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Iota Aquilae

From Wikipedia, the free encyclopedia
Star in the constellation Aquila
Iota Aquilae
Location of ι Aquilae (circled)
Observation data
Epoch J2000      Equinox J2000
ConstellationAquila[1]
Right ascension19h 36m 43.2777s[2]
Declination−01° 17′ 11.759″[2]
Apparent magnitude (V)4.364[3]
Characteristics
Spectral typeB5 III[4] or B6 IV[5]
U−Bcolor index−0.428[3]
B−Vcolor index−0.083[3]
R−Icolor index−0.08[6]
Astrometry
Radial velocity (Rv)−21.34±3.63[2] km/s
Proper motion (μ)RA: −1.426mas/yr[2]
Dec.: −21.644mas/yr[2]
Parallax (π)5.6673±0.1947 mas[2]
Distance580 ± 20 ly
(176 ± 6 pc)
Absolute magnitude (MV)−1.01[1]
Details
Mass4.8±0.3[7] M
Radius7.8±0.9[8] R
Luminosity851[7] L
Surface gravity (log g)3.64±0.05[7] cgs
Temperature14,500±600[8] K
Metallicity [Fe/H]0.09±0.04[1] dex
Rotational velocity (v sin i)55[9] km/s
Age100±8[7] Myr
Other designations
Al Thalimain,ι Aquilae, Iota Aql, ι Aql,41 Aql,GC 27103,HD 184930,HIP 96468,HR 7447,SAO 143597,PPM 180738,WDS J19367-0117A[10]
Database references
SIMBADdata

Iota Aquilae is astar in theequatorialconstellation ofAquila. Its identifier is aBayer designation that isLatinized from ι Aquilae, and abbreviated Iota Aql or ι Aql. The star has the traditional nameAl Thalimain, pronounced/ælˌθælɪˈmn/, which it shares withλ Aquilae. The name is derived from theArabic termالظليمینal-ẓalīmayn meaning "The Two Ostriches".[11] With anapparent visual magnitude of 4.364,[3] this star is bright enough to be seen with thenaked eye. Based upon an annualparallax shift of5.67±0.19 mas,[2] it is located at a distance of around 580light-years (180parsecs) from Earth.[2] The visual magnitude of the star is diminished by 0.15[7] fromextinction caused by intervening gas and dust.

In 1968, this star was assigned astellar classification of B5III,[4] which suggests it has which exhausted itshydrogen supply at itscore andevolved into ablue giant. However,stellar models from 2002 indicate it is around 100 million years old and has thus far spent 91% of its allotted lifetime on the main sequence.[7] In 2024, a study of standard stars suggested that Iota Aquilae be classified as B6 IV, matching asubgiant star.[5]

Iota Aquilae has nearly five times the mass of the Sun[7] and eight times the Sun's radius.[8] It is emitting 851[7] times the luminosity of the Sun from itsouter atmosphere at aneffective temperature of 14,500 K,[12] giving it the blue-white hue of aB-type star.[13] Theprojected rotational velocity of this star is 55 km/s.[9]

Nomenclature

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InChinese,右旗 (Yòu Qí), meaningRight Flag, refers to an asterism consisting of ι Aquilae,μ Aquilae,σ Aquilae,δ Aquilae,ν Aquilae,42 Aquilae,HD 184701,κ Aquilae and56 Aquilae.[14] Consequently, theChinese name for ι Aquilae itself is右旗五 (Yòu Qí wu, English:the Fifth Star of Right Flag.)[15]

This star, together withη Aql,θ Aql, δ Aql, κ Aql andλ Aql were once part of the obsolete constellationAntinous.[16]

References

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  1. ^abcAnderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation",Astronomy Letters,38 (5): 331,arXiv:1108.4971,Bibcode:2012AstL...38..331A,doi:10.1134/S1063773712050015,S2CID 119257644.
  2. ^abcdefgVallenari, A.; et al. (Gaia collaboration) (2023)."Gaia Data Release 3. Summary of the content and survey properties".Astronomy and Astrophysics.674: A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID 244398875. Gaia DR3 record for this source atVizieR.
  3. ^abcdKozok, J. R. (September 1985), "Photometric observations of emission B-stars in the southern Milky Way",Astronomy and Astrophysics Supplement Series,61:387–405,Bibcode:1985A&AS...61..387K.
  4. ^abLesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?",Astrophysical Journal Supplement,17: 371,Bibcode:1968ApJS...17..371L,doi:10.1086/190179.
  5. ^abNegueruela, I.; et al. (2024), "The IACOB project: XII. New grid of northern standards for the spectral classification of B-type stars",Astronomy and Astrophysics,690, id. A176,arXiv:2407.04163,Bibcode:2024A&A...690A.176N,doi:10.1051/0004-6361/202449298.
  6. ^Mallama, A. (2014), "Sloan Magnitudes for the Brightest Stars",Journal of the American Association of Variable Star Observers (Jaavso),42 (2): 443,Bibcode:2014JAVSO..42..443M.
  7. ^abcdefghLyubimkov, Leonid S.; et al. (June 2002), "Surface abundances of light elements for a large sample of early B-type stars - II. Basic parameters of 107 stars",Monthly Notices of the Royal Astronomical Society,333 (1):9–26,Bibcode:2002MNRAS.333....9L,doi:10.1046/j.1365-8711.2002.05341.x.
  8. ^abcGordon, Kathryn D.; et al. (March 2019), "Angular Sizes, Radii, and Effective Temperatures of B-type Stars from Optical Interferometry with the CHARA Array",The Astrophysical Journal,873 (1): 91,Bibcode:2019ApJ...873...91G,doi:10.3847/1538-4357/ab04b2,S2CID 125181833.
  9. ^abAbt, Helmut A.; et al. (July 2002), "Rotational Velocities of B Stars",The Astrophysical Journal,573 (1):359–365,Bibcode:2002ApJ...573..359A,doi:10.1086/340590.
  10. ^"iot Aql",SIMBAD,Centre de données astronomiques de Strasbourg, retrieved2012-07-18.
  11. ^"Patronage for Star #96165 | Patronize a star | OpenSea".
  12. ^Underhill, A. B.; et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars",Monthly Notices of the Royal Astronomical Society,189 (3):601–605,Bibcode:1979MNRAS.189..601U,doi:10.1093/mnras/189.3.601.
  13. ^"The Colour of Stars",Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived fromthe original on 2013-12-03, retrieved2012-01-16.
  14. ^(in Chinese)中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005,ISBN 978-986-7332-25-7.
  15. ^"AEEA 天文教育資訊網". Archived fromthe original on 3 December 2013. Retrieved1 September 2024.
  16. ^Ridpath, Ian,"Antinous",Ian Ridpath's Star Tales, retrieved2025-04-18.

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