Zeta Sagittarii (ζ Sagittarii, abbreviated Zeta Sgr, ζ Sgr) is a triple star system and the third-brightest star in the constellation of Sagittarius after Kaus Australis and Nunki. Based upon parallax measurements, it is about 88 light-years (27 parsecs) from the Sun.[1]
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 19h 02m 36.73024s[1] |
| Declination | –29° 52′ 48.2279″[1] |
| Apparent magnitude (V) | 2.59[2] (3.27/3.48)[3] |
| Characteristics | |
| Spectral type | A2.5 Va[4] |
| U−B color index | 0.05[2] |
| B−V color index | 0.08[2] |
| Astrometry | |
| Radial velocity (Rv) | 22[5] km/s |
| Proper motion (μ) | RA: 10.79[1] mas/yr Dec.: 21.11[1] mas/yr |
| Parallax (π) | 36.98 ± 0.87 mas[1] |
| Distance | 88 ± 2 ly (27.0 ± 0.6 pc) |
| Absolute magnitude (MV) | 1.11/1.32[3] |
| Orbit[6] | |
| Primary | Aa |
| Companion | Ab |
| Period (P) | 1 month |
| Semi-major axis (a) | 0.3 au |
| Orbit[3] | |
| Primary | A |
| Companion | B |
| Period (P) | 21.00 ± 0.01 years |
| Semi-major axis (a) | 0.489 ± 0.001"[3] (13.2 au)[6] |
| Eccentricity (e) | 0.211 ± 0.001 |
| Inclination (i) | 111.1 ± 0.1° |
| Longitude of the node (Ω) | 74.0 ± 0.1° |
| Periastron epoch (T) | 2005.99 ± 0.03 |
| Argument of periastron (ω) (secondary) | 7.2 ± 0.6° |
| Details[6] | |
| Aa | |
| Mass | 1.83 M☉ |
| Radius | 1.9 R☉ |
| Luminosity | 14.9[a] L☉ |
| Surface gravity (log g) | 3.90[7] cgs |
| Temperature | 8,230 K |
| Rotational velocity (v sin i) | 77[8] km/s |
| Age | 700 Myr |
| Ab | |
| Mass | 1.81 M☉ |
| Radius | 1.9 R☉ |
| Luminosity | 14.7[a] L☉ |
| Temperature | 8,200 K |
| Age | 700 Myr |
| B | |
| Mass | 2.03 M☉ |
| Radius | 2.3 R☉ |
| Luminosity | 24[a] L☉ |
| Temperature | 8,460 K |
| Age | 700 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The three components are designated Zeta Sagittarii Aa (officially named Ascella /əˈsɛlə/, the traditional name for the entire system),[9][10] Ab and B.[6] The Washington Double Star Catalog cites a component separated 72.3" from the system, but it is a background star unrelated to the pair.[6]
Nomenclature
editζ Sagittarii (Latinised to Zeta Sagittarii) is the system's Bayer designation. The designations of the three components as ζ Sagittarii Aa, Ab and B derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[6][11]
It bore the traditional name Ascella, from a Late Latin word meaning armpit. In the catalogue of stars in the Calendarium of Al Achsasi al Mouakket, this star was designated Thalath al Sadirah, which was translated into Latin as Tertia τού al Sadirah, meaning third returning ostrich.[12] In 2016, the IAU organized a Working Group on Star Names (WGSN)[13] to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[14] It approved the name Ascella for the component Zeta Sagittarii A on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.[10]
This star, together with Gamma2 Sagittarii, Delta Sagittarii, Epsilon Sagittarii, Lambda Sagittarii, Sigma Sagittarii, Tau Sagittarii and Phi Sagittarii comprise the Teapot asterism.[15]
In Chinese, 斗 (Dǒu), meaning Dipper, refers to an asterism consisting of Zeta Sagittarii, Phi Sagittarii, Lambda Sagittarii, Mu Sagittarii, Sigma Sagittarii and Tau Sagittarii. Consequently, the Chinese name for Zeta Sagittarii itself is 斗宿一 (Dǒu Sù yī, English: the First Star of Dipper).[16]
Properties
editZeta Sagittarii has a combined apparent visual magnitude of 2.59[2] and a combined spectral type A2Va.[4] It is moving away from the Solar System with a radial velocity of 22 km s−1,[5] and some one million years ago, came within 11 pc (36 ly) of the Sun.[6]
Zeta Sagittarii Aa and Ab form an inner pair with an orbital period estimated to be roughly one month and a separation 0.3 au. They are similar-sized A-type stars, having 1.8 times the mass and 1.9 times the radius of the Sun. When these stars evolve and become red giants, around 500 million years in the future, it is expected that they will evolve into a common envelope phase.
The outer component, named Zeta Sagittarii B, forms a visual binary with the inner pair. It is separated by 1.32 au and has an orbital period of 21 years. It is the largest and most massive star in the system, 2.3 times larger and two times more massive than the Sun. It is expected to end its life into a 0.7 M☉ white dwarf, around 700 million years in the future.[6]
Based upon data obtained by the Hipparcos mission, Zeta Sagittarii was predicted to be the brightest star in the night sky around 1.2 million years ago, peaking with an apparent magnitude of −2.74.[17] However a 2023 analysis discarded this hypothesis, as the closest distance to the Sun has been recalculated to 36 light-years, much further away than the previously estimated 10 light-years.[6]
Notes
edit- ^ a b c Calculated, using the temperature and radius figures available by the Stefan-Boltzmann law: , where T is the temperature, R is the radius and L is the luminosity. 5772 is the solar nominal effective temperature, in Kelvins. GeoGebra is used to do calculation.
References
edit- ^ a b c d e f van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
- ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J
- ^ a b c d De Rosa, Robert J.; et al. (2011), "The VAST Survey -- II. Orbital motion monitoring of A-type star multiples", Monthly Notices of the Royal Astronomical Society, 422 (4): 2765–2785, arXiv:1112.3666, Bibcode:2012MNRAS.422.2765D, doi:10.1111/j.1365-2966.2011.20397.x, S2CID 102487103
- ^ a b "* zet Sgr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-02-18.
- ^ a b Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Carnegie Institute of Washington D.C., Bibcode:1953GCRV..C......0W
- ^ a b c d e f g h i Waisberg, Idel; Klein, Ygal; Katz, Boaz (2023-11-01), "Hidden Companions to Intermediate-mass Stars. XIV. Discovery of a 1.8 M☉, 0.3 au Companion to Ascella = Zeta Sagittarii A", Research Notes of the American Astronomical Society, 7 (11): 245, Bibcode:2023RNAAS...7..245W, doi:10.3847/2515-5172/ad0e72, ISSN 2515-5172
- ^ Gray, R. O.; et al. (October 2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.", The Astronomical Journal, 126 (4): 2048–2059, arXiv:astro-ph/0308182, Bibcode:2003AJ....126.2048G, doi:10.1086/378365, S2CID 119417105
- ^ Royer, F.; Zorec, J.; Gómez, A. E. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298
- ^ Davis, George A. (1944). "The pronunciations, derivations, and meanings of a selected list of star names". Popular Astronomy. 52: 8–30. Bibcode:1944PA.....52....8D.
- ^ a b Naming Stars, IAU.org, retrieved 16 December 2017
- ^ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
- ^ Knobel, E. B. (June 1895), "Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket", Monthly Notices of the Royal Astronomical Society, 55 (8): 430, Bibcode:1895MNRAS..55..429K, doi:10.1093/mnras/55.8.429
- ^ IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.
- ^ WG Triennial Report (2015-2018) - Star Names (PDF), p. 5, retrieved 2018-07-14
- ^ Teapot, constellation-guide.com, retrieved 2017-05-13
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 11 日 Archived 2011-05-22 at the Wayback Machine
- ^ Tomkin, Jocelyn (April 1998), "Once and Future Celestial Kings", Sky and Telescope, 95 (4): 59–63, Bibcode:1998S&T....95d..59T – based on computations from HIPPARCOS data. (The calculations exclude stars whose distance or proper motion is uncertain.) PDF[permanent dead link]