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MWC 480 is a single[3] star, about 500 light-years away in the constellation of Auriga. It is located in the Taurus-Auriga Star-Forming Region.[7] The name refers to the Mount Wilson Catalog of B and A stars with bright hydrogen lines in their spectra.[8] With an apparent magnitude of 7.62,[2] it is too faint to be seen with the naked eye.

MWC 480
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 04h 58m 46.2654s[1]
Declination +29° 50′ 36.990″[1]
Apparent magnitude (V) 7.62[2]
Characteristics
Spectral type A3psh3+[3]
Astrometry
Proper motion (μ) RA: 4.793[1] mas/yr
Dec.: -25.348[1] mas/yr
Parallax (π)6.1815 ± 0.0761 mas[1]
Distance528 ± 6 ly
(162 ± 2 pc)
Details
Mass1.7-2.3[4] M☉
Radius1.67[3] R☉
Luminosity11.2[3] L☉
Temperature8250[2] K
Rotational velocity (v sin i)102.0 ± 5.0[5] km/s
Age6–7.1[4] Myr
Other designations
BD+29 774, HD 31648, HIP 23143, SAO 76866, GSC 01844-00503, 2MASS J04584626+2950370[6]
Database references
SIMBADdata

Properties


Artist impression of the protoplanetary disc surrounding MWC 480.

MWC 480 is a young Herbig Ae/Be star, a class of young stars with spectral types of A or B, but are quite young and are still not main-sequence stars. MWC 480 is about 7 million years old.[4] It is about twice the mass of the Sun,[4] and is estimated to be about 1.67 solar radii.[3]

MWC 480 has X-ray emissions typical of a pre-main-sequence Herbig Ae/Be star but with an order of magnitude more photoelectric absorption.[3] It has a gas-dust envelope and is surrounded by a protoplanetary disc that is about 11% the mass of the Sun.[4] The disc is inclined about 37° towards the line of sight, on a position angle of about 148°.[4] Astronomers using the ALMA (Atacama Large Millimeter/submillimeter Array) have found that the protoplanetary disc surrounding MWC 480 contains large amounts of methyl cyanide (CH3CN), a complex carbon-based molecule.[9] Hydrogen cyanide (HCN) has also been detected in the disc.[10] No signs of planet formation have yet been detected.


Planetary system


In 2021, an imaging of the gas flows in the circumstellar disk has suggested a presence of shrouded Jupiter-mass planet about 245 AU from the star.[11]


References


Sky around the young star MWC 480
Sky around the young star MWC 480
  1. 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.
  2. Mendigutía, I.; Mora, A.; Montesinos, B.; Eiroa, C.; Meeus, G.; Merín, B.; Oudmaijer, R. D. (2012). "Accretion-related properties of Herbig Ae/Be stars". Astronomy & Astrophysics. 543: A59. doi:10.1051/0004-6361/201219110. S2CID 59384870.
  3. Grady, C. A.; Hamaguchi, K.; Schneider, G.; Stecklum, B.; Woodgate, B. E.; McCleary, J. E.; Williger, G. M.; Sitko, M. L.; Ménard, F.; Henning, Th.; Brittain, S.; Troutmann, M.; Donehew, B.; Hines, D.; Wisniewski, J. P.; Lynch, D. K.; Russell, R. W.; Rudy, R. J.; Day, A. N.; Shenoy, A.; Wilner, D.; Silverstone, M.; Bouret, J.-C.; Meusinger, H.; Clampin, M.; Kim, S.; Petre, R.; Sahu, M.; Endres, M.; Collins, K. A. (2010). "Locating the Accretion Footprint on a Herbig Ae Star: MWC 480". The Astrophysical Journal. 719 (2): 1565–1581. Bibcode:2010ApJ...719.1565G. doi:10.1088/0004-637X/719/2/1565.
  4. Loomis, Ryan A.; Öberg, Karin I.; Andrews, Sean M.; Bergin, Edwin; Bergner, Jennifer; Blake, Geoffrey A.; Cleeves, L. Ilsedore; Czekala, Ian; Huang, Jane; Le Gal, Romane; Ménard, Francois; Pegues, Jamila; Qi, Chunhua; Walsh, Catherine; Williams, Jonathan P.; Wilner, David J. (2020). "An Unbiased ALMA Spectral Survey of the Lk Ca 15 and MWC 480 Protoplanetary Disks". The Astrophysical Journal. 893 (2): 101. arXiv:2006.16187. Bibcode:2020ApJ...893..101L. doi:10.3847/1538-4357/ab7cc8. S2CID 219077531.
  5. Mora, A.; Merín, B.; Solano, E.; Montesinos, B.; De Winter, D.; Eiroa, C.; Ferlet, R.; Grady, C. A.; Davies, J. K.; Miranda, L. F.; Oudmaijer, R. D.; Palacios, J.; Quirrenbach, A.; Harris, A. W.; Rauer, H.; Collier Cameron, A.; Deeg, H. J.; Garzón, F.; Penny, A.; Schneider, J.; Tsapras, Y.; Wesselius, P. R. (2001). "EXPORT: Spectral classification and projected rotational velocities of Vega-type and pre-main sequence stars". Astronomy and Astrophysics. 378: 116. Bibcode:2001A&A...378..116M. doi:10.1051/0004-6361:20011098.
  6. "HD 31648". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 July 2020.
  7. K. L. Luhman; et al. (2010). "The Disk Population of the Taurus Star-Forming Region". The Astrophysical Journal Supplement Series. 186 (1): 111–174. arXiv:0911.5457. Bibcode:2010ApJS..186..111L. doi:10.1088/0067-0049/186/1/111. S2CID 119189843.
  8. "Catalog of Resolved Circumstellar Disks". Circumstellardisks.org. Archived from the original on 2015-02-05. Retrieved 2015-04-08.
  9. "Complex Organic Molecules Discovered in Infant Star System". Eso.org. Retrieved 2015-04-08.
  10. "Complex Organic Molecules Discovered Around Star MWC 480". Science 2.0. 7 April 2015. Retrieved 2015-04-08.
  11. Molecules with ALMA at Planet-forming Scales (MAPS XVIII): Kinematic Substructures in the Disks of HD 163296 and MWC 480, 2021, arXiv:2109.06218


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На других языках

[de] MWC 480

MWC 480 (HD 31648) ist ein Herbig-Ae/Be-Stern in der Taurus Sternentstehungsregion im Sternbild Taurus.[2] Um den Stern hat sich eine protoplanetare Scheibe geformt. Seine Röntgenstrahlen ähneln denen eines gewöhnlichen Herbig Ae Sterns, jedoch ist im Unterschied zu diesen Sternen die fotoelektrische Absorption zehnmal größer als man erwarten könnte.[3] Mit Hilfe des ALMA-Teleskops wurden zum ersten Mal auch komplexe Kohlenwasserstoffe (Acetonitril) in einem jungen Stern gefunden, welche für die Entstehung von Leben wichtig sind.[4]
- [en] MWC 480

[ru] MWC 480

MWC 480 — молодая звезда в созвездии Возничего. Её возраст составляет всего около миллиона лет. Обозначение MWC 480 соответствует каталогу обсерватории Маунт-Вилсон звёзд типов B и A с яркими водородными линиями в спектрах.


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