WR 114

Last updated
WR 114
Observation data
Epoch J2000       Equinox J2000
Constellation Scutum
Right ascension 18h 23m 16.34s [1]
Declination −13° 43′ 26.2″ [1]
Apparent magnitude  (V)12.02 [2]
Characteristics
Evolutionary stage Wolf-Rayet
Spectral type WC5 [3]
U−B color index +0.54 [2]
B−V color index +0.97 [2]
Astrometry
Proper motion (μ)RA: 0.307 [4]   mas/yr
Dec.: −1.931 [4]   mas/yr
Parallax (π)0.4500 ± 0.0369  mas [4]
Distance 7,200 ± 600  ly
(2,200 ± 200  pc)
Absolute magnitude  (MV)−4.19 [3]
Details [3]
Mass 13.1+1.3
−1.0  M☉
Radius 2.68  R☉
Luminosity 245,000  L☉
Temperature 79,000  K
Other designations
HD  169010, GSC  05702-01056, 2MASS  J18231633-1343261, WR  114
Database references
SIMBAD data

WR 114 is a Wolf-Rayet star in the constellation of Scutum. It is an early type star of the carbon sequence (WCE) classified as WC5.

Contents

Companion

WR 114 is listed in the Catalogue of galactic Wolf Rayet stars as a possible binary system with an OB companion, but more recent studies have not confirmed this and it is now considered a single WC5 star. No x-rays have been detected from WR 114, which would be expected by a close hot companion. [5] [6]

Properties

The modelled temperature as a single star is 79,000 K, but this is an arbitrary temperature. A Wolf-Rayet star consists of a dense "core", with its surface defined as the sonic point, and a surrounding optically dense wind. The observed radiation from the star is entirely generated at different layers within the wind. The properties of a Wolf Rayet star are typically reported at an "inner boundary" of the wind, arbitrarily set at an optical depth of 20. The radius of this inner boundary in WR 114 is 2.51 R☉. The sonic point of WR 114 lies at about optical depth 60. At this level the temperature is much hotter. Another common definition for the surface of a star is at optical depth 2/3. For WR 114, this is at about 3.2 R☉ and the corresponding temperature is around 65,000 K. The luminosity is around 245,000 L☉ due to the extreme temperature, with most of this emitted as ultraviolet radiation. [3] [7]

The stellar wind from WR 114 is powered by the high temperature and luminosity to a speed of 2,000 km/s. [6] It is calculated to have a current mass of 13 M☉ and to be losing this mass at three millionths of M☉ per year. [3]

IRC −10414

WR 114 is about 45" from another luminous star of similar brightness. IRC −10414 is a red supergiant about 6,500 light years away. At this distance, the projected separation between the two stars would be 0.43 parsecs. WR 114 is listed in the Catalogue of galactic Wolf Rayet stars at around 6,500 light years, but more recent modelling estimates it to be brighter and hence probably more distant. IRC −10414 is a runaway with a visible bow shock and it is thought that a Wolf-Rayet star less than half a parsec away would disrupt the bow shock. It is still speculated that the two stars may have a common origin. [8]

Related Research Articles

<span class="mw-page-title-main">WR 136</span> Star in the constellation of Cygnus

WR 136 is a Wolf–Rayet star located in the constellation Cygnus. It is in the center of the Crescent Nebula. Its age is estimated to be around 4.7 million years and it is nearing the end of its life. Within a few hundred thousand years, it is expected to explode as a supernova.

<span class="mw-page-title-main">WR 22</span> Binary star in the constellation Carina

WR 22, also known as V429 Carinae or HR 4188, is an eclipsing binary star system in the constellation Carina. The system contains a Wolf-Rayet (WR) star that is one of the most massive and most luminous stars known, and is also a bright X-ray source due to colliding winds with a less massive O class companion. Its eclipsing nature and apparent magnitude make it very useful for constraining the properties of luminous hydrogen-rich WR stars.

WR 147 is a multiple star system in the constellation of Cygnus. The system is extremely reddened by interstellar extinction – that is, dust in front of the star scatters much of the blue light coming from WR 147, leaving the star appearing reddish.

WR 156 is a young massive and luminous Wolf–Rayet star in the constellation of Cepheus. Although it shows a WR spectrum, it is thought to be a young star still fusing hydrogen in its core.

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.

IRC −10414 is a red supergiant and runaway star in the constellation Scutum, a rare case of a red supergiant with a bow shock.

<span class="mw-page-title-main">WR 102</span> Star in the constellation Sagittarius

WR 102 is a Wolf–Rayet star in the constellation Sagittarius, 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.

<span class="mw-page-title-main">WR 93b</span> Wolf-Rayet star in the constellation of Cygnus

WR 93b is a Wolf-Rayet star in the constellation Scorpius, an extremely rare star on the WO oxygen sequence. It appears near NGC 6357 in the tail of the scorpion.

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

WR 137 is a variable Wolf-Rayet star located around 6,000 light years away from Earth in the constellation of Cygnus.

WR 111 is a Wolf-Rayet (WR) star in the constellation Sagittarius. It is magnitude 7.8 and lies about 5,150 light-years away. It is one of the brightest and most closely studied WR stars.

<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 128</span> Wolf-Rayet star in the constellation Sagitta

WR 128 is a Wolf–Rayet star located about 9,500 light years away in the constellation of Sagitta. A member of the WN class, WR 128's spectrum resembles that of a WN4 star, but hydrogen is clearly present in the star, making it the only known hydrogen-rich WN4 star in the galaxy. However, similar H-rich very early WN stars can be found in the LMC and especially in the SMC, but the only other galactic examples of this are WR 3 and WR 152.

WR 69 is a Wolf–Rayet star located 11,350 light years away in the constellation of Triangulum Australe. It is classified as a WC9 star, belonging to the late-type carbon sequence. WR 69 is also a prolific dust maker, hence the "d" in its spectral type.

WR 150 is a Wolf-Rayet star in the constellation of Cygnus. It is one of the early-type carbon sequence (WCE), and is of spectral type WC5. WR 150 is very far from the Earth, being 28,500 light-years from it.

WR 138a is a Wolf-Rayet star in the constellation Cygnus. It is of a very late spectral type of WN9h. The WR is also at the centre of a ring nebula and is a runaway.

<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.

WR 119 is a Wolf–Rayet star located about 10,500 light years away in the constellation Scutum. WR 119 is classified as a WC9 star, belonging to the late-type carbon sequence of Wolf-Rayet stars. WR 119 is noteworthy for being the least luminous known Wolf-Rayet star, at just over 50,000 L☉. The most recent estimate is even lower, at just 42,700 L☉, based on the most recent analysis using Gaia DR2 data.

References

  1. 1 2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  2. 1 2 3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  3. 1 2 3 4 5 Sander, A. A. C.; Hamann, W.-R.; Todt, H.; Hainich, R.; Shenar, T.; Ramachandran, V.; Oskinova, L. M. (2019). "The Galactic WC and WO stars". Astronomy & Astrophysics. 621: A92. arXiv: 1807.04293 . Bibcode:2019A&A...621A..92S. doi:10.1051/0004-6361/201833712. S2CID   67754788.
  4. 1 2 3 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  5. ↑ Ignace, R.; Oskinova, L. M.; Pollock, A. M. T.; Brown, J. C.; Hamann, W.-R. (2002). "X-rays from Wolf-Rayet Stars". American Astronomical Society. 201: 33.08. Bibcode:2002AAS...201.3308I.
  6. 1 2 Oskinova, L. M.; Ignace, R.; Hamann, W.-R.; Pollock, A. M. T.; Brown, J. C. (2003). "The conspicuous absence of X-ray emission from carbon-enriched Wolf-Rayet stars". Astronomy and Astrophysics. 402 (2): 755–766. arXiv: astro-ph/0303025 . Bibcode:2003A&A...402..755O. doi:10.1051/0004-6361:20030300. S2CID   9755058.
  7. ↑ Gräfener, G.; Vink, J. S. (2013). "Stellar mass-loss near the Eddington limit. Tracing the sub-photospheric layers of classical Wolf-Rayet stars". Astronomy & Astrophysics. 560: A6. arXiv: 1309.6236 . Bibcode:2013A&A...560A...6G. doi:10.1051/0004-6361/201321914. S2CID   118385793.
  8. ↑ Gvaramadze, V. V.; Menten, K. M.; Kniazev, A. Y.; Langer, N.; MacKey, J.; Kraus, A.; Meyer, D. M.-A.; Kamiński, T. (2014). "IRC -10414: A bow-shock-producing red supergiant star". Monthly Notices of the Royal Astronomical Society. 437 (1): 843. arXiv: 1310.2245 . Bibcode:2014MNRAS.437..843G. doi:10.1093/mnras/stt1943. S2CID   118416927.
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