Psi7 Aurigae

For other star systems with this Bayer designation, see Psi Aurigae.
Psi7 Aurigae
Diagram showing star positions and boundaries of the Auriga constellation and its surroundings


The location of ψ7 Aurigae (circled)

Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 06h 50m 45.94330s[1]
Declination +41° 46′ 52.4267″[1]
Apparent magnitude (V) 5.02[2]
Characteristics
Spectral type K3 III[3]
U−B color index +1.35[2]
B−V color index +1.27[2]
R−I color index 0.46
Astrometry
Radial velocity (Rv)+59.53 ± 0.25[4] km/s
Proper motion (μ) RA: –25.45[1] mas/yr
Dec.: –138.19[1] mas/yr
Parallax (π)8.61 ± 0.22[1] mas
Distance379 ± 10 ly
(116 ± 3 pc)
Details
Radius24[5] R☉
Surface gravity (log g)2.35[6] cgs
Temperature4,300[6] K
Metallicity [Fe/H]0.00[6] dex
Rotational velocity (v sin i)10[7] km/s
Other designations
58 Aurigae, BD+41 1536, FK5 2527, HD 49520, HIP 32844, HR 2516, SAO 41380.[8]

Psi7 Aurigae (ψ7 Aur, ψ7 Aurigae) is the Bayer designation for a single[9] star in the northern constellation of Auriga. It is a dim, naked eye star with an apparent visual magnitude of 5.02.[2] Based upon parallax measurements made during the Hipparcos mission,[1] it is approximately 379 light-years (116 parsecs) distant from Earth.

This is an evolved giant star with a stellar classification of K3 III.[3] The measured angular diameter of this star, after correction for limb darkening, is 1.96 ± 0.04 mas.[10] At it estimated distance,[1] this yields a physical size of about 24 times the radius of the Sun.[5] The outer envelope shines with an effective temperature of 4,300,[6] giving it the orange-hued glow of a K-type star.[11]

References

  1. 1 2 3 4 5 6 7 van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752v1, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. Note: see VizieR catalogue I/311.
  2. 1 2 3 4 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
  3. 1 2 Roman, Nancy G. (July 1952), "The Spectra of the Bright Stars of Types F5-K5", Astrophysical Journal 116: 122, Bibcode:1952ApJ...116..122R, doi:10.1086/145598.
  4. ↑ 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.
  5. 1 2 Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
    \begin{align} 2\cdot R_* & = \frac{(116\cdot 1.96\cdot 10^{-3})\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\ & \approx 48.9\cdot R_{\bigodot} \end{align}
  6. 1 2 3 4 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.
  7. ↑ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago 239 (1), Bibcode:1970CoAsi.239....1B.
  8. ↑ "58 Aur -- Star in double system", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), retrieved 2012-08-24.
  9. ↑ Eggleton, 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.
  10. ↑ 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
  11. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16.

External links

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