W Sagittarii
 
| |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18h 05m 01.22409s[1] |
| Declination | −29° 34′ 48.3199″[1] |
| Apparent magnitude (V) | 4.29 - 5.14[2] |
| Characteristics | |
| A | |
| Spectral type | F4 - G2Ib[2] + ~F5V[3] |
| U−B color index | +0.52[4] |
| B−V color index | +0.78[4] |
| Variable type | δ Cep[2] |
| B | |
| Spectral type | A0 V[3] |
| Astrometry | |
| Radial velocity (Rv) | –28.04[5] km/s |
| Proper motion (μ) | RA: +2.62[1] mas/yr Dec.: –5.28[1] mas/yr |
| Parallax (π) | 2.28 ± 0.20[6] mas |
| Distance | 409[3] pc |
| Absolute magnitude (MV) | −3.76[3] |
| Orbit[6] | |
| Primary | Aa |
| Companion | Ab |
| Period (P) | 1,582 ± 3 days |
| Semi-major axis (a) | 12.9 ± 0.3" (5.67 ± 0.13 AU) |
| Eccentricity (e) | 0.41 ± 0.02 |
| Inclination (i) | 7.0 ± 0.8° |
| Orbit[3] | |
| Primary | A |
| Companion | B |
| Period (P) | 172.9 yr |
| Semi-major axis (a) | 63 AU |
| Details | |
| A | |
| Mass | 5.8[3] M☉ |
| Radius | 61.0[7] R☉ |
| Luminosity | 2,690[3] L☉ |
| Surface gravity (log g) | 1.50 - 2.15[8] cgs |
| Temperature | 5,380 - 6,474[8] K |
| Metallicity [Fe/H] | +0.02[9] dex |
| B | |
| Mass | 2.2[3] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
W Sagittarii (W Sgr, Gamma-1 Sagittarii (γ¹ Sgr)) is a multiple star system star in the constellation Sagittarius. It is an optical line-of-sight companion to the much brighter Al Nasl (γ2 Sgr) which marks the "nozzle" ("spout") of the "teapot" asterism forming a large part of Sagittarius. The primary star is a supergiant Classical Cepheid variable.
System
W Sgr is listed as component A of a multiple star system catalogued as ADS 11029 and WDS J18050-2935. Components B and C are at 33" and 46" respectively and both are 13th magnitude. They are purely optical companions, not physically associated with W Sgr.[10]
Component A, W Sgr, is itself a triple star system, with the components referred to as W Sgr Aa, Ab, and B. The outer companion B has been resolved at a separation of 0.14" and is over 5 magnitudes fainter than the primary supergiant. The inner components can only be identified spectroscopically by their radial velocity variations. The primary is a 6 M☉ yellow supergiant, while the secondary is an early F main sequence star with a mass less than 1.4 M☉.[10]
Variability
The supergiant component W Sgr Aa is a variable star which pulsates regularly between magnitudes 4.3 and 5.1 every 7.59 days. During the pulsations, that temperature and spectral type also vary. It is classified as a Classical Cepheid (δ Cephei) variable.[3]
References
- 1 2 3 4 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752
. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. - 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.
- 1 2 3 4 5 6 7 8 9 Remage Evans, Nancy; Bond, Howard E.; Schaefer, Gail H.; Mason, Brian D.; Karovska, Margarita; Tingle, Evan (2013). "Binary Cepheids: Separations and Mass Ratios in 5 M ⊙ Binaries". The Astronomical Journal. 146 (4): 93. arXiv:1307.7123. Bibcode:2013AJ....146...93R. doi:10.1088/0004-6256/146/4/93.
- 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.
- ↑ Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213.
- 1 2 Benedict, G. Fritz; McArthur, Barbara E.; Feast, Michael W.; Barnes, Thomas G.; Harrison, Thomas E.; Patterson, Richard J.; Menzies, John W.; Bean, Jacob L.; Freedman, Wendy L. (2007). "Hubble Space Telescope Fine Guidance Sensor Parallaxes of Galactic Cepheid Variable Stars: Period-Luminosity Relations". The Astronomical Journal. 133 (4): 1810. arXiv:astro-ph/0612465. Bibcode:2007AJ....133.1810B. doi:10.1086/511980.
- ↑ Groenewegen, M. A. T. (2007). "The projection factor, period-radius relation, and surface-brightness colour relation in classical cepheids". Astronomy and Astrophysics. 474 (3): 975. Bibcode:2007A&A...474..975G. doi:10.1051/0004-6361:20078225.
- 1 2 Luck, R. E.; Andrievsky, S. M. (2004). "Phase-dependent Variation of the Fundamental Parameters of Cepheids. I. Periods from 6 to 10 Days". The Astronomical Journal. 128: 343. Bibcode:2004AJ....128..343L. doi:10.1086/420991.
- ↑ Marsakov, V. A.; Koval', V. V.; Kovtyukh, V. V.; Mishenina, T. V. (2013). "Properties of the population of classical Cepheids in the Galaxy". Astronomy Letters. 39 (12): 851. Bibcode:2013AstL...39..851M. doi:10.1134/S1063773713120050.
- 1 2 Evans, Nancy Remage; Massa, Derck; Proffitt, Charles (2009). "Massive Star Multiplicity: The Cepheid W Sgr". The Astronomical Journal. 137 (3): 3700. arXiv:0902.3281. Bibcode:2009AJ....137.3700E. doi:10.1088/0004-6256/137/3/3700.