WR 148
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
Right ascension 20h 41m 21.54855s[2]
Declination +52° 35′ 15.1426″[2]
Apparent magnitude (V) 10.3[3]
Characteristics
Spectral type WN8h + O5V?[4]
Apparent magnitude (J) 8.759[5]
Apparent magnitude (K) 8.318[6]
U−B color index −0.45[7]
B−V color index +0.57[7]
Variable type Unique[3]
Astrometry
Radial velocity (Rv)−131.4±2.7[4] km/s
Proper motion (μ) RA: −5.629[2] mas/yr
Dec.: −3.315[2] mas/yr
Parallax (π)0.1022 ± 0.0114 mas[2]
Distance8,280[8] pc
Absolute magnitude (MV)−7.22[9]
Orbit[4]
Period (P)4.317336 days
Semi-major axis (a)46 R☉
Eccentricity (e)0
Inclination (i)18°
Semi-amplitude (K1)
(primary)		88.1±3.8 km/s
Semi-amplitude (K2)
(secondary)		79.2±3.1 km/s
Details
WR
Mass44[10] M☉
Radius26.5[9] R☉
Luminosity1,585,000[9] L☉
Temperature39,800[9] K
Rotational velocity (v sin i)≤ 150[4] km/s
OB
Mass37[4] M☉
Rotational velocity (v sin i)60+20
−10[4] km/s
Other designations
V1696 Cygni, BD+52°2777, HD 197406, HIP 102088
Database references
SIMBADdata

WR 148 is a spectroscopic binary in the constellation Cygnus. The primary star is a Wolf–Rayet star and one of the most luminous stars known. The secondary has been suspected of being a stellar-mass black hole but may be a class O main sequence star.

WR 148 shows a classic WN8h spectrum, but with the addition of weak central absorption on some of the emission lines.[11] NIII and NIV emission lines are stronger than NV, and HeI lines are stronger than HeII, The Balmer series hydrogen lines and some other lines have P Cygni profiles.[12]

WR 148 is erratically variable on timescales ranging from seconds to years, but it shows consistent brightness and radial velocity variations with a period of 4.32 days. There is little doubt that it is a binary system, due to the regular variations and the presence of hard x-ray radiation from colliding winds, but the secondary is not clearly detectable in the spectrum.[4] One proposal for a companion that would match the faint absorption features would be a B3 subgiant, but that is not compatible with the orbit. An early calculated orbit based on faint absorption features gave a relatively large mass ratio which imply either a very high companion mass, meaning a black hole, or an unreasonably low primary mass for a luminous WR star.[11] Another analysis of the spectrum finds absorption features consistent with an O5 star, similar masses for the two components, and only a small orbital inclination.[4]

Because of its erratic changes in apparent magnitude at so many frequencies WR 148 is classified in the General Catalogue of Variable Stars as a unique type of variable, not a member of any of the defined classes.[3] The shape of the light curve is unusual and has been modelled as being produced by an extended secondary object which may be an ionised cavity in the dense wind of the primary star, produced as the secondary orbits at a distance comparable to the radius of the primary star.[11]

WR 148 is found unusually far from the galactic plane for a Wolf–Rayet star, at 500–800 pc. Young massive stars such as WN8h WR stars are members of the thin disc population, on average only 60 pc from the galactic plane. It is suggested that WR 148 is a runaway from a supernova explosion.[11] Calculations based on its large peculiar velocity of 197 km/s, current binary orbit, and likely lifetime since any supernova, are consistent with expulsion from a very massive triple system.[4]

References

  1. ↑ "OMC Archive". OMC Archive. The Astronomical Data Centre at CAB. Retrieved 19 December 2021.
  2. 1 2 3 4 5 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.
  3. 1 2 3 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.
  4. 1 2 3 4 5 6 7 8 9 Munoz, Melissa; Moffat, Anthony F. J.; Hill, Grant M.; Shenar, Tomer; Richardson, Noel D.; Pablo, Herbert; St-Louis, Nicole; Ramiaramanantsoa, Tahina (2017). "WR 148: Identifying the companion of an extreme runaway massive binary*". Monthly Notices of the Royal Astronomical Society. 467 (3): 3105. arXiv:1609.08289. Bibcode:2017MNRAS.467.3105M. doi:10.1093/mnras/stw2283. S2CID 119199391.
  5. ↑ 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.
  6. ↑ Van Der Hucht, K. A. (2006). "New Galactic Wolf–Rayet stars, and candidates. An annex to the VIIth Catalogue of Galactic Wolf–Rayet Stars". Astronomy and Astrophysics. 458 (2): 453–459. arXiv:astro-ph/0609008. Bibcode:2006A&A...458..453V. doi:10.1051/0004-6361:20065819. S2CID 119104786.
  7. 1 2 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. Bibcode:2002yCat.2237....0D.
  8. ↑ Zhekov, Svetozar A. (2012). "X-rays from colliding stellar winds: The case of close Wolf–Rayet+O binary systems". Monthly Notices of the Royal Astronomical Society. 422 (2): 1332–1342. arXiv:1202.1386. Bibcode:2012MNRAS.422.1332Z. doi:10.1111/j.1365-2966.2012.20706.x. S2CID 86867278.
  9. 1 2 3 4 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. arXiv:astro-ph/0608078. Bibcode:2006A&A...457.1015H. doi:10.1051/0004-6361:20065052. S2CID 18714731.
  10. ↑ 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.
  11. 1 2 3 4 Marchenko, Sergey V.; Moffat, Anthony F. J.; Lamontagne, Robert; Tovmassian, Gaghik H. (1996). "The Wolf–Rayet Star HD 197406, with Its Strongly Ionizing Close Companion". Astrophysical Journal. 461: 386. Bibcode:1996ApJ...461..386M. doi:10.1086/177067.
  12. ↑ Smith, Lindsey F.; Shara, Michael M.; Moffat, Anthony F. J. (1996). "A three-dimensional classification for WN stars". Monthly Notices of the Royal Astronomical Society. 281 (1): 163–191. Bibcode:1996MNRAS.281..163S. doi:10.1093/mnras/281.1.163.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.