Ceci est une version archivée de cette page, en date du 22 juillet 2021 à 20:00 et modifiée en dernier par Do not follow(discuter | contributions). Elle peut contenir des erreurs, des inexactitudes ou des contenus vandalisés non présents dans la version actuelle.
UY Scuti est si gigantesque que si la Terre avait le diamètre d'un ballon de plage de 20 cm, le Soleil mesurerait 22 m et UY Scuti aurait un diamètre d'environ 40 km.
Une masse d'environ 315 masses solaires en fait l'étoile la plus massive jamais observée. Avant cette découverte, les astrophysiciens pensaient que la masse stellaire maximum était 150 M☉.
↑Monthly Notices of the Royal Astronomical Society, "The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 Msun stellar mass limit", Paul A Crowther, Olivier Schnurr, Raphael Hirschi, Norhasliza Yusof, Richard J Parker, Simon P Goodwin, Hasan Abu Kassim, Volume 408, Issue 2, pp. 731-751, October 2010, doi:10.1111/j.1365-2966.2010.17167.x , Bibcode: 2010MNRAS.408..731C , arXiv:1007.3284
↑Dieterich, Sergio B.; Henry, Todd J.; Jao, Wei-Chun; Winters, Jennifer G.; Hosey, Altonio D.; Riedel, Adric R.; Subasavage, John P. (2013). "The Solar Neighborhood XXXII. The Hydrogen Burning Limit". eprint arXiv:1312.1736.
↑11th European Workshop on White Dwarfs, ASP Conference Series #169, "RX J2117+3412, the hottest known pulsating PG 1159 star", Vauclair, G.; Moskalik, P.; The Wet Team, 1999, (ISBN1-886733-91-0) , Bibcode : 1999ASPC..169...96V , pg.96
↑Alexander von Boetticher, Amaury H.M.J. Triaud, Didier Queloz, Sam Gill, Monika Lendl, Laetitia Delrez, David R. Anderson, Andrew Collier Cameron, Francesca Faedi, Michaël Gillon, Yilen Gómez Maqueo Chew, Leslie Hebb, Coel Hellier, Emmanuël Jehin, Pierre F.L. Maxted, David V. Martin, Francesco Pepe, Don Pollacco, Damien Ségransan, Barry Smalley, Stéphane Udry, Richard West, « The EBLM project; III. A Saturn-size low-mass star at the hydrogen-burning limit », Astronomy & Astrophysics, vol. 604, , p. L6 (DOI10.1051/0004-6361/201731107, Bibcode2017A&A...604L...6V, arXiv1706.08781)
↑Astrophysical Journal Letters, "Brown Dwarfs in the Pleiades Cluster Confirmed by the Lithium Test", Rebolo, R.; Martin, E. L.; Basri, G.; Marcy, G. W.; Zapatero-Osorio, M. R., v.469, p.L53, September 1996, doi:10.1086/310263 , Bibcode: 1996ApJ...469L..53R , arXiv:astro-ph/9607002
↑Astronomical Society of the Pacific Conference Series, 'In Cool Stars, Stellar Systems, and the Sun: Ninth Cambridge Workshop', "An I. K Survey of the Pleiades", Jameson, R. F.; Hodgkin, S. T.; Pinfield, D. J., vol. 109, p. 363, eds. R. Pallavicini, A. K. Dupree, 1996, Bibcode: 1996ASPC..109..363J
↑Bulletin of the American Astronomical Society, "The Record Breaking Magnetic White Dwarf RE J0317-853", Burleigh, M. R.; Jordan, S., Vol. 29, p.1234, January 1998, Bibcode: 1998AAS...191.1511B
↑Wolfram Scienceworld, "White Dwarf", Eric W. Weisstein, 2007 (accessed 2010-30-10)
↑Hayden Planetarium, "Stellar Orbits", Sébastien Lépine, Brian Abbott (accessed 2010-11-20)
↑Ohio State University, Astronomy 143: The History of the Universe (Fall 2009); "Stars and Galaxies in Motion", Barbara Sue Ryden, 15 October 2009 (accessed 2010-11-20)
↑ Astronomy & Astrophysics Supplement Series, "MSC - a catalogue of physical multiple stars", Tokovinin, A. A., Vol. 124, July 1997, pp.75-84, July 1997, doi:10.1051/aas:1997181 , Bibcode: 1997A&AS..124...75T , VizieR (accessed 2010-10-27)
↑Monthly Notices of the Royal Astronomical Society, "A catalogue of multiplicity among bright stellar systems", Eggleton, P. P.; Tokovinin, A. A., Volume 389, Issue 2, pp. 869-879, September 2008, doi:10.1111/j.1365-2966.2008.13596.x , Bibcode: 2008MNRAS.389..869E , arXiv:0806.2878v1 , VizieR (accessed 2010-10-27)