63 Ophiuchi
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Sagittarius[1] |
| Right ascension | 17h 54m 54.04315s[2] |
| Declination | −24° 53′ 13.5444″[2] |
| Apparent magnitude (V) | 6.20[3] |
| Characteristics | |
| Spectral type | O8II((f))[4] |
| U−B color index | –0.89[5] |
| B−V color index | +0.04[5] |
| Astrometry | |
| Radial velocity (Rv) | –11[6] km/s |
| Proper motion (μ) | RA: +0.704[2] mas/yr Dec.: –2.194[2] mas/yr |
| Parallax (π) | 0.9071±0.0882 mas[2] |
| Distance | 3,600 ± 300 ly (1,100 ± 100 pc) |
| Absolute magnitude (MV) | −5.14±0.22[7] |
| Details | |
| Mass | 17±4[7] M☉ 29[8] M☉ |
| Radius | 12.0±1.2[7] R☉ |
| Luminosity | 11,500+820 −770[7] L☉ |
| Surface gravity (log g) | 3.51±0.03[7] cgs |
| Temperature | 35,000±300[7] K |
| Rotational velocity (v sin i) | 48±5[7] km/s |
| Age | 3.7[7] Myr |
| Other designations | |
| 63 Oph, CD−24°13615, HD 162978, HIP 87706, HR 6672, SAO 185928 | |
| Database references | |
| SIMBAD | data |
63 Ophiuchi is an O-type giant star in the constellation Sagittarius, despite its name. During a 2009 survey for companions of massive stars, it was observed using speckle interferometry but no companion was found.[9] The small parallax measurement of 0.91±0.09 mas suggest that this extremely luminous star may be located about 3,600 light-years away. An estimate of the distance based on the strength of the Ca II line yields a more modest value of 2,605 ly (799 pc).[10] The star lies only 0.3° north of the galactic plane.
In 1983, astronomers from the Sternberg Astronomical Institute in Moscow, Russia identified a faint, shell-shaped nebula surrounding the star that was being excited by the star's energy. Named Sharpless 22, this ring-shaped nebula has a double-shell structure with an inner envelope spanning 45–50′ (9–18 pc), surrounded by a diffuse envelope some 65–80′ (14–29 pc) across. At an estimated mass loss rate of (6–8) × 10−6 M☉/yr, it would take the star about (1–5) × 105 years to produce such a nebula from the outflow of its stellar wind.[11]
In 2025 the star was found to have a weak magnetic field, which is unusual for giant stars. It is considered an example of an transitional object between main sequence strongly magnetic stars and magnetic supergiants like Alnitak.[7]
References
[edit]- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- 1 2 3 4 5 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.
- ↑ 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.
- ↑ Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. (2014). "The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars". The Astrophysical Journal Supplement. 211 (1): 10. arXiv:1312.6222. Bibcode:2014ApJS..211...10S. doi:10.1088/0067-0049/211/1/10. S2CID 118847528.
- 1 2 Schild, R. E.; et al. (April 1983), "UBV photometry for southern OB stars", Astrophysical Journal Supplement Series, 51: 321–336, Bibcode:1983ApJS...51..321S, doi:10.1086/190852
- ↑ Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Washington, Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W
- 1 2 3 4 5 6 7 8 9 Barron, James A.; Wade, Gregg A.; Holgado, Gonzalo; Simón-Díaz, Sergio (2025-05-16), "A magnetic field detection in the massive O-type bright giant 63 Oph", The Astrophysical Journal, 991 (1): 79, arXiv:2505.11374, Bibcode:2025ApJ...991...79B, doi:10.3847/1538-4357/adf6d9
- ↑ Blex, Susanne; Haas, Martin; Chini, Rolf (2024). "The rotation rate of single- and double-lined southern O stars: Determining what increases the rotation rate in binaries". Astronomy and Astrophysics. 692. Bibcode:2024A&A...692A.192B. doi:10.1051/0004-6361/202450176.
- ↑ Mason, Brian D.; et al. (February 2009), "The High Angular Resolution Multiplicity of Massive Stars", The Astronomical Journal, 137 (2): 3358–3377, arXiv:0811.0492, Bibcode:2009AJ....137.3358M, doi:10.1088/0004-6256/137/2/3358, S2CID 119268845
- ↑ Megier, A.; et al. (November 2009), "The interstellar Ca II distance scale", Astronomy and Astrophysics, 507 (2): 833–840, Bibcode:2009A&A...507..833M, doi:10.1051/0004-6361/20079144
- ↑ Lozinskaya, T. A.; et al. (June 1983), "A New Search for Ring Nebulae around Of-Stars - SHARPLESS22", Soviet Astronomy Letters, 9 (6): 344–345, Bibcode:1983SvAL....9..344L
