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{{Starbox detail
{{Starbox detail
| mass = ~10<ref name=void/><ref name=massloss>{{cite journal|bibcode=2009ApJ...697..409D|arxiv=0903.3714v1|title=Probing the Mass-Loss History of the Yellow Hypergiant IRC+10420|journal=The Astrophysical Journal|volume=697|pages=409|author1=Dinh-V.-Trung|last2=Muller|first2=Sébastien|last3=Lim|first3=Jeremy|last4=Kwok|first4=Sun|last5=Muthu|first5=C.|year=2009|doi=10.1088/0004-637X/697/1/409}}</ref>
| mass = ~10<ref name=void/><ref name=massloss>{{cite journal|bibcode=2009ApJ...697..409D|arxiv=0903.3714v1|title=Probing the Mass-Loss History of the Yellow Hypergiant IRC+10420|journal=The Astrophysical Journal|volume=697|pages=409|author1=Dinh-V.-Trung|last2=Muller|first2=Sébastien|last3=Lim|first3=Jeremy|last4=Kwok|first4=Sun|last5=Muthu|first5=C.|year=2009|doi=10.1088/0004-637X/697/1/409}}</ref>
| radius = {{nowrap|357<ref name=massloss/>{{efn|name=radius}}}} - 1,342<ref name=debeck>{{cite journal|bibcode=2010A&A...523A..18D|arxiv=1008.1083|title=Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae|journal=Astronomy and Astrophysics|volume=523|pages=A18|author1=De Beck|first1=E.|last2=Decin|first2=L.|last3=De Koter|first3=A.|last4=Justtanont|first4=K.|last5=Verhoelst|first5=T.|last6=Kemper|first6=F.|last7=Menten|first7=K. M.|year=2010|doi=10.1051/0004-6361/200913771}}</ref>
| radius = {{nowrap|357<ref name=massloss/>{{efn|name=radius}}}} (- 1,342)<ref name=debeck>{{cite journal|bibcode=2010A&A...523A..18D|arxiv=1008.1083|title=Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae|journal=Astronomy and Astrophysics|volume=523|pages=A18|author1=De Beck|first1=E.|last2=Decin|first2=L.|last3=De Koter|first3=A.|last4=Justtanont|first4=K.|last5=Verhoelst|first5=T.|last6=Kemper|first6=F.|last7=Menten|first7=K. M.|year=2010|doi=10.1051/0004-6361/200913771}}</ref>
| luminosity =
| luminosity =
| luminosity_bolometric = 500,000<ref name=tiffany/>
| luminosity_bolometric = 500,000<ref name=tiffany/>

Revision as of 05:32, 8 September 2018

IRC+10420

MERLIN and e-VLBI observations of the OH masers in IRC+10420
Credit: Joint Institute for VLBI in Europe (JIVE)
Observation data
Epoch 2000      Equinox
Constellation Aquila
Right ascension 19h 26m 48.095s[1]
Declination +11° 21′ 16.74″[1]
Apparent magnitude (V) 11.66[2]
Characteristics
Evolutionary stage yellow hypergiant
Spectral type F8Ia+[3]-A2I[4][5][6]
B−V color index 2.32[2]
Variable type unique[7]
Astrometry
Distance4,000-6,000[6] pc
Absolute magnitude (MV)−9.5[5]
Details
Mass~10[4][8] M☉
Radius357[8][a] (- 1,342)[9] R☉
Luminosity (bolometric)500,000[6] L☉
Surface gravity (log g)0.01[4] cgs
Temperature6,000-8,000[4] K
Metallicity [Fe/H]-0.18[4] dex
Other designations
IRC+10420, V1302 Aql, IRAS 19244+1115, AAVSO 1922+11
Database references
SIMBADdata

IRC+10420, also known as V1302 Aql, is a yellow hypergiant star located in the constellation of Aquila at a distance of 4-6 kiloparsecs of the Sun.

Discovery

IRC+10420 and its circumstellar material

IRC+10420 was first identified in the 1969 Infrared Catalogue of 2.2 micron sources.[10] It was quickly noted as a very unusual object after being detected at 20 microns as one of the brightest sources in the sky with a large infrared excess, and was compared to Eta Carinae during one of its outbursts.[3] It was also discovered to be a strong source of OH maser emission.[11]

It was formally catalogued as variable star V1302 Aquilae.[12] Identification on historical photographic plates showed possible irregular variations of about a magnitude before 1925, followed by a smooth gradual increase in brightness from magnitude 15 to brighter than magnitude 14 by 1976.[13]

Some authors had grouped IRC+10420 with the proto-planetary nebulae because of the surrounding nebulosity, but it was widely recognised as a highly luminous supergiant.[14]

Physical properties

Despite being one of the most luminous stars known, 500,000 times brighter than the Sun,[6] IRC+10420 cannot be seen with the naked eye and needs a telescope to be observed.

IRC+10420's spectrum has changed from late F to early A in recent decades without experiencing changes in its luminosity. This suggests IRC+10420 is a former red supergiant that is evolving blueward on the Hertzsprung-Russell diagram to become a Luminous Blue Variable, or Wolf–Rayet star. Models suggest it started its life as a 40-50 solar masses star that lost most of its mass due to strong stellar winds leaving it with just 10 solar masses and that the star - which actually has a high surface temperature - is totally enshrouded in the matter it has expelled appearing as a fake photosphere, so IRC+10420 appears with a later spectral type as humans see just the expelled dust and gas it has blown out during its life and not the star itself.[citation needed]

Surrounding nebula

IRC+10420 is surrounded by a reflection nebula with a mass of 30-40 solar masses that has been made by the material expelled by the strong stellar winds of its central star. This nebula has been studied with the help of the Hubble Space Telescope, showing a complex structure that includes arcs, rays, and condensations and that has been compared by the one surrounding the red hypergiant VY Canis Majoris. The star and its surrounding material have been compared to IRAS 17163-3907.[15]

References

  1. ^ a b Cutri, R. M.; Skrutskie, M. F.; Van Dyk, S.; Beichman, C. A.; Carpenter, J. M.; Chester, T.; Cambresy, L.; Evans, T.; Fowler, J.; Gizis, J.; Howard, E.; Huchra, J.; Jarrett, T.; Kopan, E. L.; Kirkpatrick, J. D.; Light, R. M.; Marsh, K. A.; McCallon, H.; Schneider, S.; Stiening, R.; Sykes, M.; Weinberg, M.; Wheaton, W. A.; Wheelock, S.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". VizieR On-line Data Catalog: II/246. Originally published in: 2003yCat.2246....0C. 2246. Bibcode:2003yCat.2246....0C.
  2. ^ 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. 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862.
  3. ^ a b Humphreys, Roberta M.; Strecker, D. W.; Murdock, T. L.; Low, F. J. (1973). "IRC+10420-ANOTHER Eta Carinae?". Astrophysical Journal. 179: L49. Bibcode:1973ApJ...179L..49H. doi:10.1086/181114.
  4. ^ a b c d e Nieuwenhuijzen, H.; De Jager, C. (2000). "Checking the yellow evolutionary void. Three evolutionary critical Hypergiants: HD 33579, HR 8752 & IRC +10420". Astronomy and Astrophysics. 353: 163. Bibcode:2000A&A...353..163N.
  5. ^ a b Klochkova, V. G.; Yushkin, M. V.; Chentsov, E. L.; Panchuk, V. E. (2002). "Evolutionary Changes in the Optical Spectrum of the Peculiar Supergiant IRC+10420". Astronomy Reports. 46 (2): 139. Bibcode:2002ARep...46..139K. doi:10.1134/1.1451927.
  6. ^ a b c d Tiffany, C.; Humphreys, R. M.; Jones, T. J.; Davidson, K. (2010). "THE MORPHOLOGY OF IRC+10420's CIRCUMSTELLAR EJECTA". The Astronomical Journal. 140 (2): 339. arXiv:1006.0501. Bibcode:2010AJ....140..339T. doi:10.1088/0004-6256/140/2/339.
  7. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  8. ^ a b Dinh-V.-Trung; Muller, Sébastien; Lim, Jeremy; Kwok, Sun; Muthu, C. (2009). "Probing the Mass-Loss History of the Yellow Hypergiant IRC+10420". The Astrophysical Journal. 697: 409. arXiv:0903.3714v1. Bibcode:2009ApJ...697..409D. doi:10.1088/0004-637X/697/1/409.
  9. ^ De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics. 523: A18. arXiv:1008.1083. Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771.
  10. ^ Neugebauer, G.; Leighton, R. B. (1969). "Two-micron sky survey. A preliminary catalogue". Nasa Sp. Bibcode:1969tmss.book.....N.
  11. ^ Giguere, P. T.; Woolf, N. J.; Webber, J. C. (1976). "IRC +10 420 - A hot supergiant maser". Astrophysical Journal. 207: L195. Bibcode:1976ApJ...207L.195G. doi:10.1086/182211.
  12. ^ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P. (1975). "61st Name-List of Variable Stars". Information Bulletin on Variable Stars. 1068: 1. Bibcode:1975IBVS.1068....1K.
  13. ^ Gottlieb, E. W.; Liller, W. (1978). "Photometric histories of six infrared objects and three highly reddened blue supergiants". Astrophysical Journal. 225: 488. Bibcode:1978ApJ...225..488G. doi:10.1086/156509.
  14. ^ Jones, Terry Jay; Humphreys, Roberta M.; Gehrz, Robert D.; Lawrence, Geoffrey F.; Zickgraf, Franz-Josef; Moseley, Harvey; Casey, Sean; Glaccum, William J.; Koch, Carol J.; Pina, Robert; Jones, Barbara; Venn, Kim; Stahl, Otmar; Starrfield, Sumner G. (1993). "IRC +10420 - A cool hypergiant near the top of the H-R diagram". Astrophysical Journal. 411: 323. Bibcode:1993ApJ...411..323J. doi:10.1086/172832.
  15. ^ Lagadec, E.; Zijlstra, A. A.; Oudmaijer, R. D.; Verhoelst, T.; Cox, N. L. J.; Szczerba, R.; Mékarnia, D.; Van Winckel, H. (2011). "A double detached shell around a post-red supergiant: IRAS 17163-3907, the Fried Egg nebula". Astronomy & Astrophysics. 534: L10. arXiv:1109.5947. Bibcode:2011A&A...534L..10L. doi:10.1051/0004-6361/201117521.

Notes

  1. ^ published as 1.66 AU

Further reading

<<< 10. VV Cephei A 12. SMC 018136 >>>
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