HD 38282

Last updated
HD 38282
Observation data
Epoch J2000       Equinox J2000
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  mas [1]
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
Brey 89, BAT99 118, RMC 144, R144, CPD−69°462, 2MASS  J05385338-6902007, HD  38282, GSC 09163-00992,
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

Related Research Articles

<span class="mw-page-title-main">R136</span> Super star cluster in the constellation Dorado, in the Large Magellanic Cloud

R136 is the central concentration of stars in the NGC 2070 star cluster, which lies at the centre of the Tarantula Nebula in the Large Magellanic Cloud. When originally named it was an unresolved stellar object but is now known to include 72 class O and Wolf–Rayet stars within 5 parsecs of the centre of the cluster. The extreme number and concentration of young massive stars in this part of the LMC qualifies it as a starburst region.

<span class="mw-page-title-main">R136b</span> Star in the constellation Dorado

R136b is a Wolf–Rayet star in the R136 cluster in the Large Magellanic Cloud. It is one of the most massive and most luminous stars known. It is found in the dense R136 open cluster at the centre of NGC 2070 in the Tarantula Nebula.

<span class="mw-page-title-main">WR 7</span> Star in the constellation Canis Major

WR 7 is a Wolf–Rayet star in the constellation of Canis Major. It lies at the centre of a complex bubble of gas which is shocked and partially ionised by the star's radiation and winds.

<span class="mw-page-title-main">HD 97950</span> Multiple star system in the constellation Carina

HD 97950, is a multiple star system and part of a super star cluster within the NGC 3603 H II region. It was catalogued as a single star although it was always known to be a compact cluster. It is now resolved into a massive multiple star at the centre of one of the densest clusters in the galaxy.

<span class="mw-page-title-main">HD 269810</span> Star in the constellation Dorado

HD 269810 is a blue giant star in the Large Magellanic Cloud. It is one of the most massive and most luminous stars known, and one of only a handful of stars with the spectral type O2.

<span class="mw-page-title-main">R136a1</span> Wolf–Rayet star with one of the highest mass and luminosity of any known star

R136a1 is one of the most massive and luminous stars known, at 196 M☉ and nearly 4.7 million L☉, and is also one of the hottest, at around 46,000 K. It is a Wolf–Rayet star at the center of R136, the central concentration of stars of the large NGC 2070 open cluster in the Tarantula Nebula in the Large Magellanic Cloud. The cluster can be seen in the far southern celestial hemisphere with binoculars or a small telescope, at magnitude 7.25. R136a1 itself is 100 times fainter than the cluster and can only be resolved using speckle interferometry.

<span class="mw-page-title-main">Melnick 42</span> Massive blue supergiant star in the constellation Dorado

Melnick 42 is a massive blue supergiant star in the Tarantula Nebula in the Large Magellanic Cloud located in the constellation Dorado. Although it is only 21 times the size of the sun, its high temperature of 47,300 K makes it one of the most luminous stars of the Tarantula Nebula at 3,600,000 L☉. It is less than two parsecs from the centre of the R136 cluster, although that is well outside the central core.

<span class="mw-page-title-main">VFTS 682</span> Wolf Rayet star in the constellation Dorado

VFTS 682 is a Wolf–Rayet star in the Large Magellanic Cloud. It is located over 29 parsecs (95 ly) north-east of the massive cluster R136 in the Tarantula Nebula. It is 138 times the mass of the sun and 3.2 million times more luminous which makes it one of the most massive and most luminous stars known.

<span class="mw-page-title-main">R136a2</span> Star in the constellation Dorado

R136a2 is a Wolf-Rayet star residing near the center of the R136, the central concentration of stars of the large NGC 2070 open cluster in the Tarantula Nebula, a massive H II region in the Large Magellanic Cloud which is a nearby satellite galaxy of the Milky Way. It has one of the highest confirmed masses and luminosities of any known star, at about 151 M☉ and 3.5 million L☉ respectively.

<span class="mw-page-title-main">R136c</span> Star in the constellation Dorado

R136c is a star located in R136, a tight knot of stars at the centre of NGC 2070, an open cluster weighing 450,000 solar masses and containing 10,000 stars. At 142 M☉ and 3.8 million L☉, it is the one of the most massive stars known and one of the most luminous, along with being one of the hottest, at over 40,000 K. It was first resolved and named by Feitzinger in 1980, along with R136a and R136b.

<span class="mw-page-title-main">R136a3</span> Star in the constellation Dorado

R136a3 is a Wolf–Rayet star in R136, a massive star cluster located in Dorado. It is located near R136a1, the most massive and luminous star known. R136a3 is itself one of the most massive and most luminous stars known at about 179 times more massive and 5 million times more luminous than the Sun.

<span class="mw-page-title-main">BI 253</span> O-type main sequence star in the constellation Dorado

BI 253 is an O2V star in the Large Magellanic Cloud and is a primary standard of the O2 type. It is one of the hottest main-sequence stars known and one of the most-massive and most-luminous stars known.

WR 142 is a Wolf-Rayet star in the constellation Cygnus, an extremely rare star on the WO oxygen sequence. It is a luminous and very hot star, highly evolved and close to exploding as a supernova. It is suspected to be a binary star with a companion orbiting about 1 AU away.

<span class="mw-page-title-main">Melnick 34</span> Binary star in the Large Magellanic cloud

Melnick 34, also called BAT99-116, is a binary Wolf–Rayet star near R136 in the 30 Doradus complex in the Large Magellanic Cloud. Both components are amongst the most massive and most luminous stars known, and the system is the most massive known binary system.

BAT99-98 is a star in the Large Magellanic Cloud. It is located near the R136 cluster in the 30 Doradus nebula. At 226 M☉ and 5,000,000 L☉ it is one of the most massive and luminous stars known.

<span class="mw-page-title-main">WR 120</span> Binary star system in the constellation Scutum

WR 120 is a binary containing two Wolf-Rayet stars in the constellation of Scutum, around 10,000 light years away. The primary is a hydrogen-free weak-lined WN7 star, the secondary is a hydrogen-free WN3 or 4 star, and the system is a possible member of the cluster Dolidze 33. From our point of view, WR 120 is reddened by 4.82 magnitudes, and it has the variable designation of V462 Scuti.

BAT99-7 is a WN-type Wolf-Rayet star located in the Large Magellanic Cloud, in the constellation of Dorado, about 160,000 light years away. The star has a spectrum containing extremely broad emission lines, and is the prototype for the "round line" stars, Wolf-Rayet stars whose spectra are characterized by strong and broad emission lines with round line profiles. The broad emission lines hint at an extremely high temperature of nearly 160,000 Kelvin, which would make it the hottest of all WN stars with known temperatures, as well as an extraordinarily large mass loss rate for a Wolf-Rayet star in the LMC, at 10−4.48 M☉/yr, which means that every 30,200 years, the star loses 1 solar mass worth of mass.

References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  2. 1 2 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. 1 2 3 4 5 6 7 Sana, H.; Van Boeckel, T.; Tramper, F.; Ellerbroek, L. E.; De Koter, A.; Kaper, L.; Moffat, A. F. J.; Schnurr, O.; Schneider, F. R. N.; Gies, D. R. (2013). "R144 revealed as a double-lined spectroscopic binary". Monthly Notices of the Royal Astronomical Society: Letters. 432: 26. arXiv: 1304.4591 . Bibcode:2013MNRAS.432L..26S. doi:10.1093/mnrasl/slt029. S2CID   119238483.
  4. ↑ Roman-Duval, Julia; Jenkins, Edward B.; Tchernyshyov, Kirill; Williams, Benjamin; Clark, Christopher J. R.; Gordon, Karl D.; Meixner, Margaret; Hagen, Lea; Peek, Joshua; Sandstrom, Karin; Werk, Jessica; Yanchulova Merica-Jones, Petia (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. arXiv: 2101.09399 . doi:10.3847/1538-4357/abdeb6. S2CID   234355905.
  5. ↑ Pietrzyński, G; D. Graczyk; W. Gieren; I. B. Thompson; B. Pilecki; A. Udalski; I. Soszyński; et al. (7 March 2013). "An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent". Nature. 495 (7439): 76–79. arXiv: 1303.2063 . Bibcode:2013Natur.495...76P. doi:10.1038/nature11878. PMID   23467166. S2CID   4417699.
  6. 1 2 3 4 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].
  7. ↑ 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. arXiv: 1311.2934 . Bibcode:2014MNRAS.437.4000O. doi:10.1093/mnras/stt2219. S2CID   118708404.
  8. ↑ Van Gelder, M. L.; Kaper, L.; Japelj, J.; Ramírez-Tannus, M. C.; Ellerbroek, L. E.; Barbá, R. H.; Bestenlehner, J. M.; Bik, A.; Gräfener, G.; De Koter, A.; De Mink, S. E.; Sabbi, E.; Sana, H.; Sewiło, M.; Vink, J. S.; Walborn, N. R. (2020), "VLT/X-shooter spectroscopy of massive young stellar objects in the 30 Doradus region of the Large Magellanic Cloud", Astronomy & Astrophysics, 636: A54, arXiv: 2002.02690 , doi:10.1051/0004-6361/201936361, S2CID   211066451
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