Psi5 Aurigae

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
Psi5 Aurigae
Diagram showing star positions and boundaries of the Auriga constellation and its surroundings
Cercle rouge 100%.svg
The location of ψ5 Aurigae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 06h 46m 44.3388s[1]
Declination +43° 34′ 38.737″[1]
Apparent magnitude (V) 5.25[2]
Spectral type G0 V[3]
U−B color index +0.06[2]
B−V color index +0.570[4]
Radial velocity (Rv) –24[5] km/s
Proper motion (μ) RA: –1.07[1] mas/yr
Dec.: +164.25[1] mas/yr
Parallax (π) 60.56 ± 0.73[1] mas
Distance 53.9 ± 0.6 ly
(16.5 ± 0.2 pc)
Absolute magnitude (MV) 4.13[5]
Mass 1.079[6] M
Radius 1.18[6] R
Surface gravity (log g) 4.06[3] cgs
Temperature 5,989[3] K
Metallicity [Fe/H] +0.05[3] dex
Rotational velocity (v sin i) 5.03[4] km/s
Age 3.2[5] Gyr
Other designations
56 Aurigae, ADS 5425, BD+43°1595, FK5 255, GJ 245, HD 48682, HIP 32480, HR 2483, SAO 41330.[7]
Database references

Psi5 Aurigae5 Aur, ψ5 Aurigae) is the Bayer designation for a star[8] in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 5.25.[2] Based upon parallax measurements made during the Hipparcos mission, this star is approximately 53.9 light-years (16.5 parsecs) distant from Earth.[1] There is an optical companion[8] which is 36 arcseconds away and has an apparent magnitude of +8.4.

The spectrum of this star shows it to be a G-type main sequence star with a stellar classification of G0 V.[3] Thought to be around 4 billion years old, it is similar in size, mass,[6] and composition to the Sun,[3] making this a solar analog, it is radiating energy into space at an effective temperature of 5,989 K,[3] giving it the golden-hued glow of a G-type star.[9]

Observation in the infrared shows an excess emission that suggests the presence of a circumstellar disk of dust, known as a debris disk, this material has a mean temperature of 60 K, indicating that it is orbiting at a distance of about 29 astronomical units from the host star. The dust has about half the mass of the Moon and is around 600 million years old,[10] the star is being examined for evidence of extrasolar planets,[11] but none have been found so far.


  1. ^ a b c d e f van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752v1Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.  Note: see VizieR catalogue I/311.
  2. ^ a b c Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society, 133: 475, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475. 
  3. ^ a b c d e f g Cenarro, A. J.; et al. (January 2007), "Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters", Monthly Notices of the Royal Astronomical Society, 374 (2): 664–690, arXiv:astro-ph/0611618Freely accessible, Bibcode:2007MNRAS.374..664C, doi:10.1111/j.1365-2966.2006.11196.x. 
  4. ^ a b Martínez–Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter", Astronomy and Astrophysics, 520: A79, arXiv:1002.4391Freely accessible, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725. 
  5. ^ a b c Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982Freely accessible, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191. 
  6. ^ a b c Takeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297–318, arXiv:astro-ph/0607235Freely accessible, Bibcode:2007ApJS..168..297T, doi:10.1086/509763. 
  7. ^ "psi05 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-24. 
  8. ^ a b 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:0806.2878Freely accessible, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x. 
  9. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16. 
  10. ^ Rodriguez, David R.; Zuckerman, B. (February 2012), "Binaries among Debris Disk Stars", The Astrophysical Journal, 745 (2): 147, arXiv:1111.5618Freely accessible, Bibcode:2012ApJ...745..147R, doi:10.1088/0004-637X/745/2/147. 
  11. ^ Grether, Daniel; Lineweaver, Charles H. (April 2006), "How Dry is the Brown Dwarf Desert? Quantifying the Relative Number of Planets, Brown Dwarfs, and Stellar Companions around Nearby Sun-like Stars", The Astrophysical Journal, 640 (2): 1051–1062, arXiv:astro-ph/0412356Freely accessible, Bibcode:2006ApJ...640.1051G, doi:10.1086/500161. 

External links[edit]