WR 147

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 147
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus
Right ascension 20h 36m 43.632s[1]
Declination +40° 21′ 07.44″[1]
Apparent magnitude (V) 13.86 + 16.02[2]
Characteristics
WR
Evolutionary stage Wolf-Rayet star
Spectral type WN8h[3]
B−V color index +4.06
OB
Spectral type B0.5V[3]
B−V color index +4.09
Astrometry
Proper motion (μ) RA: −1.417[1] mas/yr
Dec.: −5.737[1] mas/yr
Parallax (π)0.5014 ± 0.0797 mas
Distance2100±200 ly
(630±70[4] pc)
Absolute magnitude (MV)−7.22[5]
Details
WR 147S (WR)
Mass51[6] M☉
Radius29.8[6] R☉
Luminosity1,995,000[6] L☉
Temperature39,800[6] K
WR 147N (OB)
Radius9.18 R☉
Luminosity50,000[7] L☉
Temperature28,500[7] K
Other designations
IRAS 20349+4010, 1E 2034+40.1, 2E 4394, 2MASS J20364364+4021075
Database references
SIMBADWR 147

Distance

The distance of WR 147 has been calculated to be 630 parsecs based on infrared photometry, which would place it in front of the OB association known as Cygnus OB2.[4] The extinction in the visual range was calculated to be 11.5 magnitudes and the absolute visual magnitude assumed to be −6.7.[4] This would make WR 147 one of the closest known Wolf-Rayet stars, despite its faint apparent magnitude.[2][5]

A later calculation using optical and ultraviolet photometry derived a slightly lower value for the extinction. Combined with an assumption of a brighter absolute magnitude, this gave a distance modulus of 10.6 corresponding to a distance of about 1,200 pc. This is still one of the nearest Wolf–Rayet systems to the sun.[5]

A Gaia Data Release 3 parallax of 0.5 mas corresponds to a distance of around 2,000 parsecs although there is considerable uncertainly on that value.[1]

System

WR 147 consists of at least two very massive stars. The primary is a Wolf–Rayet star, designated WR 147S or just WR 147. A companion, designated WR 147N, is a B-type main-sequence star or O-type giant) 0.5″ away to the north.[8] A much closer companion is also suspected on the basis of a "radio pinwheel" which would be produced as the companion orbits through the wind of the primary star with a period of 1.7 years.[9]

WR 147 was resolved into two components in the 1990s,[7] separated first at radio wavelengths.[4] Based on an angular separation of about 643±157 mas,[7] this translates to an projected (i.e. minimum) separation of about 403±45 AU, which is about thirteen times the distance between Neptune and the Sun.[10] The location of the companion resolved in the near-infrared is slightly further from the primary than the radio source originally called WR 147N, and it has been referred to as WR 147NIR.[11]

The Wolf–Rayet star in the system (WR 147S) has a luminosity of 2,000,000 L☉, making it one of the most luminous stars known. The B-type companion is much less luminous, at 50,000 L☉.

The orbital elements of WR 147's orbit are poorly known, as the two components are separated far enough that no orbital motion has been detected, but it is estimated that one orbit would take 1,300 years.[9] The inclination of WR 147's orbit to our line of sight is also unknown: numerous studies have given values ranging from 30° to 60°.[7] Constraining the value of the inclination is important because the true separation of the stars depends on the value.[7]

Colliding wind

Stellar wind from these two stars collide and emit X-rays and radio waves. The Wolf–Rayet star is losing mass at a rate of 2.4×10−5 M☉/yr and the companion is losing mass at a rate of 4×10−7 M☉/yr.[7] The plasma generated from the wind collision may reach temperatures as high as 2.7 keV, or 31 million kelvins.[10]

Despite the name, the colliding wind shock is actually considered to be collisionless, that is the ions in the wind do not for the most part directly collide.[3]

X-rays

In 2010, X-ray emission from WR 147 was resolved into two sources: one where the wind collision is thought to be occurring, and another directly from the Wolf–Rayet star, the cause of which is not clear.[3] It was hypothesized to be another massive star orbiting the Wolf–Rayet star; if so, it would have an orbital period of 15 to 20 days, with the total mass of the system being 20 M☉, leading to a separation of about 0.33 AU.[12]

See also
  • WR 140, the prototype colliding-wind binary

References
  1. Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. Niemela, Virpi S.; Shara, Michael M.; Wallace, Debra J.; Zurek, David R.; Moffat, Anthony F. J. (1998). "Hubble Space Telescope Detection of Optical Companions of WR 86, WR 146, and WR 147: Wind Collision Model Confirmed". The Astronomical Journal. 115 (5): 2047. Bibcode:1998AJ....115.2047N. doi:10.1086/300320.
  3. Zhekov, S. A.; Park, S. (2010). "Chandra Observations of WR 147 Reveal a Double X-ray Source". The Astrophysical Journal Letters. 709 (2): L119–L123. arXiv:0912.3554. Bibcode:2010ApJ...709L.119Z. doi:10.1088/2041-8205/709/2/L119. S2CID 118707042.
  4. Churchwell, E.; Bieging, J. H.; van der Hucht, K. A.; Williams, P. M.; Spoelstra, T. A. Th.; Abbott, D. C. (1992). "The Wolf–Rayet system WR 147 – A binary radio source with thermal and nonthermal components". Astrophysical Journal, Part 1. 393 (1): 329–340. Bibcode:1992ApJ...393..329C. doi:10.1086/171508.
  5. Hamann, W.-R.; Gräfener, G.; Liermann, A. (2006). "The Galactic WN stars. Spectral analyses with line-blanketed model atmospheres versus stellar evolution models with and without rotation". Astronomy and Astrophysics. 457 (3): 1015–1031. arXiv:astro-ph/0608078. Bibcode:2006A&A...457.1015H. doi:10.1051/0004-6361:20065052. S2CID 18714731.
  6. Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics. A57: 625. arXiv:1904.04687. Bibcode:2019A&A...625A..57H. doi:10.1051/0004-6361/201834850. S2CID 104292503.
  7. Reimer, A.; Reimer, O. (2009). "Parameter Constraints for High-Energy Models of Colliding Winds of Massive Stars: The Case WR 147". The Astrophysical Journal. 694 (2): 1139–1146. arXiv:0901.1297. Bibcode:2009ApJ...694.1139R. doi:10.1088/0004-637X/694/2/1139. S2CID 17754125.
  8. Zhekov, S. A. (2007). "Colliding stellar wind models with non-equilibrium ionization: X-rays from WR 147". Monthly Notices of the Royal Astronomical Society. 382 (2): 886–894. arXiv:0709.1686. Bibcode:2007MNRAS.382..886Z. doi:10.1111/j.1365-2966.2007.12450.x. S2CID 17164715.
  9. Rodríguez, Luis F.; Arthur, Jane; Montes, Gabriela; Carrasco-González, Carlos; Toalá, Jesús A. (2020). "A Radio Pinwheel Emanating from WR 147". The Astrophysical Journal. 900 (1): L3. arXiv:2008.03725. Bibcode:2020ApJ...900L...3R. doi:10.3847/2041-8213/abad9d. S2CID 221090126.
  10. Skinner, S. L.; Zhekov, S. A.; Güdel, M.; Schmutz, W. (2007). "XMM-Newton X-ray observations of the Wolf–Rayet binary system WR 147". Monthly Notices of the Royal Astronomical Society. 378 (4): 1491–1498. arXiv:0704.3235. Bibcode:2007MNRAS.378.1491S. doi:10.1111/j.1365-2966.2007.11892.x. S2CID 15552884.
  11. Williams, P. M.; Dougherty, S. M.; Davis, R. J.; Van Der Hucht, K. A.; Bode, M. F.; Setia Gunawan, D. Y. A. (1997). "Radio and infrared structure of the colliding-wind Wolf–Rayet system WR147". Monthly Notices of the Royal Astronomical Society. 289 (1): 10–20. Bibcode:1997MNRAS.289...10W. CiteSeerX 10.1.1.23.1193. doi:10.1093/mnras/289.1.10.
  12. Zhekov, S. A.; Park, S. (2010). "Chandra HETG Observations of the Colliding Stellar Wind System WR 147". The Astrophysical Journal. 721 (1): 518–529. arXiv:1007.4352. Bibcode:2010ApJ...721..518Z. doi:10.1088/0004-637X/721/1/518. S2CID 118456342.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.