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WR 9
	; A visual band light curve for V443 Puppis, plotted from data published by Lamontagne et al. (1996)
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Puppis
Right ascension	07h 45m 50.3992s
Declination	−34° 19′ 48.500″
Apparent magnitude (V)	10.50
Characteristics
Spectral type	WC4 + O7
Apparent magnitude (J)	8.452
Apparent magnitude (K)	7.545
U−B color index	+0.04
B−V color index	+0.93
Variable type	Eclipsing + WR
Astrometry
Radial velocity (Rv)	321 ± 12 km/s
Proper motion (μ)	RA: −2.159 mas/yr ; Dec.: +3.175 mas/yr
Parallax (π)	0.2717 ± 0.0137 mas
Distance	12,000 ± 600 ly ; (3,700 ± 200 pc)
Absolute magnitude (MV)	WR: −3.34; O: −4.01
Orbit
Period (P)	14.305
Semi-major axis (a)	123 R☉
Eccentricity (e)	0
Inclination (i)	55±34°
Semi-amplitude (K1); (primary)	186±19 km/s
Semi-amplitude (K2); (secondary)	56±28 km/s
Details
WR
Mass	9 M☉
Radius	5 R☉
Luminosity	500,000 L☉
Temperature	139,700 K
O
Mass	32 M☉
Other designations
	V443 Puppis, CD−34°3879, HD 63099, HIP 37876
Database references
SIMBAD	data

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.

WR 9 is a binary with two components in a circular 14-day orbit. The Wolf-Rayet component is often identified as the primary because it dominates the spectrum with its broad emission lines, although it is less massive, less luminous, and less visually bright than its companion. The companion is an approximately O7 star.

The spectrum is dominated by broad emission lines, those of C_IV being the strongest, followed by He_II. C_III lines are seen but much weaker. O_V lines are also stronger than C_III. The classification is usually given as WC4, although it has previously been assigned as WC5. By comparison, the absorption lines of the secondary star are narrower and weaker, although at blue and shorter wavelengths they become stronger than the WR lines. The spectral type of the secondary can be set at O7.^[4] The luminosity class cannot be determined clearly, although it has been suggested to be a supergiant.^[11] The Wolf-Rayet star shows no hydrogen in its spectrum and is thought to be hydrogen-free. It is calculated to consist of 42% helium and 58% heavier elements, mostly carbon and oxygen.^[10]

WR 9 is listed as an eclipsing binary in the General Catalogue of Variable Stars, as well as having the more irregular brightness changes frequently seen in Wolf Rayet stars. The total amplitude is only 0.04 magnitudes.^[6] The eclipses are so shallow because only the atmosphere of the WR star eclipses the O star on each orbit.^[1]

References

^ ^a ^b ^c ^d Lamontagne, Robert; Moffat, Anthony F. J.; Drissen, Laurent; Robert, Carmelle; Matthews, Jaymie M. (1996). "Photometric Determination of Orbital Inclinations and Mass Loss Rates for Wolf-Rayet Stars in WR+O Binaries". Astronomical Journal. 112: 2227. Bibcode:1996AJ....112.2227L. doi:10.1086/118175.
^ ^a ^b ^c ^d ^e 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.
^ ^a ^b ^c 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. Bibcode:2002yCat.2237....0D.
^ ^a ^b Bartzakos, P.; Moffat, A. F. J.; Niemela, V. S. (2001). "Magellanic Cloud WC/WO Wolf-Rayet stars - I. Binary frequency and Roche lobe overflow formation". Monthly Notices of the Royal Astronomical Society. 324 (1): 18–32. Bibcode:2001MNRAS.324...18B. doi:10.1046/j.1365-8711.2001.04126.x.
^ ^a ^b 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.
^ ^a ^b 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.
^ ^a ^b Bartzakos, P.; Moffat, A. F. J.; Niemela, V. S. (2001). "Magellanic Cloud WC/WO Wolf-Rayet stars - II. Colliding winds in binaries". Monthly Notices of the Royal Astronomical Society. 324 (1): 33–50. Bibcode:2001MNRAS.324...33B. doi:10.1046/j.1365-8711.2001.04127.x.
^ Van Der Hucht, Karel A. (2001). "The VIIth catalogue of galactic Wolf-Rayet stars". New Astronomy Reviews. 45 (3): 135–232. Bibcode:2001NewAR..45..135V. doi:10.1016/S1387-6473(00)00112-3.
^ ^a ^b Petrovic, J.; Langer, N.; Van Der Hucht, K. A. (2005). "Constraining the mass transfer in massive binaries through progenitor evolution models of Wolf-Rayet+O binaries". Astronomy and Astrophysics. 435 (3): 1013. arXiv:astro-ph/0504242. Bibcode:2005A&A...435.1013P. doi:10.1051/0004-6361:20042368. S2CID 16778765.
^ ^a ^b ^c Nugis, T.; Lamers, H. J. G. L. M. (2000). "Mass-loss rates of Wolf-Rayet stars as a function of stellar parameters". Astronomy and Astrophysics. 360: 227. Bibcode:2000A&A...360..227N.
^ Niemela, V. S.; Massey, P.; Conti, P. S. (1984). "The WC5 + O7 binary system HD 63099". Astronomical Society of the Pacific. 96: 549. Bibcode:1984PASP...96..549N. doi:10.1086/131377.