Astronomy:GCIRS 16SW
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Sagittarius[1] |
| Right ascension | 17h 45m 40.124s[2] |
| Declination | −29° 00′ 29.02″[2] |
| Characteristics | |
| Evolutionary stage | Slash star |
| Spectral type | Ofpe/WN9[3] |
| Apparent magnitude (J) | 14.75[4] |
| Apparent magnitude (H) | 11.6[4] |
| Apparent magnitude (K) | 9.34[5] |
| Orbit[6] | |
| Primary | Sagittarius A* |
| Companion | GCIRS 16SW |
| Period (P) | 1270±309 yr |
| Semi-major axis (a) | 2.32±0.46″ |
| Eccentricity (e) | 0.35±0.11 |
| Inclination (i) | 113.0±1.3° |
| Longitude of the node (Ω) | 113.2±1.4° |
| Periastron epoch (T) | 2132±29 |
| Argument of periastron (ω) (secondary) | 28±14° |
| Orbit[7] | |
| Period (P) | 19.4513±0.0011 d |
| Semi-major axis (a) | 140.6±4.7 R☉ |
| Inclination (i) | 70.85±0.6° |
| Periastron epoch (T) | 2451775.102±0.032 |
| Details[7] | |
| A | |
| Mass | ~50 M☉ |
| Radius | 54.5±1.8 × 58.2±1.9 × 62.7±2.1 R☉ |
| Luminosity | 1,100,000 L☉ |
| Surface gravity (log g) | 3.0 cgs |
| Temperature | 24,400 K |
| B | |
| Mass | ~50 M☉ |
| Radius | 54.5±1.8 × 58.2±1.9 × 62.7±2.1 R☉ |
| Luminosity | 1,100,000 L☉ |
| Surface gravity (log g) | 3.0 cgs |
| Temperature | 23,500 K |
| Other designations | |
GCIRS 16SW, IRS 16SW, S97, S1-16[8] | |
| Database references | |
| SIMBAD | data |
GCIRS 16SW, also known as S97, is a contact binary star located in the Galactic Center. It is composed of two hot massive stars of equal size that orbit each other with a period of 19.5 days. The stars are so close that their atmospheres overlap, and the two stars form an eclipsing binary varying in brightness by 0.35 magnitudes at infrared wavelengths.[7]
GCIRS 16SW orbits Sagittarius A* at approximately 19,000 AU, with a period of approximately 1,270 years.[6] At the stars' estimated mass of about 50 solar masses, they are predicted to have a lifespan of about 4 million years, indicating that the system formed within 0.1 parsecs (0.33 ly; 21,000 astronomical unit|AU) of Sagittarius A*, instead of having migrated inward from a greater distance.[7]
GCIRS 16SW was classified as a candidate luminous blue variable on the basis of its spectrum and physical properties.[9] This was before it was identified as an eclipsing binary, but it is still treated as a candidate LBV.[10]
Each star is strongly distorted by the gravity of the other star. The polar radius is calculated to be 54.5 R☉, while the radius along the direction of orbital motion is 58.2 R☉. The radius along the line joining the two stars is 62.7 R☉, while the separation of the centres of the two stars is 132.8 R☉. A calculation of properties treating the binary as a single star gave an effective temperature of 24,400 K.[9] The secondary component is found to have a temperature 96% of that of the primary. However, these temperatures yield a luminosity over a million times that of the sun, uncomfortably close to the Eddington luminosity for each star, and it is suspected the actual temperatures are slightly lower.[7]
The stellar wind of IRS 16SW may be the origin of three gas clouds in the galactic center called G1, G2 and G3.[11]
References
- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific 99 (617): 695. doi:10.1086/132034. Bibcode: 1987PASP...99..695R Constellation record for this object at VizieR.
- ↑ 2.0 2.1 Miho N. Ishigaki; Nozomu Tominaga; Chiaki Kobayashi; Ken'ichi Nomoto (2014). "Faint Population III Supernovae as the Origin of the Most Iron-Poor Stars". The Astrophysical Journal Letters 792 (2): L32. doi:10.1088/2041-8205/792/2/L32. Bibcode: 2014ApJ...792L..32I.
- ↑ Paumard, T.; Genzel, R.; Martins, F.; Nayakshin, S.; Beloborodov, A.M.; Levin, Y.; Trippe, S.; Eisenhauer, F. et al. (2006). "The two young star disks in the central parsec of the galaxy: Properties, dynamics, and formation". The Astrophysical Journal 643 (2): 1011–1035. doi:10.1086/503273. Bibcode: 2006ApJ...643.1011P.
- ↑ 4.0 4.1 Blum, R. D.; Ramírez, Solange V.; Sellgren, K.; Olsen, K. (2003). "Really Cool Stars and the Star Formation History at the Galactic Center". The Astrophysical Journal 597 (1): 323–346. doi:10.1086/378380. Bibcode: 2003ApJ...597..323B.
- ↑ Blum, R. D.; Sellgren, K.; Depoy, D. L. (1996). "JHKL Photometry and the K-Band Luminosity Function at the Galactic Center". The Astrophysical Journal 470: 864. doi:10.1086/177917. Bibcode: 1996ApJ...470..864B.
- ↑ 6.0 6.1 Gillessen, S.; Plewa, P. M.; Eisenhauer, F.; Sari, R.; Waisberg, I.; Habibi, M.; Pfuhl, O.; George, E. et al. (2017). "An Update on Monitoring Stellar Orbits in the Galactic Center" (in en). The Astrophysical Journal 837 (1): 30. doi:10.3847/1538-4357/aa5c41. ISSN 0004-637X. Bibcode: 2017ApJ...837...30G.
- ↑ 7.0 7.1 7.2 7.3 7.4 Peeples, Molly S. (January 2007). "The Nature of the Variable Galactic Center Source GCIRS 16SW Revisited: A Massive Eclipsing Binary". The Astrophysical Journal 654 (1): L61–L64. doi:10.1086/510720. Bibcode: 2007ApJ...654L..61P.
- ↑ "GCIRS 16SW". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=GCIRS+16SW.
- ↑ 9.0 9.1 Najarro, F.; Krabbe, A.; Genzel, R.; Lutz, D.; Kudritzki, R. P.; Hillier, D. J. (1997). "Quantitative spectroscopy of the HeI cluster in the Galactic center.". Astronomy and Astrophysics 325: 700. Bibcode: 1997A&A...325..700N.
- ↑ Smith, Nathan; Aghakhanloo, Mojgan; Murphy, Jeremiah W.; Drout, Maria R.; Stassun, Keivan G.; Groh, Jose H. (2019). "On the Gaia DR2 distances for Galactic luminous blue variables". Monthly Notices of the Royal Astronomical Society 488 (2): 1760. doi:10.1093/mnras/stz1712. Bibcode: 2019MNRAS.488.1760S.
- ↑ Gillessen, S.; Eisenhauer, F. et al. (March 2026). "The gas streamer G1–2–3 in the Galactic center". Astronomy & Astrophysics 707: A79. doi:10.1051/0004-6361/202555808. ISSN 0004-6361. Bibcode: 2026A&A...707A..79G.
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