Astronomy:WR 24
  WR 24
Credit: ESO | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Carina |
| Right ascension | 10h 43m 52.25894s[1] |
| Declination | –60° 07′ 04.0215″[1] |
| Apparent magnitude (V) | 6.48 - 6.50[2] |
| Characteristics | |
| Spectral type | WN6ha-w[3] |
| U−B color index | –0.91[4] |
| B−V color index | –0.04[4] |
| Variable type | suspected[2] |
| Astrometry | |
| Proper motion (μ) | RA: –6.649[5] mas/yr Dec.: +1.593[5] mas/yr |
| Parallax (π) | 0.2398 ± 0.0344[5] mas |
| Distance | approx. 14,000 ly (approx. 4,200 pc) |
| Absolute magnitude (MV) | –7.34[3] |
| Details[3] | |
| Mass | 114 M☉ |
| Radius | 21.73 R☉ |
| Luminosity (bolometric) | 2,950,000 L☉ |
| Temperature | 50,100 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
WR 24 (HD 93131) is a Wolf-Rayet star in the constellation Carina. It is one of the most luminous stars known. At the edge of naked eye visibility it is also one of the brightest Wolf Rayet stars in the sky.
The spectrum of WR 24 has the characteristic strong nitrogen and helium emission lines of a WN star, but also lines of hydrogen that show Doppler-displaced absorption components. The lowest ionisation nitrogen emission lines are strongest, with NV lines being very weak. The HeI lines are weaker than the HeII lines, leading to a WN6ha spectral class. The spectral type is annotated with a letter w, indicating weaker emission than for a typical WN6 star.[6][3]
WR 24 is thought to be a member of the open cluster Collinder 228, sometimes considered to be just an extension of the rich cluster Trumpler 16. It lies on the southwestern side of the Carina Nebula. Collinder 228 and the Carina Nebula are approximately 2.2 kpc away.[7] However, the Gaia Data Release 2 parallax gives a distance around 4200 for WR 24.[5]
WR 24 has been reported to vary in brightness by about 0.02 magnitudes.[7] Analysis of Hipparcos photometry shows an amplitude of 0.082 magnitudes and a primary period of 4.76 days.[9] It has not yet been assigned a variable star designation in the General Catalogue of Variable Stars and is still formally listed as a suspected variable.[2]
The hydrogen-rich WN stars have been referred to as WNL stars or as WNH stars since they do not necessarily have late nitrogen-sequence spectra. They are systematically more massive and more luminous than stars with similar spectra but lacking nitrogen. WR 24 has a mass of 54 M☉ and is over two million times as luminous as the sun. These stars are proposed to be young hydrogen-burning stars, effectively main sequence objects, rather than post-supergiant stars.[10] WR 24 is calculated to have 44% hydrogen in its atmosphere.[3] The cluster Collinder 228 is thought to be around 6.78 million years old.[7] The WR-type spectra are caused because helium and nitrogen and convected to the surface by the extreme temperature gradients caused by the CNO cycle in the core, and then expelled by powerful stellar winds.[10] WR 24 has a wind reducing its mass by 40×10−6 M☉ per year, at a velocity of 2,160 km/s.[3]
See also
References
- ↑ 1.0 1.1 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 Samus, N. N. 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.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. et al. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics A57: 625. doi:10.1051/0004-6361/201834850. Bibcode: 2019A&A...625A..57H.
- ↑ 4.0 4.1 Turner, D. G.; Moffat, A. F. J. (1980). "Anomalous extinction in the Carina Nebula". Monthly Notices of the Royal Astronomical Society 192 (2): 283. doi:10.1093/mnras/192.2.283. Bibcode: 1980MNRAS.192..283T.
- ↑ 5.0 5.1 5.2 5.3 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ Smith, Lindsey F.; Shara, Michael M.; Moffat, Anthony F. J. (1996). "A three-dimensional classification for WN stars". Monthly Notices of the Royal Astronomical Society 281 (1): 163–191. doi:10.1093/mnras/281.1.163. Bibcode: 1996MNRAS.281..163S.
- ↑ 7.0 7.1 7.2 Zejda, M.; Paunzen, E.; Baumann, B.; Mikulášek, Z.; Liška, J. (2012). "Catalogue of variable stars in open cluster fields". Astronomy & Astrophysics 548: A97. doi:10.1051/0004-6361/201219186. Bibcode: 2012A&A...548A..97Z.
- ↑ "/ftp/cats/more/HIP/cdroms/cats". Strasbourg astronomical Data Center. https://cdsarc.cds.unistra.fr/viz-bin/ftp-index?/ftp/cats/more/HIP/cdroms/cats.
- ↑ Koen, Chris; Eyer, Laurent (2002). "New periodic variables from the Hipparcos epoch photometry". Monthly Notices of the Royal Astronomical Society 331 (1): 45–59. doi:10.1046/j.1365-8711.2002.05150.x. Bibcode: 2002MNRAS.331...45K.
- ↑ 10.0 10.1 Smith, Nathan; Conti, Peter S. (2008). "On the Role of the WNH Phase in the Evolution of Very Massive Stars: Enabling the LBV Instability with Feedback". The Astrophysical Journal 679 (2): 1467–1477. doi:10.1086/586885. Bibcode: 2008ApJ...679.1467S.
External links
- Collinder 228 SEDS.org
 |  |
