Astronomy:Psi5 Aurigae

From HandWiki
Short description: Star in the constellation Auriga


Psi5 Aurigae
Auriga constellation map.svg
Red circle.svg
Location of ψ5 Aurigae (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Auriga
Right ascension  06h 46m 44.3388s[1]
Declination +43° 34′ 38.737″[1]
Apparent magnitude (V) 5.25[2]
Characteristics
Spectral type G0 V[3]
U−B color index +0.06[2]
B−V color index +0.570[4]
Astrometry
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
Distance53.9 ± 0.6 ly
(16.5 ± 0.2 pc)
Absolute magnitude (MV)4.13[5]
Details
Mass1.079[6] M
Radius1.18[6] R
Surface gravity (log g)4.06[3] cgs
Temperature5,989[3] K
Metallicity [Fe/H]+0.05[3] dex
Rotational velocity (v sin i)5.03[4] km/s
Age3.2[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
SIMBADdata
ψ5 Aurigae in optical light

Psi5 Aurigae5 Aur, ψ5 Aurigae) is 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.

It used to be known to be part of a much bigger constellation named Telescopium Herschelii before it was unrecognized by the International Astronomical Union (IAU).

Characteristics

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]

Debris disk

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.

See also

References

  1. Jump up to: 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode2007A&A...474..653V.  Note: see VizieR catalogue I/311.
  2. Jump up to: 2.0 2.1 2.2 Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society 133 (4): 475, doi:10.1093/mnras/133.4.475, Bibcode1966MNRAS.133..475A. 
  3. Jump up to: 3.0 3.1 3.2 3.3 3.4 3.5 3.6 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, doi:10.1111/j.1365-2966.2006.11196.x, Bibcode2007MNRAS.374..664C. 
  4. Jump up to: 4.0 4.1 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, doi:10.1051/0004-6361/200913725, Bibcode2010A&A...520A..79M, http://eprints.ucm.es/37826/1/davidmontes17libre.pdf, retrieved 2018-11-04. 
  5. Jump up to: 5.0 5.1 5.2 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, doi:10.1051/0004-6361/200811191, Bibcode2009A&A...501..941H. 
  6. Jump up to: 6.0 6.1 6.2 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, doi:10.1086/509763, Bibcode2007ApJS..168..297T. 
  7. "psi05 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=psi05+Aur. 
  8. Jump up to: 8.0 8.1 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode2008MNRAS.389..869E. 
  9. "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16. 
  10. Rodriguez, David R.; Zuckerman, B. (February 2012), "Binaries among Debris Disk Stars", The Astrophysical Journal 745 (2): 147, doi:10.1088/0004-637X/745/2/147, Bibcode2012ApJ...745..147R. 
  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, doi:10.1086/500161, Bibcode2006ApJ...640.1051G. 

External links