24 Aquilae
Observation data
Epoch J2000      Equinox J2000
Constellation Aquila
Right ascension 19h 18m 50.94777s[1]
Declination 00° 20′ 20.5448″[1]
Apparent magnitude (V) 6.423[2]
Characteristics
Spectral type K0-IIIa:CH1Ba0.5[3]
U−B color index +0.770[2]
B−V color index +1.050[2]
Astrometry
Radial velocity (Rv)−26.13±0.15[1] km/s
Proper motion (μ) RA: +10.755[1] mas/yr
Dec.: +11.298[1] mas/yr
Parallax (π)7.5115 ± 0.0437 mas[1]
Distance434 ± 3 ly
(133.1 ± 0.8 pc)
Absolute magnitude (MV)+0.64[4]
Details
Mass2.2[4] M☉
Radius11.17+0.32
−0.70[1] R☉
Luminosity56.397±0.468[1] L☉
Surface gravity (log g)2.48[5] cgs
Temperature4,733+155
−67[1] K
Metallicity [Fe/H]−0.19±0.06[5] dex
Age0.5[4] Gyr
Other designations
BD+00 4170, HD 181053, HIP 94913, HR 7321, SAO 124492[6]
Database references
SIMBADdata

24 Aquilae (abbreviated 24 Aql) is a star in the equatorial constellation of Aquila. 24 Aquilae is its Flamsteed designation. It is located at a distance of around 434 light-years (133 parsecs)[1] from Earth and has an apparent visual magnitude of 6.4.[2] According to the Bortle Dark-Sky Scale, this star is just visible to the naked eye in dark rural skies. It is drifting closer to the Sun with a radial velocity of −26 km/s.[1]

This is a so-called mild barium star, as identified by the presence of a weak absorption line of singly-ionized barium atoms at a wavelength of 455.4 nm. Such stars display an atmospheric overabundance of carbon and the heavy elements produced by the s-process, which was most likely transferred into the atmosphere by a wide binary stellar companion. However, in the case of 24 Aquilae, the abundances of heavy elements are near normal.[4]

At an estimated age of a half billion years,[4] 24 Aquilae is a evolved giant star with a stellar classification of K0 IIIa.[4] It has more than double the mass of the Sun, 11 times the Sun's radius, and shines with 56 times the Sun's luminosity.[1] It is radiating this energy into space from its outer atmosphere at an effective temperature of 4,733 K.[1] This heat is what gives it the cool orange hue characteristic of a K-type star.[7]

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 13 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data 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. Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants", Monthly Notices of the Royal Astronomical Society, 172 (3): 667–679, Bibcode:1975MNRAS.172..667J, doi:10.1093/mnras/172.3.667.
  3. ↑ Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
  4. 1 2 3 4 5 6 Smiljanic, R.; Porto de Mello, G. F.; da Silva, L. (June 2007), "Abundance analysis of barium and mild barium stars", Astronomy and Astrophysics, 468 (2): 679–693, arXiv:astro-ph/0702421, Bibcode:2007A&A...468..679S, doi:10.1051/0004-6361:20065867, S2CID 5863942.
  5. 1 2 Soubiran, C.; Le Campion, J.-F.; Cayrel de Strobel, G.; Caillo, A. (June 2010), "The PASTEL catalogue of stellar parameters", Astronomy and Astrophysics, 515: A111, arXiv:1004.1069, Bibcode:2010A&A...515A.111S, doi:10.1051/0004-6361/201014247, S2CID 118362423.
  6. ↑ "* 24 Aql". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-07-25.{{cite web}}: CS1 maint: postscript (link)
  7. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16
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