IRC +10420 was first identified in the 1969 Infrared Catalogue of 2.2 micron sources.[12] 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 largeinfrared excess, and was compared toEta Carinae during one of its outbursts.[3] It was also discovered to be a strong source ofOHmaser emission.[13]
It was formally catalogued as variable star V1302 Aquilae.[14] 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.[11]
Some authors had grouped IRC +10420 with theproto-planetary nebulae because of the surrounding nebulosity, but it was widely recognised as a highly luminous supergiant.[15]
IRC +10420'sspectrum has changed from late F to early A in recent decades without experiencing changes in its luminosity. This suggests IRC +10420 is a formerred supergiant that is evolving blueward on theHertzsprung-Russell diagram to become aluminous blue variable, orWolf–Rayet star. Models suggest it started its life as a 40-50solar 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 fakephotosphere, 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]
IRC +10420 is surrounded by areflection 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 theHubble Space Telescope, showing a complex structure that includes arcs, rays, and condensations and that has been compared to the one surrounding the red hypergiantVY Canis Majoris. The star and its surrounding material have been compared toIRAS 17163-3907.[16]
^abHøg, 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.
^abHumphreys, 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.
^abcdeNieuwenhuijzen, 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.
^abKlochkova, 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.S2CID84835394.
^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.
^abGottlieb, 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.
^Neugebauer, G.; Leighton, R. B. (1969). "Two-micron sky survey. A preliminary catalogue".NASA Sp.Bibcode:1969tmss.book.....N.
^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.
^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.S2CID55754316.
Volk, Bruce J.; Kwok, Sun; Volk, Kevin M. (1989). "A study of several F and G supergiant-like stars with infrared excesses as candidates for proto-planetary nebulae".Astrophysical Journal.346: 265.Bibcode:1989ApJ...346..265H.doi:10.1086/168007.
Humphreys, Roberta M. (2007). "The Circumstellar Environments of the Cool Hypergiants: Implications for the Mass Loss Mechanism".Revista Mexicana de Astronomía y Astrofísica.30:6–11.Bibcode:2007RMxAC..30....6H.ISSN0185-1101.
Humphreys, Roberta M.; Davidson, Kris; Smith, Nathan (2002). "Crossing the Yellow Void: Spatially Resolved Spectroscopy of the Post–Red Supergiant IRC +10420 and Its Circumstellar Ejecta".The Astronomical Journal.124 (2): 1026.arXiv:astro-ph/0205247.Bibcode:2002AJ....124.1026H.doi:10.1086/341380.S2CID15274760.
Humphreys, Roberta M.; Smith, Nathan; Davidson, Kris; Jones, Terry Jay; Gehrz, Robert T.; Mason, Christopher G.; Hayward, Thomas L.; Houck, James R.; Krautter, Joachim (1997). "HST and Infrared Images of the Circumstellar Environment of the Cool Hypergiant IRC + 10420".Astronomical Journal.114: 2778.Bibcode:1997AJ....114.2778H.doi:10.1086/118686.
