Epsilon Sagittarii (Latinised from ε Sagittarii, abbreviated Epsilon Sgr, ε Sgr), formally named Kaus Australis /
Epoch J2000 Equinox J2000
|Right ascension||18h 24m 10.31840s|
|Declination||–34° 23′ 04.6193″|
|Apparent magnitude (V)||+1.85|
|Spectral type||B9.5 III|
|U−B color index||+0.13|
|B−V color index||–0.03|
|Radial velocity (Rv)||–15 km/s|
|Proper motion (μ)|| RA: –39.42 mas/yr |
Dec.: –124.20 mas/yr
|Parallax (π)||22.76 ± 0.24 mas|
|Distance||143 ± 2 ly |
(43.9 ± 0.5 pc)
|Absolute magnitude (MV)||–1.41|
|ε Sgr A|
|Mass||3.515 ± 0.138 M☉|
|Surface gravity (log g)||4.50 cgs|
|Rotational velocity (v sin i)||236 km/s|
|ε Sgr B|
The primary star, ε Sagittarii A, of this binary star system has a stellar classification of B9.5 III, with the luminosity class of III suggesting this is an evolved giant star that has exhausted the supply of hydrogen at its core. The interferometry-measured angular diameter of this star, after correcting for limb darkening, is 1.44 ± 0.06 mas, which, at its estimated distance, equates to a physical radius of about 6.8 times the radius of the Sun. This is a close match to the empirically-determined value of 6.9 solar radii. It has about 3.5 times the mass of the Sun and is radiating around 363 times the Sun's luminosity from its outer atmosphere at an effective temperature of 9,960 K. At this heat, the star glows with a blue-white hue.
This star is spinning rapidly with a projected rotational velocity of 236 km s−1. It has a magnetic field with a strength in the range 10.5–130.5 Gauss and it is an X-ray source with a luminosity of about 1030 erg s−1. The system displays an excess emission of infrared radiation, which suggests the presence of a circumstellar disk of dust. Based upon the temperature of this disk, it is orbiting at a mean separation of 155 AU from the primary.
As of 2001, the secondary star, ε Sagittarii B, is located at an angular separation of 2.392 arcseconds from the primary along a position angle of 142.3°. At the distance of this system, this angle is equivalent to a physical separation of about 106 AU, which places it inside the debris disk. It is a main sequence star with about 95% of the mass of the Sun. The system has a higher optical linear polarisation than expected for its distance from the Sun; this has been attributed to light scattered off the disk from the secondary. Prior to its 1993 identification using an adaptive optics coronagraph, this companion may have been responsible for the spectral anomalies that were attributed to the primary star. There is a candidate stellar companion at an angular separation of 32.3 arcseconds.
It bore the traditional name Kaus Australis, which derived from the Arabic قوس qaws 'bow' and Latin austrālis 'southern'. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included Kaus Australis for the star ε Sagittarii A.
In Chinese, 箕 (Jī), meaning Winnowing Basket, refers to an asterism consisting of Epsilon Sagittarii, Gamma Sagittarii, Delta Sagittarii and Eta Sagittarii. Consequently,the Chinese name for Epsilon Sagittarii itself is 箕宿三 (Jī Sù sān, English: the Third Star of Winnowing Basket.)
This star, together with:
- Gamma Sagittarii, Delta Sagittarii, Zeta Sagittarii, Lambda Sagittarii, Sigma Sagittarii, Tau Sagittarii and Phi Sagittarii, comprise the Teapot asterism.
- Gamma Sagittarii, Delta Sagittarii and Eta Sagittarii were Al Naʽām al Wārid (النعم الوارد), the 'Going Ostriches'.
- Gamma Sagittarii and Delta Sagittarii were Akkadian Sin-nun‑tu, or Si-nu-nu‑tum, 'the Swallow'.
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