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104 Aquarii

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This article is about A2Aquarii. For A1Aquarii, see103 Aquarii.For all stars with the sameBayer designation,seeA Aquarii.
104 Aquarii
Observation data
EpochJ2000EquinoxJ2000
Constellation Aquarius
A
Right ascension 23h41m45.80579s[1]
Declination –17° 48′ 59.5175″[1]
Apparent magnitude(V) 4.83[2]
B
Right ascension 23h41m46.37788s[1]
Declination –17° 47′ 00.7237″[1]
Apparent magnitude(V) 8.54[2]
Characteristics
A
Spectral type G2 Ib/II[3]
U−Bcolor index +0.49[2]
B−Vcolor index +0.82[2]
B
Spectral type A5/7 (V)[3]
B−Vcolor index +0.15[2]
Astrometry
A
Radial velocity(Rv)+6.52±0.15[4]km/s
Proper motion(μ)RA:+14.872[1]mas/yr
Dec.:+0.862[1]mas/yr
Parallax(π)4.5774 ± 0.1882mas[1]
Distance710 ± 30ly
(218 ± 9pc)
Absolute magnitude(MV)–2.49[4]
B
Proper motion(μ)RA:–27.214[1]mas/yr
Dec.:–28.539[1]mas/yr
Parallax(π)3.2221 ± 0.0487mas[1]
Distance1,010 ± 20ly
(310 ± 5pc)
Details
104 Aqr A
Mass4.23[5]M☉
Radius31.9±2.3[4]R☉
Luminosity447[5]L☉
Surface gravity(logg)2.20[4]cgs
Temperature5,444±14[4]K
Metallicity[Fe/H]+0.05[6]dex
Rotational velocity(vsini)15[7]km/s
Age135[5]Myr
Other designations
HR8982,SAO165836.[8]
A:BD−18 6358,HD222574,HIP116901
B:BD −18 6359, HD 222561, HIP 116904
Database references
SIMBADdata
B

104 Aquarii(abbreviated104 Aqr) is astarin theequatorialconstellationofAquarius.104 Aquariiis theFlamsteed designation,although it also bears theBayer designationA2Aquarii.Based on an annualparallaxshift of only3.89 ± 0.25milliarcseconds,the distance to this star is about 840light-years(260parsecs).[9]At that range, the brightness of the star in the V-band is reduced by 0.10 magnitudes as a result ofextinctioncaused by intervening gas and dust.[5]

This is a double star and possiblebinary system.[10]The primary component has astellar classificationof G2 Ib/II,[3]which places it on the borderline between thebright giantand lower luminositysupergiantstars. It has passed the firstdredge-upand may be undergoing Cepheid-like pulsations.[4]With more than four times the mass of the Sun,[5]this is anevolvedstar that has reached its current stage after only 135 million years.[5]It has expanded to around 51–88[11]times the Sun's radius and is radiating 447–fold[5]the luminosity of the Sun. This energy is being emitted from itsouter atmosphereat aneffective temperatureof 5,478 K,[6]giving it the golden-hued glow of aG-type star.[12]It is a suspectedvariable star.[13]

The companion is a magnitude 7.9 star with anangular separationof 120.1arcsecondsfrom the primary.[10]

References[edit]

  1. ^abcdefghijBrown, A. G. A.;et al. (Gaia collaboration) (August 2018)."GaiaData Release 2: Summary of the contents and survey properties ".Astronomy & Astrophysics.616.A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051.
  2. ^abcdeDucati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system".CDS/ADC Collection of Electronic Catalogues.2237.Bibcode:2002yCat.2237....0D.
  3. ^abcHouk, N.; Smith-Moore, M. (1988). "Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars. Volume 4, Declinations -26°.0 to -12°.0".Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars. Volume 4.Bibcode:1988mcts.book.....H.
  4. ^abcdefUsenko, I. A.; et al. (November 2015), "Spectroscopic studies of four southern-hemisphere G-K supergiants: HD 192876 (α1 Cap), HD 194215 (HR 7801), HD 206834 (c Cap), and HD 222574 (104 Aqr)",Astronomy Letters,41(11): 660–676,Bibcode:2015AstL...41..660U,doi:10.1134/S1063773715110067,S2CID124555577.
  5. ^abcdefgTakeda, Yoichi; Sato, Bun'ei; Murata, Daisuke (2008), "Stellar Parameters and Elemental Abundances of Late-G Giants",Publications of the Astronomical Society of Japan,60(4): 781–802,arXiv:0805.2434,Bibcode:2008PASJ...60..781T,doi:10.1093/pasj/60.4.781.
  6. ^abLuck, R. E.; Bond, H. E. (October 1980), "The chemical compositions of 26 distant late-type supergiants and the metallicity gradient in the galactic disk",Astrophysical Journal, Part 1,241:218–228,Bibcode:1980ApJ...241..218L,doi:10.1086/158334.
  7. ^Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities",Contributi Osservatorio Astronomico di Padova in Asiago,239(1): 1,Bibcode:1970CoAsi.239....1B.
  8. ^"104 Aqr".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2012-07-16.
  9. ^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,S2CID18759600.
  10. ^abEggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems",Monthly Notices of the Royal Astronomical Society,389(2): 869–879,arXiv:0806.2878,Bibcode:2008MNRAS.389..869E,doi:10.1111/j.1365-2966.2008.13596.x,S2CID14878976.
  11. ^Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics",Astronomy and Astrophysics,367(2): 521–524,arXiv:astro-ph/0012289,Bibcode:2001A&A...367..521P,doi:10.1051/0004-6361:20000451,S2CID425754.
  12. ^"The Colour of Stars",Australia Telescope, Outreach and Education,Commonwealth Scientific and Industrial Research Organisation,December 21, 2004, archived fromthe originalon February 22, 2012,retrieved2012-01-16.
  13. ^Demartino, Robert; et al. (April 1996), "Accurate Positions Of Suspected Variable Stars Near The South Galactic Pole",Information Bulletin on Variable Stars,4322:1,Bibcode:1996IBVS.4322....1D.

External links[edit]

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