Astronomy:Epsilon Sagittarii

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Short description: Binary star in the constellation Sagittarius
ε Sagittarii
Sagittarius constellation map.svg
Red circle.svg
Location of ε Sagittarii (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Sagittarius
Right ascension  18h 24m 10.31840s[1]
Declination –34° 23′ 04.6193″[1]
Apparent magnitude (V) +1.85[2]
Characteristics
Spectral type B9.5 III[3]
U−B color index +0.13[2]
B−V color index –0.03[2]
Astrometry
Radial velocity (Rv)–15[4] km/s
Proper motion (μ) RA: –39.42[1] mas/yr
Dec.: –124.20[1] mas/yr
Parallax (π)22.76 ± 0.24[1] mas
Distance143 ± 2 ly
(43.9 ± 0.5 pc)
Absolute magnitude (MV)–1.41[5]
Details
ε Sgr A
Mass3.515 ± 0.138[5] M☉
Radius6.8[6] R☉
Luminosity363[5] L☉
Surface gravity (log g)4.50[7] cgs
Temperature9,960[8] K
Rotational velocity (v sin i)236[9] km/s
Age232[5] Myr
ε Sgr B
Mass0.95[5] M☉
Luminosity0.89[5] L☉
Temperature5,807[5] K
Other designations
Kaus Australis, ε Sagittarii, ε Sgr, Epsilon Sgr, 20 Sagittarii, CCDM J18242-3423A, FK5 689, GC 25100, HD 169022, HIP 90185, HR 6879, IDS 18175-3427 A, PPM 297655, SAO 210091, WDS J18242-3423A
Database references
SIMBADdata

Epsilon Sagittarii (Latinised from ε Sagittarii, abbreviated Epsilon Sgr, ε Sgr), formally named Kaus Australis /ˈkɔːs ɔːˈstreɪlɪs/,[10][11] is a binary star system in the southern zodiac constellation of Sagittarius. The apparent visual magnitude of +1.85[2] makes it the brightest object in Sagittarius. Based upon parallax measurements, this star is around 143 light-years (44 parsecs) from the Sun.

Observation

Epsilon Sagittarii can best be viewed in the months of June and July, since Sagittarius (constellation) is a summer constellation(winter in the southern hemisphere). The star is at least 10 degrees away from the ecliptic, and the Sun passes it overhead around December 25-26th. The star is visible from late January to late November from mid-northern latitudes. From mid-southern latitudes, the star is visible from early January until the middle of December. The star is not visible in areas above 55°N latitude. From latitudes below 55°S, Epsilon Sagittarii is a circumpolar star.

Stellar system

The primary star, ε Sagittarii A, of this binary star system has a stellar classification of B9.5 III,[3] 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,[12] which, at its estimated distance, equates to a physical radius of about 6.8 times the radius of the Sun.[6] This is a close match to the empirically-determined value of 6.9 solar radii.[13] 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.[5] At this heat, the star glows with a blue-white hue.[14]

This star is spinning rapidly with a projected rotational velocity of 236 km s−1.[9] It has a magnetic field with a strength in the range 10.5–130.5 Gauss[15] and it is an X-ray source with a luminosity of about 1030 erg s−1.[5] 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.[16]

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.[17] 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.[18] There is a candidate stellar companion at an angular separation of 32.3 arcseconds.[5]

Nomenclature

ε Sagittarii (Latinised to Epsilon Sagittarii) is the star system's Bayer designation.

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)[19] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[20] 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 the catalogue of stars in the Calendarium of Al Achsasi al Mouakket, this star was designated Thalath al Waridah, or Thalith al Waridah, meaning 'third of Warida'.[21]

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.)[22]

This star, together with:

Kaus Australis is listed in the Babylonian compendium MUL.APIN as MA.GUR8, meaning "the Bark".[25]

The Kalapalo people of Mato Grosso state in Brazil called this star and λ Scorpii, through ι Scorpii, θ Scorpii, ν Scorpii, υ Scorpii and ρ Scorpii Taugi kusugu, "Taugi's fishing basket".[26]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V 
  2. ↑ 2.0 2.1 2.2 2.3 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4: 99–100, Bibcode: 1966CoLPL...4...99J 
  3. ↑ 3.0 3.1 Houk, Nancy; Smith-Moore, M. (1979), "Michigan catalogue of two-dimensional spectral types for the HD stars", Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars. Volume_3. Declinations -40.0° to -26.0° (Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan) 3, Bibcode: 1982mcts.book.....H 
  4. ↑ Evans, D. S. (June 20–24, 1966). "Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30". in Batten, Alan Henry; Heard, John Frederick. 30. University of Toronto: International Astronomical Union. 57. Bibcode: 1967IAUS...30...57E. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 5.9 Hubrig, S.; Le Mignant, D.; North, P.; Krautter, J. (June 2001), "Search for low-mass PMS companions around X-ray selected late B stars", Astronomy and Astrophysics 372: 152–164, doi:10.1051/0004-6361:20010452, Bibcode: 2001A&A...372..152H 
  6. ↑ 6.0 6.1 Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1, https://books.google.com/books?id=OvTjLcQ4MCQC&pg=PA41 . The radius (R*) is given by:
    [math]\displaystyle{ \begin{align} 2\cdot R_* & = \frac{(10^{-3}\cdot 43.9\cdot 1.44)\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\ & \approx 13.6\cdot R_{\bigodot} \end{align} }[/math]
  7. ↑ Adelman, Saul J. (December 2004). "The A-Star Puzzle, held in Poprad, Slovakia, July 8-13, 2004". in Zverko, J.; Ziznovsky, J.; Adelman, S. J. et al.. 2004. Cambridge, UK: Cambridge University Press. pp. 1–11. doi:10.1017/S1743921304004314. Bibcode: 2004IAUS..224....1A. 
  8. ↑ Zorec, J. et al. (July 2009), "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ_1, D) parameters into Teff", Astronomy and Astrophysics 501 (1): 297–320, doi:10.1051/0004-6361/200811147, Bibcode: 2009A&A...501..297Z 
  9. ↑ 9.0 9.1 Royer, F. et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics 393 (3): 897–911, doi:10.1051/0004-6361:20020943, Bibcode: 2002A&A...393..897R 
  10. ↑ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7. 
  11. ↑ "IAU Catalog of Star Names". http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt. 
  12. ↑ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics 431 (2): 773–777, doi:10.1051/0004-6361:20042039, Bibcode: 2005A&A...431..773R 
  13. ↑ Jerzykiewicz, M.; Molenda-Zakowicz, J. (September 2000), "Empirical Luminosities and Radii of Early-Type Stars after Hipparcos", Acta Astronomica 50: 369–380, Bibcode: 2000AcA....50..369J 
  14. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16 
  15. ↑ Bychkov, V. D.; Bychkova, L. V.; Madej, J. (August 2003), "Catalogue of averaged stellar effective magnetic fields. I. Chemically peculiar A and B type stars", Astronomy and Astrophysics 407 (2): 631–642, doi:10.1051/0004-6361:20030741, Bibcode: 2003A&A...407..631B 
  16. ↑ Rodriguez, David R.; Zuckerman, B. (February 2012), "Binaries among Debris Disk Stars", The Astrophysical Journal 745 (2): 147, doi:10.1088/0004-637X/745/2/147, Bibcode: 2012ApJ...745..147R 
  17. ↑ Cotton, D. V. (January 2016). "The linear polarization of Southern bright stars measured at the parts-per-million level". Monthly Notices of the Royal Astronomical Society 455 (2): 1607–1628. doi:10.1093/mnras/stv2185. Bibcode: 2016MNRAS.455.1607C. 
  18. ↑ Golimowski, David A.; Durrance, Samuel T.; Clampin, Mark (March 1993), "Detection of an apparent star 2.1 arcsec from the circumstellar disk candidate Epsilon Sagittarii", Astronomical Journal 105 (3): 1108–1113, doi:10.1086/116498, Bibcode: 1993AJ....105.1108G 
  19. ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/. 
  20. ↑ "Bulletin of the IAU Working Group on Star Names, No. 1". http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf. 
  21. ↑ 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): 435. doi:10.1093/mnras/55.8.429. Bibcode: 1895MNRAS..55..429K. 
  22. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 11 日
  23. ↑ "Teapot". constellation-guide.com. http://www.constellation-guide.com/teapot/. 
  24. ↑ 24.0 24.1 Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. p. 355. ISBN 0-486-21079-0. https://archive.org/details/starnamestheirlo00alle/page/355. Retrieved 2012-09-04. 
  25. ↑ Rogers, J. H. (February 1998), "Origins of the ancient constellations: I. The Mesopotamian traditions", Journal of the British Astronomical Association 108 (1): 9–28, Bibcode: 1998JBAA..108....9R 
  26. ↑ Basso, Ellen B. (1987). In Favor of Deceit: A Study of Tricksters in an Amazonian Society. Tucson, Arizona: University of Arizona Press. p. 360. ISBN 0-8165-1022-9. https://archive.org/details/infavorofdeceits0000bass. 

External links



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