Astronomy:Xi Puppis

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Short description: Star in the constellation Puppis
ξ Puppis
Puppis constellation map.svg
Red circle.svg
Location of ξ Puppis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Puppis
Right ascension  07h 49m 17.65567s[1]
Declination −24° 51′ 35.2305″[1]
Apparent magnitude (V) 3.35[2]
Characteristics
Spectral type G6 Iab-Ib[3]
U−B color index +1.18[2]
B−V color index +1.25[2]
Astrometry
Radial velocity (Rv)+2.7[4] km/s
Proper motion (μ) RA: −4.81[1] mas/yr
Dec.: −0.89[1] mas/yr
Parallax (π)2.72 ± 0.21[1] mas
Distance1,200 ± 90 ly
(370 ± 30 pc)
Absolute magnitude (MV)–4.73[5]
Details
Mass9.9 ± 1.0[3] M
Luminosity60,000[6] L
Surface gravity (log g)1.21 ± 0.09[3] cgs
Temperature4,880 ± 150[3] K
Metallicity [Fe/H]+0.24[7] dex
Rotational velocity (v sin i)9.2[8] km/s
Age23[3] Myr
Other designations
Azmidi, Azmidiske, Asmidiske, ξ Puppis, ξ Pup, Xi Pup, 7 Puppis, CCDM J07493-2452A; CPD−24  2939, FK5 1204, GC 10562, HD 63700, HIP 38170, HR 3045, IDS 07451-2437 A, PPM 253258, SAO 174601, WDS J07493-2452A.
Database references
SIMBADdata

Xi Puppis (ξ Puppis, abbreviated Xi Pup, ξ Pup) is a multiple star system in the southern constellation of Puppis. With an apparent visual magnitude of 3.35,[2] it is one of the brighter members of this constellation. Based on parallax measurements made during the Hipparcos mission, it is located approximately 1,200 light-years (370 parsecs) from the Sun, with a 7.5% margin of error.[1]

The system consists of a spectroscopic binary, designated Xi Puppis A,[9] together with a third companion star, Xi Puppis B. A's two components are themselves designated Xi Puppis Aa (formally named Azmidi /ˈæzmɪdi/)[10] and Ab.

Nomenclature

ξ Puppis (Latinised to Xi Puppis) is the system's Bayer designation. The designations of the two constituents as Xi Puppis A and B, and those of A's components - Xi Puppis Aa and Ab - derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[11]

The system was sometimes known as Asmidiske (Azmidiske), a misspelling and misplacement of Aspidiske (from the Greek for 'little shield), the traditional name of Iota Carinae.[12] In 2016, the IAU organized a Working Group on Star Names (WGSN)[13] to catalog 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 Azmidi for the component Xi Puppis Aa on 1 June 2018 and it is now so included in the List of IAU-approved Star Names.[10]

Properties

Because of the distance of this system from the Earth, its visual magnitude is reduced by 0.73 as a result of extinction from the intervening gas and dust.[5]

Xi Puppis A presents as a yellow supergiant of spectral class G6 with a luminosity 8,300 times that of the Sun.[12]

The 13th-magnitude companion, Xi Puppis B, is about 5 arcseconds distant and is a Sun-like star that orbits at least 2000 AU away with an orbital period of at least 26,000 years.[12]

References

  1. Jump up to: 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode2007A&A...474..653V 
  2. Jump up to: 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): 99, Bibcode1966CoLPL...4...99J 
  3. Jump up to: 3.0 3.1 3.2 3.3 3.4 Lyubimkov, Leonid S. et al. (February 2010), "Accurate fundamental parameters for A-, F- and G-type Supergiants in the solar neighbourhood", Monthly Notices of the Royal Astronomical Society 402 (2): 1369–1379, doi:10.1111/j.1365-2966.2009.15979.x, Bibcode2010MNRAS.402.1369L 
  4. Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication (Carnegie Institute of Washington D.C.). Bibcode1953GCRV..C......0W. 
  5. Jump up to: 5.0 5.1 Luck, R. E. (May 1, 1982), "The chemical composition of late-type supergiants. IV - Homogeneous abundances and galactic metallicity trends", Astrophysical Journal, Part 1 256: 177–188, doi:10.1086/159895, Bibcode1982ApJ...256..177L 
  6. Reimers, D.; Huensch, M.; Schmitt, J. H. M. M.; Toussaint, F. (1996). "Hybrid stars and the reality of "dividing lines" among G to K bright giants and supergiants". Astronomy and Astrophysics 310: 813. Bibcode1996A&A...310..813R. 
  7. Malagnini, M. L.; Morossi, C.; Buzzoni, A.; Chavez, M. (2000). "Observations and Atmospheric Parameters of Super-Metal-rich Candidates". The Publications of the Astronomical Society of the Pacific 112 (777): 1455. doi:10.1086/317714. Bibcode2000PASP..112.1455M. 
  8. De Medeiros, J. R.; Udry, S.; Burki, G.; Mayor, M. (2002). "A catalog of rotational and radial velocities for evolved stars. II. Ib supergiant stars". Astronomy and Astrophysics 395: 97–98. doi:10.1051/0004-6361:20021214. Bibcode2002A&A...395...97D. 
  9. "Washington Double Star Catalog". United States Naval Observatory. http://ad.usno.navy.mil/wds/. 
  10. Jump up to: 10.0 10.1 "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/. 
  11. 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].
  12. Jump up to: 12.0 12.1 12.2 Kaler, James B., "ASMIDISKE (Xi Puppis)", Stars (University of Illinois), http://stars.astro.illinois.edu/sow/asmidiske.html, retrieved 2018-06-20 
  13. "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/. 
  14. "WG Triennial Report (2015-2018) - Star Names". p. 5. https://www.iau.org/static/science/scientific_bodies/working_groups/280/wg-starnames-triennial-report-2015-2018.pdf. 

External links