Astronomy:HD 38282
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Dorado |
| Right ascension | 05h 38m 53.3783s[1] |
| Declination | −69° 02′ 00.896″[1] |
| Apparent magnitude (V) | 11.11[2] |
| Characteristics | |
| Evolutionary stage | Wolf Rayet |
| Spectral type | WN5-6h + WN6-7h[3] |
| B−V color index | −0.13[2] |
| Astrometry | |
| Radial velocity (Rv) | 267.5±52.5[4] km/s |
| Proper motion (μ) | RA: 2.033[1] mas/yr Dec.: 0.926[1] mas/yr |
| Parallax (π) | 0.0107 ± 0.0226[1] mas |
| Distance | 163,000 ly (49,970[5] pc) |
| Absolute magnitude (MV) | −7.96[6] |
| Details | |
| Mass | 80-170 + 95-205[3] M☉ |
| Luminosity | 4,500,000[6] – 6,300,000[3] L☉ |
| Temperature | 47,000[6] K |
| Age | <2[3] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 38282 (R144, BAT99-118, Brey 89) is a massive spectroscopic binary star in the Tarantula Nebula (Large Magellanic Cloud), consisting of two hydrogen-rich Wolf-Rayet stars.
R144 is located near the R136 cluster at the center of NGC 2070 and may have been ejected from it after an encounter with another massive binary.[7] It shares a common X-ray cavity with the R146 (HD 269926) and R147 (HD 38344) Wolf-Rayet star systems.[8]
Both components of R144 are detected in the spectrum and both are WNh stars, very hot stars with strong emission lines due to their strong stellar winds. The orbit has not been determined, but is likely to be between two and six months long, possibly more if it is eccentric. The primary, slightly hotter, star is observed to be the less massive of the two.[3]
Each star is amongst the most luminous known, but the exact parameters of each has not been determined. Their combined luminosity is around 4,500,000 L☉[6] to 6,300,000 L☉.[3] The masses have not yet been calculated accurately from the orbital parameters, but the stars have been modelled to initially have been around 260 M☉ and 175 M☉. Depending on their exact age, this has now decreased to between 90 M☉ and 170 M☉ for the primary and 95 M☉ and 205 M☉ for the secondary.[3]
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)". VizieR On-line Data Catalog: I/322A. Originally Published in: 2012yCat.1322....0Z; 2013AJ....145...44Z 1322. Bibcode: 2012yCat.1322....0Z.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Sana, H.; Van Boeckel, T.; Tramper, F.; Ellerbroek, L. E.; De Koter, A.; Kaper, L.; Moffat, A. F. J.; Schnurr, O. et al. (2013). "R144 revealed as a double-lined spectroscopic binary". Monthly Notices of the Royal Astronomical Society: Letters 432: 26. doi:10.1093/mnrasl/slt029. Bibcode: 2013MNRAS.432L..26S.
- ↑ Roman-Duval, Julia; Jenkins, Edward B.; Tchernyshyov, Kirill; Williams, Benjamin; Clark, Christopher J. R.; Gordon, Karl D.; Meixner, Margaret; Hagen, Lea et al. (2021). "METAL: The Metal Evolution, Transport, and Abundance in the Large Magellanic Cloud Hubble Program. II. Variations of Interstellar Depletions and Dust-to-gas Ratio within the LMC". The Astrophysical Journal 910 (2): 95. doi:10.3847/1538-4357/abdeb6. Bibcode: 2021ApJ...910...95R.
- ↑ Pietrzyński, G et al. (7 March 2013). "An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent". Nature 495 (7439): 76–79. doi:10.1038/nature11878. PMID 23467166. Bibcode: 2013Natur.495...76P.
- ↑ 6.0 6.1 6.2 6.3 Hainich, R.; Rühling, U.; Todt, H.; Oskinova, L. M.; Liermann, A.; Gräfener, G.; Foellmi, C.; Schnurr, O.; Hamann, W. -R. (2014). "The Wolf-Rayet stars in the Large Magellanic Cloud: A comprehensive analysis of the WN class". arXiv:1401.5474v1 [astro-ph.SR].
- ↑ Oh, Seungkyung; Kroupa, Pavel; Banerjee, Sambaran (2014). "R144: A very massive binary likely ejected from R136 through a binary-binary encounter". Monthly Notices of the Royal Astronomical Society 437 (4): 4000. doi:10.1093/mnras/stt2219. Bibcode: 2014MNRAS.437.4000O.
- ↑ Van Gelder, M. L.; Kaper, L.; Japelj, J.; Ramírez-Tannus, M. C.; Ellerbroek, L. E.; Barbá, R. H.; Bestenlehner, J. M.; Bik, A. et al. (2020), "VLT/X-shooter spectroscopy of massive young stellar objects in the 30 Doradus region of the Large Magellanic Cloud", Astronomy & Astrophysics 636: A54, doi:10.1051/0004-6361/201936361, Bibcode: 2020A&A...636A..54V
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