 9 500 light years from Earth If placed at the center of the Solar System its photosphere would at least engulf the orbit of Jupiter UY ScutiDSS2 image of red supergiant star UY Scuti brightest star in the image surrounded by a dense starfield Observation dataEpoch J2000 Equinox J2000Constellation ScutumRight ascension 18h 27m 36 5334s 1 Declination 12 27 58 866 1 Apparent magnitude V 8 29 10 56 2 CharacteristicsEvolutionary stage Red hypergiant 3 Spectral type M2 M4Ia Iab 2 U B color index 3 29 4 B V color index 3 00 5 Variable type SRc 6 AstrometryRadial velocity Rv 18 33 0 82 7 km sProper motion m RA 1 3 8 mas yr Dec 1 6 8 mas yrParallax p 0 5166 0 0494 mas 9 Distance9 500 1 030 10 ly 2 900 317 10 pc Absolute magnitude MV 6 2 10 DetailsMass7 10 4 M Radius1 708 192 4 R Luminosity340 000 290 000 160 000 4 L Surface gravity log g 0 5 4 cgsTemperature3 365 134 4 KOther designationsUY Sct BD 12 5055 IRC 10422 RAFGL 2162 HV 3805Database referencesSIMBADdata Contents 1 Nomenclature and history 2 Characteristics 3 Supernova 4 See also 5 ReferencesNomenclature and history A visual band light curve for UY Scuti plotted from ASAS data 11 UY Scuti was first catalogued in 1860 by German astronomers at the Bonn Observatory who were completing a survey of stars for the Bonner Durchmusterung Stellar Catalogue 12 It was designated BD 12 5055 the 5 055th star between 12 S and 13 S counting from 0h right ascension On detection in the second survey the star was found to have changed slightly in brightness suggesting that it was a new variable star In accordance with the international standard for designation of variable stars it was called UY Scuti denoting it as the 38th variable star of the constellation Scutum 13 UY Scuti is located a few degrees north of the A type star Gamma Scuti and northeast of the Eagle Nebula Although the star is very luminous it is at its brightest only 9th magnitude as viewed from Earth due to its distance and location in the Zone of Avoidance within the Cygnus rift 14 Characteristics An illustration of the approximate size of UY Scuti compared to the Sun Relative sizes of the planets in the Solar System and several stars including UY Scuti 1 Mercury lt Mars lt Venus lt Earth 2 Earth lt Neptune lt Uranus lt Saturn lt Jupiter 3 Jupiter lt Proxima Centauri lt Sun lt Sirius 4 Sirius lt Pollux lt Arcturus lt Aldebaran 5 Aldebaran lt Rigel lt Antares lt Betelgeuse 6 Betelgeuse lt NML Cygni lt VV Cephei A lt VY Canis Majoris Wittkowski et al 2012 estimate lt UY Scuti UY Scuti is a dust enshrouded bright red supergiant 15 and is classified as a semiregular variable with an approximate pulsation period of 740 days 6 16 17 Based on a radius of 1 708 R this pulsation would be an overtone of the fundamental pulsation period or it may be a fundamental mode corresponding to a smaller radius 18 In the summer of 2012 AMBER interferometry with the Very Large Telescope VLT in the Atacama Desert in Chile was used to measure the parameters of three red supergiants near the Galactic Center region 4 UY Scuti AH Scorpii and KW Sagittarii They determined that all three stars are over 1 000 times bigger than the Sun and over 100 000 times more luminous than the Sun The stars sizes were calculated using the Rosseland radius the location at which the optical depth is 2 3 19 with distances adopted from earlier publications UY Scuti was found to be the largest and the most luminous of the three stars measured at 1 708 192 R 1 188 109 134 000 000 km 7 94 0 89 AU based on an angular diameter of 5 48 0 10 mas and an assumed distance of 2 9 0 317 kiloparsecs kpc about 9 500 1 030 light years which was originally derived in 1970 based on the modelling of the spectrum of UY Scuti 10 The luminosity is then calculated to be 340 000 L at an effective temperature of 3 365 134 K giving an initial mass of 25 M possibly up to 40 M for a non rotating star 4 A hypothetical object travelling at the speed of light would be observed to take about seven hours to travel along UY Scuti s great circle whereas it would take 14 5 seconds to circle the Sun 20 Direct measurements of the parallax of UY Scuti published in the Gaia Data Release 2 give a parallax of 0 6433 0 1059 mas 7 implying a closer distance of approximately 1 5 kiloparsecs 4 900 ly 21 and consequently much lower luminosity and radius values of around 86 300 87 100 L and 755 R respectively 22 However the Gaia parallax might be unreliable at least until further observations due to a very high level of astrometric noise 7 Gaia Early Data Release 3 has published a parallax of 0 5166 0 0494 mas for this star again with a large value for astrometric noise rated at a significance of 122 where anything over 2 is probably significant 9 UY Scuti has no known companion star and so its mass is uncertain However it is expected on theoretical grounds to be between 7 and 10 M 4 Mass is being lost at 5 8 10 5 M per year leading to an extensive and complex circumstellar environment of gas and dust 23 SupernovaBased on current models of stellar evolution UY Scuti has begun to fuse helium and continues to fuse hydrogen in a shell around the core The location of UY Scuti deep within the Milky Way disc suggests that it is a metal rich star 24 After fusing heavy elements its core will begin to produce iron disrupting the balance of gravity and radiation in its core and resulting in a core collapse supernova It is expected that stars like UY Scuti should evolve back to hotter temperatures to become a yellow hypergiant luminous blue variable or a Wolf Rayet star creating a strong stellar wind that will eject its outer layers and expose the core before exploding as a type IIb IIn or type Ib Ic supernova 25 See alsoStephenson 2 18 AH Scorpii KW SagittariiReferences a b Hog E Kuzmin A Bastian U Fabricius C Kuimov K Lindegren L Makarov V V Roeser S 1998 The TYCHO Reference Catalogue Astronomy and Astrophysics 335 L65 Bibcode 1998A amp A 335L 65H a b VSX Detail for UY Sct American Association of Variable Star Observers Retrieved 2018 09 20 a b Tabernero H M Dorda R Negueruela I Marfil E 2021 The nature of VX Sagitarii Astronomy amp Astrophysics 646 A98 arXiv 2011 09184 doi 10 1051 0004 6361 202039236 S2CID 227013580 a b c d e f g h i Arroyo Torres B Wittkowski M Marcaide J M Hauschildt P H 2013 The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii UY Scuti and KW Sagittarii Astronomy amp Astrophysics 554 A76 arXiv 1305 6179 Bibcode 2013A amp A 554A 76A doi 10 1051 0004 6361 201220920 S2CID 73575062 Ducati J R 2002 VizieR Online Data Catalog Catalogue of Stellar Photometry in Johnson s 11 color system CDS ADC Collection of Electronic Catalogues 2237 0 Bibcode 2002yCat 2237 0D a b Kholopov P N Samus N N Kazarovets E V Perova N B 1985 The 67th Name List of Variable Stars Information Bulletin on Variable Stars 2681 1 Bibcode 1985IBVS 2681 1K a b c Brown A G A et al Gaia collaboration August 2018 Gaia Data Release 2 Summary of the contents and survey properties Astronomy amp Astrophysics 616 A1 arXiv 1804 09365 Bibcode 2018A amp A 616A 1G doi 10 1051 0004 6361 201833051 Gaia DR2 record for this source at VizieR a b Hog E Fabricius C Makarov V V Urban S Corbin T Wycoff G Bastian U Schwekendiek P Wicenec A 2000 The Tycho 2 catalogue of the 2 5 million brightest stars Astronomy and Astrophysics Vol 355 pp L27 Bibcode 2000A amp A 355L 27H doi 10 1888 0333750888 2862 ISBN 978 0333750889 a b Brown A G A et al Gaia collaboration 2021 Gaia Early Data Release 3 Summary of the contents and survey properties Astronomy amp Astrophysics 649 A1 arXiv 2012 01533 Bibcode 2021A amp A 649A 1G doi 10 1051 0004 6361 202039657 S2CID 227254300 Erratum doi 10 1051 0004 6361 202039657e Gaia EDR3 record for this source at VizieR a b c d Lee T A 1970 Photometry of high luminosity M type stars Astrophysical Journal 162 217 Bibcode 1970ApJ 162 217L doi 10 1086 150648 ASAS All Star Catalogue The All Sky Automated Survey Retrieved 8 December 2021 UY Scuti Universe Guide Universe Guide Retrieved 15 January 2016 Prager R 1927 Katalog und Ephemeriden veraenderlicher Sterne fuer 1927 Kleine Veroeffentlichungen der Universitaetssternwarte zu Berlin Babelsberg 1 1 i Bibcode 1927KVeBB 1 1P UY Sct UY Scuti kusastro Retrieved 15 January 2016 Van Loon J Th Cioni M R L Zijlstra A A Loup C 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 1 273 289 arXiv astro ph 0504379 Bibcode 2005A amp A 438 273V doi 10 1051 0004 6361 20042555 S2CID 16724272 Whiting Wendy A 1978 Observations of Three Variable Stars in Scutum The Journal of the American Association of Variable Star Observers 7 2 71 Bibcode 1978JAVSO 7 71W Jura M Kleinmann S G 1990 Mass losing M supergiants in the solar neighborhood The Astrophysical Journal Supplement Series 73 769 Bibcode 1990ApJS 73 769J doi 10 1086 191488 Joyce Meridith Leung Shing Chi Molnar Laszlo Ireland Michael Kobayashi Chiaki Nomoto Ken Ichi 2020 Standing on the Shoulders of Giants New Mass and Distance Estimates for Betelgeuse through Combined Evolutionary Asteroseismic and Hydrodynamic Simulations with MESA The Astrophysical Journal 902 1 63 arXiv 2006 09837 Bibcode 2020ApJ 902 63J doi 10 3847 1538 4357 abb8db S2CID 221507952 Wehrse R Scholz M Baschek B June 1991 The parameters R and Teff in stellar models and observations Astronomy and Astrophysics 246 2 374 382 Bibcode 1991A amp A 246 374B Solar System Exploration Planets Sun Facts amp Figures NASA Archived from the original on January 2 2008 Retrieved 15 January 2016 Bailer Jones C A L Rybizki J Fouesneau M Mantelet G Andrae R 2018 Estimating Distance from Parallaxes IV Distances to 1 33 Billion Stars in Gaia Data Release 2 The Astronomical Journal 156 2 58 arXiv 1804 10121 Bibcode 2018AJ 156 58B doi 10 3847 1538 3881 aacb21 S2CID 119289017 Messineo M Brown A G A 2019 A Catalog of Known Galactic K M Stars of Class I Candidate Red Supergiants in Gaia DR2 The Astronomical Journal 158 1 20 arXiv 1905 03744 Bibcode 2019AJ 158 20M doi 10 3847 1538 3881 ab1cbd S2CID 148571616 Sylvester R J Skinner C J Barlow M J 1998 Silicate and hydrocarbon emission from Galactic M supergiants Monthly Notices of the Royal Astronomical Society 301 4 1083 1094 Bibcode 1998MNRAS 301 1083S doi 10 1046 j 1365 8711 1998 02078 x Meynet Georges 2008 Israelian Garik ed The metal rich universe Cambridge Cambridge University Press ISBN 9780521879989 Retrieved 15 January 2016 Groh Jose H Meynet Georges Georgy Cyril Ekstrom Sylvia 2013 Fundamental properties of core collapse supernova and GRB progenitors Predicting the look of massive stars before death Astronomy amp Astrophysics 558 A131 arXiv 1308 4681 Bibcode 2013A amp A 558A 131G doi 10 1051 0004 6361 201321906 S2CID 84177572 Portals Astronomy Stars Spaceflight Outer space Solar System Retrieved from https en wikipedia org w index php title UY Scuti amp oldid 1123890215, wikipedia, wiki, book, books, library,

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