WR 22
WR 22, also known as V429 Carinae or HR 4188, is an eclipsing binary star system in the constellation Carina. The system contains a Wolf-Rayet (WR) star that is one of the most massive and most luminous stars known, and is also a bright x-ray source due to colliding winds with a less massive O class companion.
System
The WR 22 system contains two massive stars which orbit every 80 days. The spectrum and luminosity are dominated by the primary, which has a spectral type of WN7h, indicating that it is a WR star on the nitrogen sequence, but also with hydrogen lines in its spectrum. The secondary is an O9 star which appears to have the spectral luminosity class of a giant star, but the brightness of a main sequence star.[5]
There is a shallow eclipse detectable when the primary passes in front of the secondary, which would be classed as the secondary eclipse. However, no primary eclipse is detected, which is believed to be due to the eccentricity of the system placing the stars further apart when the primary eclipse would occur. The separation of the stars varies from over 500 R☉ to less than 150 R☉. This strongly constrains the possible inclinations of the system.[8]
Properties
The masses of the two stars can be determined fairly accurately because WR 22 is an eclipsing binary. It is one of the most massive star systems measured in this way rather than by assumptions about stellar evolution. Despite this, the dynamical masses derived from orbital fitting vary from over 70 M☉ to less than 60 M☉ for the primary and about 21 - 27 M☉ for the secondary.[9] The spectroscopic mass of the primary has been calculated at 74 M☉[11] or 78.1 M☉.[8]
The temperature of both stars is high, but somewhat poorly defined. The Wolf Rayet primary has a temperature of approximately 44,700 K derived from a model atmosphere fitting of the spectrum, and the secondary is assumed to have a temperature of 33,000 K which is typical for a star of its spectral type.[10]
The brightness of the two stars cannot be measured separately, but the luminosity ratio can be calculated. The total system absolute magnitude, for a distance of 2.7 kpc and extinction of 1.12 magnitudes, is −6.85.[5] The luminosities calculated for a similar distance are two million L☉ and 130,000 L☉.[8]
Evolution
High mass hydrogen-rich WR stars are young stars still burning hydrogen in their cores, rather than evolved stars fusing heavier elements. They show the WR characteristics of strong helium and nitrogen emission because they are strongly convective all the way to the core and have dredged up fusion products to the surface. About two million years ago, WR22 would have been an even hotter O type main sequence star with a mass of around 120 M☉. It will soon exhaust the hydrogen in its core and evolve into a classical hydrogen-poor WR star, possibly after a period as a Luminous Blue Variable then explode as a supernova. The secondary star is expected to have a more traditional evolution into a red supergiant in a few million years time.[8]
References
- 1 2 3 4 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752
. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. - 1 2 3 4 5 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.
- ↑ Gagné, M.; Fehon, G.; Savoy, M. R.; Cartagena, C. A.; Cohen, D. H.; Owocki, S. P. (2012). "An X-Ray Survey of Colliding Wind Binaries". Proceedings of a Scientific Meeting in Honor of Anthony F. J. Moffat held at Auberge du Lac Taureau. 465: 301. arXiv:1205.3510. Bibcode:2012ASPC..465..301G.
- 1 2 3 4 5 Cutri, R. M.; Skrutskie, M. F.; Van Dyk, S.; Beichman, C. A.; Carpenter, J. M.; Chester, T.; Cambresy, L.; Evans, T.; Fowler, J.; Gizis, J.; Howard, E.; Huchra, J.; Jarrett, T.; Kopan, E. L.; Kirkpatrick, J. D.; Light, R. M.; Marsh, K. A.; McCallon, H.; Schneider, S.; Stiening, R.; Sykes, M.; Weinberg, M.; Wheaton, W. A.; Wheelock, S.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". VizieR On-line Data Catalog: II/246. Originally published in: 2003yCat.2246....0C. 2246. Bibcode:2003yCat.2246....0C.
- 1 2 3 4 5 Gosset, E.; Nazé, Y.; Sana, H.; Rauw, G.; Vreux, J.-M. (2009). "Phase-resolved XMM-Newton observations of the massive WR+O binary WR 22". Astronomy and Astrophysics. 508 (2): 805. Bibcode:2009A&A...508..805G. doi:10.1051/0004-6361/20077981.
- ↑ Kharchenko, N. V.; Scholz, R.-D.; Piskunov, A. E.; Röser, S.; Schilbach, E. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ˜55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv:0705.0878. Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776.
- ↑ Gaia Collaboration (2016). "VizieR Online Data Catalog: Gaia DR1 (Gaia Collaboration, 2016)". VizieR On-line Data Catalog: I/337. Originally published in: Astron. Astrophys. 1337. Bibcode:2016yCat.1337....0G.
- 1 2 3 4 5 6 7 8 9 10 11 Gräfener, G.; Hamann, W.-R. (2008). "Mass loss from late-type WN stars and its Z-dependence. Very massive stars approaching the Eddington limit". Astronomy and Astrophysics. 482 (3): 945. arXiv:0803.0866. Bibcode:2008A&A...482..945G. doi:10.1051/0004-6361:20066176.
- 1 2 Schweickhardt, J.; Schmutz, W.; Stahl, O.; Szeifert, Th.; Wolf, B. (1999). "Revised mass determination of the super massive Wolf-Rayet star WR 22". Astronomy and Astrophysics. 347: 127. Bibcode:1999A&A...347..127S.
- 1 2 3 4 5 Parkin, E. R.; Gosset, E. (2011). "Investigating the X-ray emission from the massive WR+O binary WR 22 using 3D hydrodynamical models". Astronomy & Astrophysics. 530: A119. arXiv:1104.2383. Bibcode:2011A&A...530A.119P. doi:10.1051/0004-6361/201016125.
- ↑ Hamann, W.-R.; Gräfener, G.; Liermann, A. (2006). "The Galactic WN stars. Spectral analyses with line-blanketed model atmospheres versus stellar evolution models with and without rotation". Astronomy and Astrophysics. 457 (3): 1015. arXiv:astro-ph/0608078. Bibcode:2006A&A...457.1015H. doi:10.1051/0004-6361:20065052.