HD 152408

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HD 152408
Scorpius constellation map.svg
Red circle.svg
Location of WR 79a (circled)
Observation data
Epoch J2000        Equinox J2000
Constellation Scorpius
Right ascension 16h 54m 58.5049s [1]
Declination −41° 09′ 03.092″ [1]
Apparent magnitude  (V)5.81-5.85 [2]
Characteristics
Spectral type WN9ha [3]
U−B color index −0.8 [4]
B−V color index 0.017 [4]
Variable type WR [2]
Astrometry
Radial velocity (Rv)−138 [5]  km/s
Proper motion (μ)RA: 0.47 [1]   mas/yr
Dec.: −2.25 [1]   mas/yr
Parallax (π)1.44 ± 0.34  mas [1]
Distance 2,020+980
−510 [3]   pc
Absolute magnitude  (MV)−7.1 [3]
Details
Mass 24.4 [6]   M☉
Radius 32 [7]   R☉
Luminosity (bolometric)603,000 [8]   L☉
Temperature 35,000 [8]   K
Other designations
HD  152408, WR  79a, HR  6272, HIP  82775, SAO  227425, CD–40°10919, Trumpler 24 159 [9]
Database references
SIMBAD data
HD 152408 in Trumpler 24 is the brightest star, above centre, between the Prawn Nebula on the left and NGC 6231 on the right The Prawn Nebula in Scorpius.jpg
HD 152408 in Trumpler 24 is the brightest star, above centre, between the Prawn Nebula on the left and NGC 6231 on the right

HD 152408, also known as WR 79a, is a Wolf-Rayet star located in the constellation Scorpius, close to the galactic plane. Its distance is around 2,020 parsecs (6,500 lightyears) away from the Earth. [8]

HD 152408 lies in the north of the open cluster NGC 6231, the center of the OB association Scorpius OB1; it is not clear whether it is a part of the association or not. [10] With an apparent magnitude of about 5.77, [11] it is the third brightest Wolf-Rayet star. The other Wolf-Rayet stars that can be seen with the naked eye (although it can only be seen with the naked eye under excellent viewing conditions) are γ2 Velorum (WR 11), θ Muscae (WR 48), WR 22, WR 24 and HD 151932 (WR 78).

HD 152408 is about 24 times as massive as the Sun. Like most extremely massive stars, it is losing mass via its stellar wind. The total rate of mass loss is 2.4×10−5 M☉/yr. [8] With an effective temperature of 35,000  K , its bolometric luminosity is more than 600,000  L☉.

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WR 135 is a variable Wolf-Rayet star located around 6,000 light years away from Earth in the constellation of Cygnus, surrounded by a faint bubble nebula blown by the intense radiation and fast wind from the star. It is just over four times the radius of the sun, but due to a temperature of 63,000 K it is 250,000 times as luminous as the sun.

<span class="mw-page-title-main">WR 137</span> Star in the constellation of Cygnus

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<span class="mw-page-title-main">WR 1</span> Star in the constellation Cassiopeia

WR 1 is a Wolf-Rayet star located around 10,300 light years away from Earth in the constellation of Cassiopeia. It is only slightly more than twice the size of the sun, but due to a temperature over 100,000 K it is over 758,000 times as luminous as the sun.

<span class="mw-page-title-main">WR 12</span> Star in the constellation Vela

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<span class="mw-page-title-main">WR 9</span> Spectroscopic binary star system in the constellation Puppis

WR 9 is a spectroscopic binary in the constellation Puppis consisting of a Wolf-Rayet star and a class O star. It is around 12,000 light years away.

<span class="mw-page-title-main">HD 151932</span> Star in the constellation of Scorpius

HD 151932, also known as WR 78, is a Wolf-Rayet star located in the constellation Scorpius, close to the galactic plane. Its distance is around 1,300 parsecs away from the Earth. Despite being a blue-colored Wolf-Rayet star, it is extremely reddened by interstellar extinction, so its apparent magnitude is brighter for longer-wavelength passbands. HD 151932 lies about 22′ west of the open cluster NGC 6231, the center of the OB association Scorpius OB1; it is not clear whether it is a part of the association or not. With an apparent magnitude of about 6.5, it is one of the few Wolf-Rayet stars that can be seen with the naked eye.

<span class="mw-page-title-main">WR 133</span> Wolf-Rayet star and spectroscopic binary star in the constellation of Cygnus

WR 133 is a visually moderately bright Wolf-Rayet star. It is a spectroscopic binary system containing a Wolf-Rayet primary and a class O supergiant secondary. It is in the constellation of Cygnus, lying in the sky at the centre of the triangle formed by β and γ Cygni, near η Cygni. It is the brightest member of the sparse open cluster NGC 6871.

References

  1. 1 2 3 4 5 van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
  2. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. 1 2 3 Crowther, Paul A.; Rate, Gemma (2020). "Unlocking Galactic Wolf–Rayet stars with Gaia DR2 – I. Distances and absolute magnitudes". Monthly Notices of the Royal Astronomical Society. 493 (1): 1512–1529. arXiv: 1912.10125 . Bibcode:2020MNRAS.493.1512R. doi:10.1093/mnras/stz3614. S2CID   209444955.
  4. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862.
  5. ↑ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Washington, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
  6. ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID   118629873.
  7. ↑ Lamers, H. J. G. L. M.; Nugis, T. (November 2002). "An explanation for the curious mass loss history of massive stars: From OB stars, through Luminous Blue Variables to Wolf-Rayet stars". Astronomy & Astrophysics. 395 (1): L1–L4. arXiv: astro-ph/0210388 . Bibcode:2002A&A...395L...1L. doi:10.1051/0004-6361:20021381. ISSN   0004-6361. S2CID   18826723.
  8. 1 2 3 4 Skinner, Stephen L.; Zhekov, Svetozar A.; Güdel, Manuel; Schmutz, Werner; Sokal, Kimberly R. (2012-05-01). "New X-Ray Detections of WNL Stars". The Astronomical Journal. 143 (5): 116. arXiv: 1203.5098 . Bibcode:2012AJ....143..116S. doi:10.1088/0004-6256/143/5/116. ISSN   0004-6256. S2CID   119281411.
  9. ↑ "HD 152408". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 6 February 2021.
  10. ↑ Seggewiss, W.; Moffat, A. F. (1979). "The intrinsically bright Wolf-Rayet stars of type WN 7. III - The probable single SCO OB 1 star HD 151932 with variable He I envelope". Astronomy and Astrophysics. 72 (3): 332–338. Bibcode:1979A&A....72..332S.
  11. ↑ Heske, A.; Wendker, H. J. (1985). "Further photometry and spectroscopy in the young cluster region TR 24/Sco OB 1". Astronomy and Astrophysics. 151: 309–314. Bibcode:1985A&A...151..309H.
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