Zeta Sagittarii
| |
| 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[1] mas |
| Distance | 88 ± 2 ly (27.0 ± 0.6 pc) |
| Absolute magnitude (MV) | 1.11/1.32[3] |
| Orbit[3] | |
| Period (P) | 21.00 ± 0.01 years |
| Semi-major axis (a) | 0.489 ± 0.001" |
| 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 | |
| Surface gravity (log g) | 3.90[6] cgs |
| Temperature | 8,799[6] K |
| Rotational velocity (v sin i) | 77[7] km/s |
| Other designations | |
Zeta Sagittarii (Zeta Sgr, ζ Sagittarii, ζ Sgr) is the third brightest star system in the constellation Sagittarius, with an apparent visual magnitude of +2.59.[2] It has the traditional name Ascella. Based upon parallax measurements, the distance to Ascella is about 88 ly (27 pc).[1] Ascella is moving away from the Solar System with a radial velocity of 22 km s−1.[5] Some 1.0–1.4 million years ago, this system came within 7.5 ± 1.8 ly (2.30 ± 0.55 pc) of the Sun.[8]
This is a binary star system, with the two components orbiting each other over a period of 21 years at an eccentricity of 0.211. The combined mass of the system is 5.26 ± 0.37 times the mass of the Sun[3] and their blended stellar classification is A2.5 Va.[4]
The system consists of a spectral class A2 giant with an apparent magnitude of +3.27, and an A4 subgiant with apparent magnitude of +3.48. The pair have a mean separation of 13.4 astronomical units (AU).[9] Ascella has a faint, 10th magnitude companion, separated from the primary by a distance of 75 arcseconds.
Name and etymology
- The name Ascella from a Late Latin word meaning armpit.
- This star, together with :
- γ Sgr, δ Sgr, ε Sgr, λ Sgr, σ Sgr, τ Sgr and φ Sgr comprising the asterism Teapot.[10][11]
- φ Sgr, σ Sgr, χ Sgr and τ Sgr were Al Naʽām al Ṣādirah (النعم السادرة), the Returning Ostriches.[12]
- σ Sgr and π Sgr may have been the Akkadian Gu-shi-rab‑ba, the Yoke of the Sea.[12]
- τ Sgr, ν Sgr, ψ Sgr, ω Sgr and 60 Sgr were Al Udḥiyy, the Ostrich's Nest.[12]
- 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.[13]
- In Chinese, 斗 (Dǒu), meaning Dipper, refers to an asterism consisting of ζ Sagittarii, φ Sagittarii, λ Sagittarii, μ Sagittarii, σ Sagittarii and τ Sagittarii. Consequently, ζ Sagittarii itself is known as 斗宿一 (Dǒu Sù yī, English: the First Star of Dipper.)[14]
Namesakes
- USS Ascella (AK-137) was a United States Navy Crater class cargo ship named after the star.
References
- 1 2 3 4 5 6 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
- 1 2 3 4 Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99). Bibcode:1966CoLPL...4...99J.
- 1 2 3 4 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: 2765–2785, arXiv:1112.3666, Bibcode:2012MNRAS.422.2765D, doi:10.1111/j.1365-2966.2011.20397.x
- 1 2 3 "CCDM J19026-2953AB -- Double or multiple star", SIMBAD Astronomical Object Database (Centre de Données astronomiques de Strasbourg), retrieved 2012-02-18
- 1 2 Wilson, R. E. (1953). General Catalogue of Stellar Radial Velocities. Carnegie Institute of Washington D.C. Bibcode:1953GCRV..C......0W.
- 1 2 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
- ↑ 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
- ↑ Dybczyński, P. A. (April 2006), "Simulating observable comets. III. Real stellar perturbers of the Oort cloud and their output", Astronomy and Astrophysics 449 (3): 1233–1242, Bibcode:2006A&A...449.1233D, doi:10.1051/0004-6361:20054284
- ↑ Kaler, James B., "ASCELLA (Zeta Sagittarii)", Stars (University of Illinois), retrieved 2012-02-18
- ↑ "Sagittarius". deepsky.astroinfo.org. Retrieved 30 August 2008.
- ↑ skywatchers Archived June 29, 2004 at the Wayback Machine
- 1 2 3 Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. p. 355. ISBN 0-486-21079-0. Retrieved 2012-09-04.
- ↑ 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: 430. Bibcode:1895MNRAS..55..429K. doi:10.1093/mnras/55.8.429.
- ↑ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 11 日
| ||||||||||||||||||||||||||||||||||
This article is issued from Wikipedia - version of the Sunday, February 14, 2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.