Psi5 Aurigae

Today we will explore the fascinating world of Psi5 Aurigae. Whether you are interested in its impact on society, its historical relevance or simply want to know more about Psi5 Aurigae, this article will provide you with a complete and detailed overview of the topic. From its origins to its current influence, through its many facets and controversies, we will dive into a comprehensive analysis to better understand what Psi5 Aurigae is and why it is so important. So get ready for an informative journey that will open up new perspectives and knowledge about Psi5 Aurigae.

For other stars with a similar Bayer designation, see ψ Aurigae.
Psi5 Aurigae
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]
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 mas[1]
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 +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 Aurigae (ψ5 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. ^ 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:0708.1752v1, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600. 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 (4): 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/0611618, Bibcode:2007MNRAS.374..664C, doi:10.1111/j.1365-2966.2006.11196.x, S2CID 119428437.
  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" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
  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:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
  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/0607235, Bibcode:2007ApJS..168..297T, doi:10.1086/509763, S2CID 18775378.
  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:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  9. ^ "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.
  10. ^ Rodriguez, David R.; Zuckerman, B. (February 2012), "Binaries among Debris Disk Stars", The Astrophysical Journal, 745 (2): 147, arXiv:1111.5618, Bibcode:2012ApJ...745..147R, doi:10.1088/0004-637X/745/2/147, S2CID 73681879.
  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/0412356, Bibcode:2006ApJ...640.1051G, doi:10.1086/500161, S2CID 8563521.