UY Scuti: Difference between revisions
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==Mass== |
==Mass== |
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UY Scuti's mass is also uncertain, primarily because it has no visible companion star by which its mass can be measured through gravitational interference. Stellar evolutionary models conclude that the initial mass of a star (the mass of a star when it is formed) reaching the red supergiant stage like UY Scuti would have been around {{solar mass|25}} (possibly up to {{solar mass|40}} for a non-rotating star), and has probably lost more than half of that.<ref name="Torres2013"/> |
UY Scuti's mass is also uncertain, primarily because it has no visible companion star by which its mass can be measured through gravitational interference. Stellar evolutionary models conclude that the initial mass of a star (the mass of a star when it is formed, expressed in [[solar mass]]es,) reaching the red supergiant stage like UY Scuti would have been around {{solar mass|25}} (possibly up to {{solar mass|40}} for a non-rotating star), and has probably lost more than half of that.<ref name="Torres2013"/> |
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==Supernova== |
==Supernova== |
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Revision as of 08:42, 20 July 2018
File:UY Scuti zoomed in, Rutherford Observatory, 07 September 2014.jpeg Dense starfield around the red supergiant star UY Scuti (brightest star in the image) as seen from the Rutherfurd Observatory in the Columbia University in New York, United States. The picture was captured in 2011. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Scutum |
| Right ascension | 18h 27m 36.5334s[1] |
| Declination | −12° 27′ 58.866″[1] |
| Apparent magnitude (V) | 8.9[2] - 11.20[3] |
| Characteristics | |
| Spectral type | M4Ia[4] |
| U−B color index | 3.29[4] |
| B−V color index | 3.00[3] |
| Variable type | SRC[5] |
| Astrometry | |
| Proper motion (μ) | RA: 1.3[6] mas/yr Dec.: −1.6[6] mas/yr |
| Parallax (π) | 0.6433 ± 0.1059 mas[7] |
| Distance | 9,500 ly (2,900[8] pc) |
| Absolute magnitude (MV) | −6.2[9] |
| Details | |
| Mass | 7–10[4] M☉ |
| Radius | 1,708 ± 192[4] R☉ |
| Luminosity | 340,000[4] L☉ |
| Surface gravity (log g) | −0.5[4] cgs |
| Temperature | 3,365 ± 134[4] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
UY Scuti is a red supergiant and pulsating variable star in the constellation Scutum. It is one of the largest known stars by radius.
Nomenclature and history
UY Scuti was first cataloged in 1860, by German astronomers at the Bonn Observatory, during the first sky survey of stars for the Bonner Durchmusterung Stellar Catalogue.[10] It was named BD -12 5055, the 5,055th star between 12°S and 13°S counting from 0h right ascension.
On the next detection of the star in the second survey, it was found to have changed slightly in brightness, suggesting that it was a new variable star. In accordance with the international standard of designation of variable stars, it was called UY Scuti, the 38th variable star of the constellation Scutum (see variable star designation).[11]
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.[12]
Characteristics
The star is classified as a semiregular variable with an approximate pulsation period of 740 days.[5][13] [14]
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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.
In the summer of 2012, astronomers from the Very Large Telescope in the Atacama Desert in Chile measured 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 Sun. The stars' sizes were calculated using the Rosseland Radius, the location at which the optical depth is 2/3,[15] 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☉ which larger than the orbit of Jupiter, and at 340,000 L☉, at an assumed distance of 2.9 kpc. An effective temperature of 3,365 ± 134 K was derived from the radius and the luminosity.[4]
A hypothetical object travelling at the speed of light would take about seven hours to travel around UY Scuti at maximum, whereas it would take 14.5 seconds to circle the Sun.[16]
Mass
UY Scuti's mass is also uncertain, primarily because it has no visible companion star by which its mass can be measured through gravitational interference. Stellar evolutionary models conclude that the initial mass of a star (the mass of a star when it is formed, expressed in solar masses,) reaching the red supergiant stage like UY Scuti would have been around 25 M☉ (possibly up to 40 M☉ for a non-rotating star), and has probably lost more than half of that.[4]
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.[17]
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.[18]
See also
References
- ^ 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.
- ^ Röser, S.; Bastian, U.; Kuzmin, A. (1994). "PPM Star Catalogue: The 90000 Stars Supplement". Astronomy and Astrophysics. 105. Bibcode:1994A&AS..105..301R.
- ^ a b 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 c d e f g h i j 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.
- ^ 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 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.
- ^ 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.
- ^ 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.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ Lee, T. A. (1970). "Photometry of high-luminosity M-type stars". Astrophysical Journal. 162: 217. Bibcode:1970ApJ...162..217L. doi:10.1086/150648.
- ^ "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.
- ^ Whiting, Wendy A. (1978). "Observations of Three Variable Stars in Scutum". The Journal of the American Association of Variable Star Observers. 7: 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.
- ^ 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.
- ^ "Solar System Exploration: Planets: Sun: Facts & Figures". NASA. Archived from the original on January 2, 2008. Retrieved 15 January 2016.
{{cite web}}: Unknown parameter|deadurl=ignored (|url-status=suggested) (help) - ^ 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; 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.
