| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Dorado |
| Right ascension | 05h 39m 34.302s[1] |
| Declination | −68° 44′ 09.16″[1] |
| Apparent magnitude (V) | 15.204[2] |
| Characteristics | |
| Evolutionary stage | Wolf-Rayet |
| Spectral type | WO3[3] |
| U−B color index | −1.335[2] |
| B−V color index | 0.422[2] |
| Astrometry | |
| Proper motion (μ) | RA: 1.718[1] mas/yr Dec.: 0.876[1] mas/yr |
| Parallax (π) | −0.0198 ± 0.055 mas[1] |
| Distance | 50,000 pc |
| Details | |
| Mass | 7.7[3] M☉ |
| Radius | 0.47[3] R☉ |
| Luminosity | 158,500[3] L☉ |
| Temperature | 170,000[3] K |
| Other designations | |
Brey 93, 2MASS J05393430-6844091 | |
| Database references | |
| SIMBAD | data |
BAT99-123, also known as Brey 93, is a rare WO-type (oxygen sequence) Wolf–Rayet star located in the Large Magellanic Cloud, about 160,000 light years away in Dorado. BAT99-123 was the first WO star discovered in the LMC, and only 3 are known to exist in the galaxy, the other two being LH 41-1042 and LMC195-1.
BAT99-123 was first discovered in 1970, and identified as a star with strong OVI emission in 1971, alongside other WO stars like WR 102, WR 142 and SMC AB8.[4] Most stars with strong OVI emission known at the time were central stars of planetary nebulae.
Properties
[edit]Analysis of BAT99-123's spectrum reveals a surface temperature of 170,000 K. Assuming a distance of 50.12 kpc, or about 163,500 light years, BAT99-123's luminosity is about 158,500 L☉, corresponding to a radius of 0.47 R☉. BAT99-123's strong stellar wind, which has a very high terminal velocity of 3300 km/s, causes it to lose 10-5.14 M☉ (about 7.24×10−6 M☉) a year.[3]
WO-type Wolf-Rayet stars are very very close to the end of their lives. BAT99-123 is predicted to explode in a type Ic supernova in about 7,000 years. By then, it's predicted to have a mass of 7.7 M☉, much lower than its initial mass which was likely a few dozen solar masses.[3] It likely has a similar mass right now as its stellar wind will not change the mass much in this timescale.
References
[edit]- ^ 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 Bonanos, A. Z.; Massa, D. L.; Sewilo, M.; Lennon, D. J.; Panagia, N.; Smith, L. J.; Meixner, M.; Babler, B. L.; Bracker, S.; Meade, M. R.; Gordon, K. D.; Hora, J. L.; Indebetouw, R.; Whitney, B. A. (2009-10-01). "Spitzer SAGE Infrared Photometry of Massive Stars in the Large Magellanic Cloud". The Astronomical Journal. 138 (4): 1003–1021. arXiv:0905.1328. Bibcode:2009AJ....138.1003B. doi:10.1088/0004-6256/138/4/1003. ISSN 0004-6256.
- ^ a b c d e f g 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. (2015-09-01). "Massive stars on the verge of exploding: the properties of oxygen sequence Wolf-Rayet stars". Astronomy and Astrophysics. 581: A110. arXiv:1507.00839. Bibcode:2015A&A...581A.110T. doi:10.1051/0004-6361/201425390. ISSN 0004-6361.
- ^ Sanduleak, N. (1971-03-01). "On Stars Having Strong O VI Emission". The Astrophysical Journal. 164: L71. Bibcode:1971ApJ...164L..71S. doi:10.1086/180694. ISSN 0004-637X.
Well, that’s interesting to know that Psilotum nudum are known as whisk ferns. Psilotum nudum is the commoner species of the two. While the P. flaccidum is a rare species and is found in the tropical islands. Both the species are usually epiphytic in habit and grow upon tree ferns. These species may also be terrestrial and grow in humus or in the crevices of the rocks.
View the detailed Guide of Psilotum nudum: Detailed Study Of Psilotum Nudum (Whisk Fern), Classification, Anatomy, Reproduction