LH 41-1042
 The N119 HII regions. LH41-1042 and LMC195-1 are both in the central core of the dense cluster to the right of centre. Credit: ESO | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Dorado |
| Right ascension | +05h 18m 11.01s[1] |
| Declination | −69° 13′ 11.3″[1] |
| Apparent magnitude (V) | 13.95[2] |
| Characteristics | |
| Spectral type | WO4[2] |
| U−B color index | −1.38[2] |
| B−V color index | +0.31[2] |
| Astrometry | |
| Distance | 160,000 ly (49,000 pc) |
| Details[3] | |
| Mass | 8.4 M☉ |
| Radius | 0.62 R☉ |
| Luminosity | 182,000 L☉ |
| Temperature | 150,000 K |
| Other designations | |
LH 41-1042 | |
| Database references | |
| SIMBAD | data |
LH41-1042 is a Wolf-Rayet star located in the Large Magellanic Cloud (LMC). It is an extremely rare member of the WO oxygen sequence, the second to be discovered in the LMC and one of only three found so far.
The star was identified in 2012 during an investigation of the LH41 stellar association, also known as NGC 1910, using one of the 6.5m Magellan Telescopes at Las Campanas Observatory in Chile.[2]
LH 41-1042 is located in the rich LH 41 (NGC 1910) stellar association that contains two luminous blue variables, S Doradus and R85, the WN5 star BAT99-27, and another WO star LMC195-1.[4] The two WO stars are only 9" apart. WO stars are classified on the basis of OVI emission at 381.1-383.4 nm, which is weak or absent in other Wolf Rayet stars. The WO4 subclass is defined as having the ratio of OVI to OV emission strength between 0.5 and 1.8.[5] In the new star, the ratio of these line strengths was 0.7.[2]
The high temperature and high luminosity of LH 41-1042 produce a stellar wind travelling at 3,500 km/s and it is losing mass about a billion times more quickly than the sun. It is estimated that it has exhausted its core helium and only has 9,000 years left before it explodes as a type Ic supernova.[3]
References
- ^ a b Massey, Philip; Waterhouse, Elizabeth; Degioia-Eastwood, Kathleen (2000). "The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. I. Results from 19 OB Associations in the Magellanic Clouds". The Astronomical Journal. 119 (5): 2214. arXiv:astro-ph/0002233. Bibcode:2000AJ....119.2214M. doi:10.1086/301345.
- ^ a b c d e f Neugent, Kathryn F.; Massey, Philip; Morrell, Nidia (2012). "The Discovery of a Rare WO-type Wolf-Rayet Star in the Large Magellanic Cloud". The Astronomical Journal. 144 (6): 162. arXiv:1210.0062. Bibcode:2012AJ....144..162N. doi:10.1088/0004-6256/144/6/162.
- ^ a b Tramper, F.; Straal, S. M.; Sanyal, D.; Sana, H.; De Koter, A.; Gräfener, G.; Langer, N.; Vink, J. S.; De Mink, S. E.; Kaper, L. (2015). "Massive stars on the verge of exploding: The properties of oxygen sequence Wolf-Rayet stars". Astronomy & Astrophysics. 581: A110. arXiv:1507.00839. Bibcode:2015A&A...581A.110T. doi:10.1051/0004-6361/201425390.
- ^ Massey, Philip; Neugent, Kathryn F.; Morrell, Nidia; Hillier, D. John (2014). "A Modern Search for Wolf-Rayet Stars in the Magellanic Clouds: First Results". The Astrophysical Journal. 788: 83. arXiv:1404.7441. Bibcode:2014ApJ...788...83M. doi:10.1088/0004-637X/788/1/83.
- ^ Crowther, P. A.; De Marco, Orsola; Barlow, M. J. (1998). "Quantitative classification of WC and WO stars". Monthly Notices of the Royal Astronomical Society. 296 (2): 367. Bibcode:1998MNRAS.296..367C. doi:10.1046/j.1365-8711.1998.01360.x.
