Astronomy:Cygnus OB2-12

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Short description: Blue hypergiant star
Cygnus OB2 #12
CygOB2 med.jpg
Red circle.svg
Location of Cygnus OB2 #12 (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Cygnus
Right ascension  20h 32m 40.9572s[1]
Declination 41° 14′ 29.279″[1]
Apparent magnitude (V) 11.702
Characteristics
Apparent magnitude (B) 14.41[2]
Apparent magnitude (V) 11.40[2]
Apparent magnitude (J) 4.667±0.324[3]
Apparent magnitude (H) 3.512±0.260[3]
Apparent magnitude (K) 2.704±0.364[3]
U−B color index 1.69[2]
B−V color index 3.01[2]
Variable type cLBV
Astrometry
Radial velocity (Rv)−11.00[4] km/s
Proper motion (μ) RA: −1.703[1] mas/yr
Dec.: −3.412[1] mas/yr
Parallax (π)0.5895 ± 0.0518[1] mas
Distance5,500 ± 500 ly
(1,700 ± 100 pc)
Absolute magnitude (MV)−9.82[5]
Details
Mass110[6] M☉
Radius246[6] R☉
Luminosity1,660,000[5] L☉
Temperature13,700[6] K
Age3.0[6] Myr
Other designations
Cyg OB2 #12, Schulte 12, 2MASS J20324096+4114291, NSV 13138, HIP 101364, Gaia DR2 2067782734461462912
Database references
SIMBADdata

Cygnus OB2 #12 is an extremely luminous blue hypergiant with an absolute bolometric magnitude (all electromagnetic radiation) of −10.9, among the most luminous stars known in the galaxy. This makes the star nearly two million times more luminous than the Sun, although estimates were even higher when the star was first discovered. It is now known to be a binary, with the companion approximately a tenth as bright. A very approximate initial estimate of the orbit gives the total system mass as 120 M☉ and the period as 30 years.

Cygnus OB2

Cygnus OB2 #12 is generally assumed to be a member of the Cyg OB2 Association, a cluster of young massive stars about 4,600 light-years (1,400 pc) away in Cygnus, and resides in a region of the Milky Way from which visible light is heavily absorbed by interstellar dust when viewed from Earth. The dust causes the star to be strongly reddened despite being an intrinsically hot and blue star, hence it has been extensively studied in the infra-red. Were it not for the dust extinction, the star would have a visual magnitude about 1.5, nearly as bright as Deneb (Alpha Cygni), but because of the dust the observed visual magnitude is 11.4 so that it requires binoculars or a small telescope to be seen.[7]

There are several fainter stars around Cygnus OB2 #12, thought to comprise a small cluster. Two stars are only resolved by speckle interferometry. One is thought to be a main sequence B star in a 100–200 year orbit. It is 2.3 magnitudes fainter than the primary star and 0.063" away. The other is 4.8 magnitudes fainter and about an arc-second distant. No spectroscopic companion could be detected in the spectrum.[8] However, analysis of x-ray emission suggests that there may be a hot luminous companion in a close orbit, with their colliding winds creating the x-rays.[5]

Distance

The Gaia Data Release 2 parallax for Cygnus OB2 #12 indicated a distance around 840 pc, which was inconsistent with the distance of other Cygnus OB2 members.[9] However, the result included a significant amount of noise suggesting that it may have been inaccurate.[10] Earlier measures of the parallax were too imprecise to be meaningful.[11] If the closer distance were accepted then the star would be a more conventional blue supergiant with a luminosity around 440,000 L☉, a radius of 118 R☉, and a current mass of 25 M☉.[9]

The later Gaia Data Release 3 is more precise and indicates a distance around 1,700 pc, more consistent with estimates of the distance to Cygnus OB2, although there is still a significant amount of astrometric noise.[1] Using the distance provided by Gaia EDR3 implies a luminosity of only about 316,000 L☉, a radius of about 100 R☉, and a mass much lower than the currently accepted 110 M☉. This would put the star’s luminosity below the Humphreys-Davidson limit.[12]

Properties

UKIDSS near-infrared image of Cygnus OB2 #12

Cygnus OB2 #12 is a candidate luminous blue variable (LBV). Its position in the HR diagram, luminosity, and spectrum all classify it as an LBV. It shows brightness variations of a few tenths of a magnitude, but these do not seem to be associated with colour changes that would be expected from an LBV.[13] The spectral type has varied slightly since its discovery, but not to the extent that would be normal for an LBV.[6] If the lower Gaia DR2 distance were correct then the properties of Cygnus OB2 #12 would mean it would be expected to pulsate at low amplitude with a period of a few days.[9]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 Reed, B. Cameron (2003). "Catalog of Galactic OB Stars". The Astronomical Journal 125 (5): 2531–2533. doi:10.1086/374771. Bibcode: 2003AJ....125.2531R. 
  3. ↑ 3.0 3.1 3.2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (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. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246. 
  4. ↑ Klochkova, V. G.; Chentsov, E. L. (2004). "The Optical Spectrum of an LBV Candidate in the Cyg OB2 Association". Astronomy Reports 48 (12): 1005–1018. doi:10.1134/1.1836024. Bibcode: 2004ARep...48.1005K. 
  5. ↑ 5.0 5.1 5.2 Oskinova, L. M.; Huenemoerder, D. P.; Hamann, W. -R.; Shenar, T.; Sander, A. A. C.; Ignace, R.; Todt, H.; Hainich, R. (2017). "On the Binary Nature of Massive Blue Hypergiants: High-resolution X-Ray Spectroscopy Suggests That Cyg OB2 12 is a Colliding Wind Binary". The Astrophysical Journal 845 (1): 39. doi:10.3847/1538-4357/aa7e79. Bibcode: 2017ApJ...845...39O. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 Clark, J. S.; Najarro, F.; Negueruela, I.; Ritchie, B. W.; Urbaneja, M. A.; Howarth, I. D. (2012). "On the nature of the galactic early-B hypergiants". Astronomy & Astrophysics 541: A145. doi:10.1051/0004-6361/201117472. Bibcode: 2012A&A...541A.145C. 
  7. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named cn
  8. ↑ Maryeva, O. V.; Chentsov, E. L.; Goranskij, V. P.; Dyachenko, V. V.; Karpov, S. V.; Malogolovets, E. V.; Rastegaev, D. A. (2016). "On the nature of high reddening of Cygnus OB2 #12 hypergiant". Monthly Notices of the Royal Astronomical Society 1602 (1): 491–507. doi:10.1093/mnras/stw385. Bibcode: 2016MNRAS.458..491M. 
  9. ↑ 9.0 9.1 9.2 Nazé, Yaël; Rauw, Gregor; Czesla, Stefan; Mahy, Laurent; Campos, Fran (2019). "Variations on a theme: The puzzling behaviour of Schulte 12". Astronomy and Astrophysics 627: A99. doi:10.1051/0004-6361/201935141. Bibcode: 2019A&A...627A..99N. 
  10. ↑ Berlanas, S. R.; Wright, N. J.; Herrero, A.; Drew, J. E.; Lennon, D. J. (2019). "Disentangling the spatial substructure of Cygnus OB2 from Gaia DR2". Monthly Notices of the Royal Astronomical Society 484 (2): 1838. doi:10.1093/mnras/stz117. Bibcode: 2019MNRAS.484.1838B. 
  11. ↑ Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  12. ↑ Klochkova, V. G.; Islentieva, E. S.; Panchuk, V. E. (2023-01-01), On the status of the star Schulte 12 in the association Cyg OB2, doi:10.48550/arXiv.2301.08916, https://ui.adsabs.harvard.edu/abs/2023arXiv230108916K, retrieved 2024-01-22 
  13. ↑ Chentsov, E. L.; Klochkova, V. G.; Panchuk, V. E.; Yushkin, M. V.; Nasonov, D. S. (2013). "Spectroscopy of 13 high-mass stars in the Cyg OB2 association". Astronomy Reports 57 (7): 527–547. doi:10.1134/S1063772913070019. Bibcode: 2013ARep...57..527C. 

External links



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