Tau Aquilae

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Tau Aquilae
Diagram showing star positions and boundaries of the Aquila constellation and its surroundings
Cercle rouge 100%.svg

Location of τ Aquilae (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Aquila
Right ascension 20h 04m 08.31550s[1]
Declination +07° 16′ 40.6683″[1]
Apparent magnitude (V) 5.6799 ± 0.0009[2]
Characteristics
Spectral type K0 III[3]
U−B color index +0.86[4]
B−V color index +1.06[4]
Astrometry
Radial velocity (Rv) –29.52 ± 0.23[2] km/s
Proper motion (μ) RA: +14.74[1] mas/yr
Dec.: +12.10[1] mas/yr
Parallax (π) 7.06 ± 0.41[1] mas
Distance 460 ± 30 ly
(142 ± 8 pc)
Details
Radius 16.5[5] R
Surface gravity (log g) 2.69[3] cgs
Temperature 4,660[3] K
Metallicity [Fe/H] –0.15[3] dex
Other designations
63 Aquilae, BD+06 4416, FK5 1524, HD 190327, HR 7669,HIP 98823, SAO 125403.[6]

Tau Aquilae (τ Aql, τ Aquilae) is the Bayer designation for a star in the equatorial constellation of Aquila. The apparent visual magnitude of 5.7[2] indicates it is a faint star that is visible to the naked eye from suburban skies; at least according to the Bortle Dark-Sky Scale. The annual orbital motion of the Earth causes a parallax shift of 7.06 mas,[1] which means the distance to this star is approximately 460 light-years (140 parsecs). The magnitude of the star is diminished by 0.28 from extinction caused by interstellar gas and dust.[2]

The spectrum of Tau Aquilae matches a stellar classification of K0 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 and left the main sequence of stars like the Sun. The measured angular diameter of this star is 1.08 ± 0.01 mas.[7] At the estimated distance of this system, this yields a physical size of about 16.5 times the radius of the Sun.[5] The outer envelope is radiating energy into space with an effective temperature of 4,660 K,[3] giving it the orange hued glow of a K-type star.[8]

References[edit]

  1. ^ a b c d e f 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. 
  2. ^ a b c d Famaey, B. et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics 430 (1): 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272. 
  3. ^ a b c d e f McWilliam, Andrew (December 1990), "High-resolution spectroscopic survey of 671 GK giants. I - Stellar atmosphere parameters and abundances", Astrophysical Journal Supplement Series 74: 1075–1128, Bibcode:1990ApJS...74.1075M, doi:10.1086/191527. 
  4. ^ a b Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99), Bibcode:1966CoLPL...4...99J. 
  5. ^ a b Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library 1 (3 ed.), Birkhäuser, ISBN 3-540-29692-1 . The radius (R*) is given by:
    \begin{align} 2\cdot R_*
 & = \frac{(142\cdot 1.08\cdot 10^{-3})\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\
 & \approx 33\cdot R_{\bigodot}
\end{align}
  6. ^ "tau Aql -- Star", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), retrieved 2012-07-21. 
  7. ^ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics 431: 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039 
  8. ^ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16 

External links[edit]