HD 269810

Last updated
HD 269810
HD 269810.png
An image from the Two Micron All-Sky Survey. HD 269810 is the upper left of the pair of bright stars to the upper right of the nebulosity.
Observation data
Epoch J2000       Equinox J2000
Constellation Dorado
Right ascension 05h 35m 13.90s [1]
Declination −67° 33′ 27.5″ [1]
Apparent magnitude  (V)12.22 [2]
Characteristics
Spectral type O2III(f*) [3]
B−V color index −0.14 [2]
Astrometry
Radial velocity (Rv)303 [4]  km/s
Proper motion (μ)RA: +1.801 [1]   mas/yr
Dec.: +0.677 [1]   mas/yr
Parallax (π)−0.0098 ± 0.0310  mas [1]
Absolute magnitude  (MV)−6.6 [3]
Details
Mass 130 [3]   M☉
Radius 18 [5]   R☉
Luminosity 2.2 million [3]   L☉
Surface gravity (log g)4.0 [3]   cgs
Temperature 52,500 [3]   K
Metallicity ≤0.1 [3] He/H
Rotation 173 [6]
Other designations
GCRV 24403, RMC 122, UBV 5767, ARDB C54, SK −67° 211, UCAC2 2218036, ARDB 317, GSC 09162-00101, TYC 9162-101-1, CSI−67-05351, 2MASS J05351389-6733275, UBV M 28781
Database references
SIMBAD data

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.

Contents

Name

The star's name, HD 269810, comes from the Henry Draper Catalogue. The serial number 269810 indicates it was published in the extension of the catalogue and is formally referred to as HDE 269810.

Details

HD 269810 is classified as an O2 III (f*) star with a temperature of 52,500  K (52,200 °C; 94,000 °F). The luminosity class of III indicates a star somewhat evolved and expanded compared to the zero-age main sequence. The spectral peculiarity code (f*) indicates strong NIII emission lines, even stronger NNIV emission, and weak HeNII emission. The star's radius is 18  R☉, but because of its high surface temperature it is two million times brighter than the Sun. The high temperature generates a fast stellar wind of 3,750 km/s (2,330 mi/s), [7] shedding over a millionth of the mass of the sun each year. [3] In 1995, HD 269810 was estimated to be 190 times the mass of the Sun [8] and was thought to be the heaviest star known, but its mass estimate is now revised down to be around 130  M☉. [3]

Evolution

Stars as massive as HD 269810 with metallicity typical of the Large Magellanic Cloud will maintain near-homogeneous chemical structure due to strong convection and rotational mixing. This produces strong helium and nitrogen surface abundance enhancement even during core hydrogen burning. Their rotation rates will also decrease significantly due to mass loss and envelope inflation, so that gamma-ray bursts are unlikely when this type of star reaches core collapse. They are expected to develop directly into Wolf–Rayet stars, passing through WN, WC, and WO stages before exploding as a type Ic supernova and leaving behind a black hole. The total lifetime would be around 2 million years, showing an O-type spectrum for most of that time before a shorter period with a WR spectrum. [9] [10]

Related Research Articles

<span class="mw-page-title-main">Wolf–Rayet star</span> Heterogeneous class of stars with unusual spectra

Wolf–Rayet stars, often abbreviated as WR stars, are a rare heterogeneous set of stars with unusual spectra showing prominent broad emission lines of ionised helium and highly ionised nitrogen or carbon. The spectra indicate very high surface enhancement of heavy elements, depletion of hydrogen, and strong stellar winds. The surface temperatures of known Wolf–Rayet stars range from 20,000 K to around 210,000 K, hotter than almost all other kinds of stars. They were previously called W-type stars referring to their spectral classification.

<span class="mw-page-title-main">Tarantula Nebula</span> H II region in the constellation Dorado

The Tarantula Nebula is a large H II region in the Large Magellanic Cloud (LMC), forming its south-east corner.

<span class="mw-page-title-main">NGC 3603</span> Open cluster in the constellation Carina

NGC 3603 is a nebula situated in the Carina–Sagittarius Arm of the Milky Way around 20,000 light-years away from the Solar System. It is a massive H II region containing a very compact open cluster HD 97950.

<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">NGC 346</span> Open cluster in the constellation Tucana

NGC 346 is a young open cluster of stars with associated nebula located in the Small Magellanic Cloud (SMC) that appears in the southern constellation of Tucana. It was discovered August 1, 1826 by Scottish astronomer James Dunlop. J. L. E. Dreyer described it as, "bright, large, very irregular figure, much brighter middle similar to double star, mottled but not resolved". On the outskirts of the cluster is the multiple star system HD 5980, one of the brightest stars in the SMC.

<span class="mw-page-title-main">HD 93205</span> Star system in the constellation Carina

HD 93205, or V560 Carinae, is a binary stellar system, in the Carina Nebula in the constellation Carina. It consists of two massive O-stars that revolve around each other in 6 days.

<span class="mw-page-title-main">HD 37974</span> Star in the constellation Dorado

HD 37974 a variable B[e] hypergiant in the Large Magellanic Cloud. It is surrounded by an unexpected dust disk.

<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.

15 Sagittarii is a blue-hued binary star system in the southern zodiac constellation of Sagittarius. The estimated distance based upon photometry is around 4,200 ly (1,300 pc). It is faintly visible to the naked eye with an apparent visual magnitude of 5.37. The system is moving closer to the Sun with a heliocentric radial velocity of around −6 km/s.

<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">WR 25</span> Binary star system in the constellation Carina

WR 25 is a binary star system in the turbulent star-forming region the Carina Nebula, about 6,800 light-years from Earth. It contains a Wolf-Rayet star and a hot luminous companion and is a member of the Trumpler 16 cluster. The name comes from the Catalogue of Galactic Wolf–Rayet Stars.

HD 38282 is a massive spectroscopic binary star in the Tarantula Nebula, consisting of two hydrogen-rich Wolf-Rayet stars.

<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.

R99 is a star in the Large Magellanic Cloud in the constellation Dorado. It is classified as a possible luminous blue variable and is one of the most luminous stars known.

<span class="mw-page-title-main">HD 316285</span> Star in the constellation Sagittarius

HDE 316285 is a blue supergiant star in the constellation Sagittarius. It is a candidate luminous blue variable and lies about 6,000 light years away in the direction of the galactic centre.

<span class="mw-page-title-main">HD 15558</span> Star in the constellation Cassiopeia

HD 15558 is a massive O-type multiple star system in Cassiopeia and is specifically in our galaxy's Heart Nebula in open cluster IC 1805. The primary is a very massive star with 152 M☉ and 660,000 L☉.

<span class="mw-page-title-main">HD 73882</span> Eclipsing binary system in constellation Vela

HD 73882 is a visual binary system with the components separated by 0.6″ and a combined spectral class of O8. One of stars is an eclipsing binary system. The period of variability is listed as both 2.9199 days and 20.6 days, possibly due to the secondary being a spectroscopic binary star.

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.; et al. (February 2013). "The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)". The Astronomical Journal. 145 (2): 44. arXiv: 1212.6182 . Bibcode:2013AJ....145...44Z. doi:10.1088/0004-6256/145/2/44. S2CID   119299381.
    Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; et al. (July 2012). "VizieR On-line Data Catalog: UCAC4 Catalogue". VizieR On-line Data Catalog: I/322A. 1322. Bibcode:2012yCat.1322....0Z.
  3. 1 2 3 4 5 6 7 8 9 Evans, C. J.; Walborn, N. R.; Crowther, P. A.; Hénault-Brunet, V.; Massa, D.; et al. (June 2010). "A Massive Runaway Star from 30 Doradus". The Astrophysical Journal Letters. 715 (2): L74–L79. arXiv: 1004.5402 . Bibcode:2010ApJ...715L..74E. doi:10.1088/2041-8205/715/2/L74. S2CID   118498849.
  4. ↑ Ardeberg, A.; Brunet, J. P.; Maurice, E.; Prevot, L. (July 1972). "Spectrographic and photometric observations of supergiants and foreground stars in the direction of the Large Magellanic Cloud". Astronomy and Astrophysics Supplement Series. 6: 249. Bibcode:1972A&AS....6..249A.
  5. ↑ Walborn, N. R.; Morrell, N. I.; Howarth, I. D.; Crowther, P. A.; Lennon, D. J.; et al. (June 2004). "A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds". The Astrophysical Journal. 608 (2): 1028–1038. arXiv: astro-ph/0403557 . Bibcode:2004ApJ...608.1028W. doi:10.1086/420761. S2CID   16656083.
  6. ↑ Penny, L. R.; Sprague, A. J.; Seago, G.; Gies, D. R. (December 2004). "Effects of Metallicity on the Rotational Velocities of Massive Stars". The Astrophysical Journal. 617 (2): 1316–1322. arXiv: astro-ph/0409757 . Bibcode:2004ApJ...617.1316P. doi:10.1086/425573. S2CID   14026671.
  7. ↑ Howk, J.C.; Sembach, K.R.; Savage, B.D.; Massa, D.; Friedman, S.D.; Fullerton, A.W. (April 2002). "The global content, distribution, and kinematics of interstellar OVI in the Large Magellanic Cloud". The Astrophysical Journal . 569 (1): 214–232. arXiv: astro-ph/0111566 . Bibcode:2002ApJ...569..214H. doi:10.1086/339322. S2CID   9421429.
  8. ↑ Walborn, N.R.; Long, K.S.; Lennon, D.J.; Kudritzki, R.P. (November 1995). "A reconnaissance of the 900–1200 Å spectra of early O stars in the Magellanic Clouds". The Astrophysical Journal Letters . 454: L27. Bibcode:1995ApJ...454L..27W. doi: 10.1086/309768 . S2CID   121642113.
  9. ↑ Yusof, N.; Hirschi, R.; Meynet, G.; Crowther, P. A.; Ekstrom, S.; et al. (August 2013). "Evolution and fate of very massive stars". Monthly Notices of the Royal Astronomical Society. 433 (2): 1114–1132. arXiv: 1305.2099 . Bibcode:2013MNRAS.433.1114Y. doi:10.1093/mnras/stt794. S2CID   26170005.
  10. ↑ Köhler, K.; Langer, N.; De Koter, A.; De Mink, S. E.; Crowther, P. A.; et al. (January 2015). "The evolution of rotating very massive stars with LMC composition". Astronomy & Astrophysics. 573: A71. arXiv: 1501.03794 . Bibcode:2015A&A...573A..71K. doi:10.1051/0004-6361/201424356. S2CID   28962151.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.