V861 Scorpii
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 Location of V861 Scorpii | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Scorpius |
| Right ascension | 16h 56m 35.98s[1] |
| Declination | −40° 49′ 24.4″[1] |
| Apparent magnitude (V) | 6.07 (- 5.28) - 6.40[2] |
| Characteristics | |
| Evolutionary stage | Blue supergiant |
| Spectral type | B2Iab/b[3] or B0 Iae + B2V [4] |
| Variable type | EB[2] |
| Astrometry | |
| Radial velocity (Rv) | −40.6 km/s |
| Proper motion (μ) | RA: −0.162[1] mas/yr[1] Dec.: −1.398[1] mas/yr[1] |
| Parallax (π) | 0.6577±0.0333 mas |
| Distance | 5,000 ± 300 ly (1,520 ± 80 pc) |
| Orbit[5] | |
| Period (P) | 7.84826 days |
| Eccentricity (e) | 0.163±0.024 |
| Periastron epoch (T) | JD 2443734.35±0.16 |
| Argument of periastron (ω) (secondary) | 35.9±7.6° |
| Semi-amplitude (K1) (primary) | 79.2±2.0 km/s |
| Details[6] | |
| A | |
| Mass | 40-60 M☉ |
| B | |
| Mass | 12.5±2 M☉ |
| Other designations | |
| Hen 3-1291, MCW 1269, OAO 1653-40, V861 Scorpii, CD+40°10975, HD 152667, HIP 82911, HR 6283, SAO 227473, TIC 341512659, 2MASS J16563597−4049244[3] | |
| Database references | |
| SIMBAD | data |
V861 Scorpii (also known as HD 152667, or V861 Sco) is a blue supergiant star and eclipsing binary system located in the constellation of Scorpius, within the open cluster Trumpler 24. Classified as a Beta Lyrae-type variable star, it exhibits both spectroscopic and photometric variability with an orbital period of approximately 7.848 days. Its visual magnitude ranges from 6.07 to 6.40, making it faintly visible to the naked eye under optimal conditions.[7][8][9][10]
Charecterstics
[edit]V861 Scorpii is a massive binary system with a primary star classified as a blue supergiant of spectral type B0.5Iae or B2Iab/b, indicating a hot, luminous star with emission lines. The system is located at a distance of approximately 5,000 light-years (1,520 parsecs) from Earth, based on Gaia DR3 parallax measurements of 0.6577±0.0333 milliarcseconds.
Binary System
[edit]V861 Scorpii is a spectroscopic binary with an orbital period of 7.848 days. The primary is a blue supergiant, while the nature of the secondary component remains less certain. Early studies suggested a possible compact companion, such as a black hole, due to its tentative association with the X-ray source OAO 1653-40. However, subsequent observations indicate that the X-ray emission is variable but consistent with a normal supergiant spectrum, and the association with a compact object is unconfirmed, with later evidence suggesting the X-ray source may be unrelated.[11][12][10][9]
Observations
[edit]
V861 Scorpii has been studied extensively for its photometric and spectroscopic variability. Observations from 1977–1980 revealed potential short-period variations in radial velocity, suggesting complex orbital dynamics. The star's light curves and stellar wind properties have been analyzed, showing no significant phase-dependent variations in infrared or ultraviolet observations. Its membership in the Trumpler 24 cluster has aided in determining its distance and evolutionary context.[9][14]
Reference
[edit]- ^ a b c d e 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.
- ^ a b Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085.
- ^ a b "V861 Scorpii". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2025-10-13.
- ^ sedici.unlp.edu.ar/bitstream/handle/10915/83324/Documento_completo.pdf?sequence=1
- ^ Stickland, D. J.; Howarth, I. D. (1991). "Spectroscopic binary orbits from ultraviolet radial velocities. Paper 7: V861 Scorpii (HD 152667)". The Observatory. 111: 23. Bibcode:1991Obs...111...23S.
- ^ Wolff, S. C.; Beichman, C. A. (June 1979). "The physical properties and orbital parameters of the B0 Ia star HD 152667 = V861 Scorpii: a supergiant with a black hole companion?". The Astrophysical Journal. 230: 519–525. Bibcode:1979ApJ...230..519W. doi:10.1086/157107. ISSN 0004-637X.
- ^ Guide, Universe (2015-01-25). "V861 Scorpii Star : Distance, Colour, Size (Radius), Location and Other Facts - Universe Guide". www.universeguide.com. Retrieved 2025-10-08.
- ^ Massey, P.; Conti, P. S. (July 1978). "V861 Scorpii". International Astronomical Union Circular (3247): 1. Bibcode:1978IAUC.3247....1M. ISSN 0081-0304.
- ^ a b c Polidan, R. S.; Oegerle, W. R.; Pollard, G. S. G.; Sanford, P. W.; Parmar, A. N. (1979). "1979ApJ...233L...7P Page L7". The Astrophysical Journal. 233. Bibcode:1979ApJ...233L...7P. doi:10.1086/183065.
- ^ a b Armstrong, J. T.; Johnston, M. D.; Bradt, H. V.; Cowley, A. P.; Doxsey, R. E.; Griffiths, R. E.; Hesser, J. E.; Schwartz, D. A. (1980). "Precise positions and optical search for the 38 second X-ray, pulsar near OAO 1653-40 and upper limit on X-ray emission from, V861 Sco". The Astrophysical Journal. 236. Bibcode:1980ApJ...236L.131A. doi:10.1086/183213.
- ^ Massey, P.; Conti, P. S. (July 1978). "V861 Scorpii". International Astronomical Union Circular (3247): 1. Bibcode:1978IAUC.3247....1M. ISSN 0081-0304.
- ^ W., Bunk; R., Haefner (November 1991). "Optical observations of the massive early-type binary V 861 Scorpii (= HD152667)". Astronomy and Astrophysics. 251: 515. Bibcode:1991A&A...251..515B. ISSN 0004-6361.
- ^ EAS (1997). "The HIPPARCOS and TYCHO catalogues". Astrometric and Photometric Star Catalogues Derived from the ESA Hipparcos Space Astrometry Mission. ESA SP Series. 1200. Noordwijk, Netherlands: ESA Publications Division. Bibcode:1997HIP...C......0E. ISBN 9290923997. Retrieved 13 October 2025.
- ^ Howarth, Ian D.; Wilson, R. (1981). "The Nature of V861 SCO (=HD 152667)". Effects of Mass Loss on Stellar Evolution. Astrophysics and Space Science Library. Vol. 89. pp. 481–486. doi:10.1007/978-94-009-8500-1_67. ISBN 978-94-009-8502-5.
