WR 2
| Observation data Epoch 2000 Equinox 2000 | |
|---|---|
| Constellation | Cassiopeia |
| Right ascension | 01h 05m 23.01436s[1] |
| Declination | +60° 25′ 18.9652″[1] |
| Apparent magnitude (V) | 11.33[2] |
| Characteristics | |
| Evolutionary stage | Wolf-Rayet |
| Spectral type | WN2-w[3] |
| B−V color index | +0.16[2] |
| Astrometry | |
| Proper motion (μ) | RA: −12.80[1] mas/yr Dec.: −7.18[1] mas/yr |
| Parallax (π) | 4.46 ± 3.31 mas[1] |
| Distance | 2,510[4] pc |
| Absolute magnitude (MV) | −2.43[3] |
| Details | |
| Mass | 16[3] M☉ |
| Radius | 0.89[3] R☉ |
| Luminosity | 282,000[3] L☉ |
| Temperature | 141,000[3] K |
| Rotational velocity (v sin i) | 500[5] km/s |
| Age | 4.0[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
WR 2 is a Wolf-Rayet star located around 8,000 light years away from Earth in the constellation of Cassiopeia. It is smaller than the sun, but due to a temperature over 140,000 K it is 282,000 times as luminous as the sun.
WR 2 is considered to be a member of the nitrogen sequence of WR stars, but completely lacks lines of NIII, NIV, NV, and HeI. Its spectrum is dominated by broad rounded emission lines of HeII, leading to the classification of WN2-b (for broad).[7] It is now given the spectral type of WN2-w (for weak), due to the relative strength of the continuum and lack of extremely intense emission lines. It is the only galactic WN2 star known.[3] Weak-lined Wolf-Rayet stars often have hot luminous companions which dilute the emission. WR 2 does have a companion, but it is much fainter than the primary and not thought to be the cause of the weak-lined spectrum.[5]
WR 2 is the smallest and hottest WN star known in the galaxy. Its unusual rounded emission lines are thought to be due to extremely fast rotation, although the exact rotation rate is not known. Estimates range from 500 km/s to approximately the breakup rate for the star of 1,900 km/s.[8][3][5] The high temperature also leads to a very fast stellar wind of 1,800 km/s,[3] although the overall rate of mass loss is one of the lowest for any Wolf-Rayet star.[9] The combination of a massive Wolf-Rayet star and rapid rotation is likely to result in a gamma-ray burst when the star explodes as a supernova.[8]
X-rays have been detected from WR 2 although they may not be due to colliding winds as is common for massive stars.[9]
References
- ^ a b c d e 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.
- ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H.
- ^ a b c d e f g h i Hamann, W. -R.; Gräfener, G.; Liermann, A. (2006). "The Galactic WN stars". Astronomy and Astrophysics. 457 (3): 1015. arXiv:astro-ph/0608078. Bibcode:2006A&A...457.1015H. doi:10.1051/0004-6361:20065052.
- ^ Van Der Hucht, K. A. (2001). "The VIIth catalogue of galactic Wolf–Rayet stars". New Astronomy Reviews. 45 (3): 135. Bibcode:2001NewAR..45..135V. doi:10.1016/S1387-6473(00)00112-3.
- ^ a b c Shenar, T.; Hamann, W.-R.; Todt, H. (2014). "The impact of rotation on the line profiles of Wolf-Rayet stars". Astronomy & Astrophysics. 562: A118. arXiv:1401.2159. Bibcode:2014A&A...562A.118S. doi:10.1051/0004-6361/201322496.
- ^ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410: 190. arXiv:1007.4883. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ Hiltner, W. A.; Schild, R. E. (1966). "Spectral Classification of Wolf-Rayet Stars". Astrophysical Journal. 143: 770. Bibcode:1966ApJ...143..770H. doi:10.1086/148556.
- ^ a b Sander, A.; Hamann, W.-R.; Todt, H. (2012). "The Galactic WC stars. Stellar parameters from spectral analyses indicate a new evolutionary sequence" (PDF). Astronomy & Astrophysics. 540: A144. arXiv:1201.6354. Bibcode:2012A&A...540A.144S. doi:10.1051/0004-6361/201117830.
- ^ a b Skinner, Stephen L.; Zhekov, Svetozar A.; Güdel, Manuel; Schmutz, Werner; Sokal, Kimberly R. (2012). "New X-Ray Detections of WNL Stars". The Astronomical Journal. 143 (5): 116. arXiv:1203.5098. Bibcode:2012AJ....143..116S. doi:10.1088/0004-6256/143/5/116.
