WR 133

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WR 133
V1676CygLightCurve.png
A light curve for V1676 Cygni, adapted from Marchenko et al. (1998) [1]
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Cygnus
Right ascension 20h 05m 57.32445s [2]
Declination +35° 47′ 18.1508″ [2]
Apparent magnitude  (V)6.75 - 6.84 [3]
Characteristics
Spectral type WN5o + O9I [4]
Apparent magnitude  (J)6.319 [5]
Apparent magnitude  (K)6.247 [5]
U−B color index −0.77 [6]
B−V color index +0.13 [6]
Variable type WR [3]
Astrometry
Proper motion (μ)RA: −3.175 [2]   mas/yr
Dec.: −6.537 [2]   mas/yr
Parallax (π)0.5380 ± 0.0223  mas [2]
Distance 6,100 ± 300  ly
(1,860 ± 80  pc)
Absolute magnitude  (MV)−3.4 / −5.4 [7]
Orbit [4]
Period (P)112.736±0.073 days
Semi-major axis (a)0.7791±0.0024″
Eccentricity (e)0.3646±0.0103
Inclination (i)162.08±1.74°
Semi-amplitude (K1)
(primary)		13.41±2.34 km/s
Semi-amplitude (K2)
(secondary)		32.56±3.98 km/s
Details [4]
WR
Mass 9.3±1.6  M☉
Radius 3.4±0.5  R☉
Luminosity 263,000+68,000
−54,000  L☉
Temperature 71,000±5,000  K
O
Mass 22.6±3.2  M☉
Radius 16.6±1.0  R☉
Luminosity195,000+50,000
−40,000  L☉
Surface gravity (log g)3.30±0.15  cgs
Temperature 30,000±1,000  K
Rotational velocity (v sin i)96±10 km/s
Other designations
V1676  Cygni, BD+35°3953, HD  190918, HIP  99002, WDS  J20060+3547, 2MASS J20055731+3547181
Database references
SIMBAD data

WR 133 is a visually moderately bright Wolf-Rayet star. It is a spectroscopic binary system containing a Wolf-Rayet primary and a class O supergiant secondary. It is in the constellation of Cygnus, lying in the sky at the centre of the triangle formed by β and γ Cygni, near η Cygni. It is the brightest member of the sparse open cluster NGC 6871.

WR 133 is one of the brightest Wolf Rayet (WR) stars in the northern hemisphere, slightly brighter than WR 140 which also in Cygnus. [8] The WR star is typically identified as the primary, being more luminous, and dominating the spectrum. However, the supergiant secondary is more massive and visually brighter. The primary star is a WN5 nitrogen-rich WR star and the secondary has a spectral type of O9I. The orbit is moderately eccentric and has a period of 113 d, which has been determined from the velocity variations observed with the component's spectral lines, mostly from the HeII emission lines at 541.1  nm for the WR primary, and helium and oxygen absorption lines for the primary. This is the first WN-type WR star to have its mass dynamically determined from orbital motion, although the precision is hampered by the nearly face-on orientation of the orbit. [4]

WR 133 is listed as a Wolf-Rayet variable star and has been given the variable star designation V1676 Cyg in the General Catalogue of Variable Stars. Its visual magnitude varies between 6.75 and 6.84. [3]

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<span class="mw-page-title-main">Theta Muscae</span> Star in the constellation Musca

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<span class="mw-page-title-main">WR 134</span> Star in the constellation of Cygnus

WR 134 is a variable Wolf-Rayet star located around 6,000 light years away from Earth in the constellation of Cygnus, surrounded by a faint bubble nebula blown by the intense radiation and fast wind from the star. It is five times the radius of the sun, but due to a temperature over 63,000 K it is 400,000 times as luminous as the Sun.

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<span class="mw-page-title-main">WR 31a</span> Wolf Rayet star in the constellation Carina

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<span class="mw-page-title-main">BC Cygni</span> Star in the constellation Cygnus

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WR 135 is a variable Wolf-Rayet star located around 6,000 light years away from Earth in the constellation of Cygnus, surrounded by a faint bubble nebula blown by the intense radiation and fast wind from the star. It is just over four times the radius of the sun, but due to a temperature of 63,000 K it is 250,000 times as luminous as the sun.

<span class="mw-page-title-main">WR 137</span> Star in the constellation of Cygnus

WR 137 is a variable Wolf-Rayet star located around 6,000 light years away from Earth in the constellation of Cygnus.

<span class="mw-page-title-main">WR 86</span>

WR 86 is a visual binary in the constellation Scorpius consisting of a Wolf-Rayet star and a β Cephei variable. It lies 2° west of NGC 6357 on the edge of the Great Rift in the Milky Way in the tail of the Scorpion.

<span class="mw-page-title-main">WR 140</span> Star in the constellation of Cygnus

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<span class="mw-page-title-main">WR 1</span> Star in the constellation Cassiopeia

WR 1 is a Wolf-Rayet star located around 10,300 light years away from Earth in the constellation of Cassiopeia. It is only slightly more than twice the size of the sun, but due to a temperature over 100,000 K it is over 758,000 times as luminous as the sun.

<span class="mw-page-title-main">WR 12</span> Star in the constellation Vela

WR 12 is a spectroscopic binary in the constellation Vela. It is an eclipsing binary consisting of a Wolf-Rayet star and a luminous companion of unknown spectral type. The primary is one of the most luminous stars known.

<span class="mw-page-title-main">WR 9</span> Spectroscopic binary star system in the constellation Puppis

WR 9 is a spectroscopic binary in the constellation Puppis consisting of a Wolf-Rayet star and a class O star. It is around 12,000 light years away.

<span class="mw-page-title-main">HD 151932</span> Star in the constellation of Scorpius

HD 151932, also known as WR 78, is a Wolf-Rayet star located in the constellation Scorpius, close to the galactic plane. Its distance is around 1,300 parsecs away from the Earth. Despite being a blue-colored Wolf-Rayet star, it is extremely reddened by interstellar extinction, so its apparent magnitude is brighter for longer-wavelength passbands. HD 151932 lies about 22′ west of the open cluster NGC 6231, the center of the OB association Scorpius OB1; it is not clear whether it is a part of the association or not. With an apparent magnitude of about 6.5, it is one of the few Wolf-Rayet stars that can be seen with the naked eye.

References

  1. ↑ Marchenko, S. V.; Moffat, A. F. J.; van der Hucht, K. A.; Seggewiss, W.; Schrijver, H.; Stenholm, B.; Lundström, I.; Setia Gunawan, D. Y. A.; Sutantyo, W.; van den Heuvel, E. P. J.; De Cuyper, J. P.; Gómez, A. E. (March 1998). "Wolf-Rayet stars and O-star runaways with HIPPARCOS II. Photometry". Astronomy and Astrophysics. 331: 1022–1036. Bibcode:1998A&A...331.1022M . Retrieved 28 December 2021.
  2. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  3. 1 2 3 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.
  4. 1 2 3 4 Richardson, Noel D.; Lee, Laura; Schaefer, Gail; Shenar, Tomer; Sander, Andreas A. C.; Hill, Grant M.; Fullard, Andrew G.; Monnier, John D.; Anugu, Narsireddy; Claire L Davies; Gardner, Tyler; Lanthermann, Cyprien; Kraus, Stefan; Setterholm, Benjamin R. (2021). "The First Dynamical Mass Determination of a Nitrogen-rich Wolf-Rayet Star using a Combined Visual and Spectroscopic Orbit". The Astrophysical Journal. 908 (1): L3. arXiv: 2101.04232 . Bibcode:2021ApJ...908L...3R. doi:10.3847/2041-8213/abd722. S2CID   231582956.
  5. 1 2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  6. 1 2 Ducati, J. R. (2002). "VizieR On-line Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  7. ↑ Massey, P.; Degioia-Eastwood, K.; Waterhouse, E. (2001). "The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. II. Results from 12 Galactic Clusters and OB Associations". The Astronomical Journal. 121 (2): 1050–1070. arXiv: astro-ph/0010654 . Bibcode:2001AJ....121.1050M. doi:10.1086/318769. S2CID   53345173.
  8. ↑ Fahed, R.; Moffat, A. F. J.; Zorec, J.; Eversberg, T.; Chené, A. N.; Alves, F.; Arnold, W.; Bergmann, T.; Corcoran, M. F.; Correia Viegas, N. G.; Dougherty, S. M.; Fernando, A.; Frémat, Y.; Gouveia Carreira, L. F.; Hunger, T.; Knapen, J. H.; Leadbeater, R.; Marques Dias, F.; Martayan, C.; Morel, T.; Pittard, J. M.; Pollock, A. M. T.; Rauw, G.; Reinecke, N.; Ribeiro, J.; Romeo, N.; Sánchez-Gallego, J. R.; Dos Santos, E. M.; Schanne, L.; et al. (2011). "Spectroscopy of the archetype colliding-wind binary WR 140 during the 2009 January periastron passage". Monthly Notices of the Royal Astronomical Society. 418 (1): 2–13. Bibcode:2011MNRAS.418....2F. doi: 10.1111/j.1365-2966.2011.19035.x .
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