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  • 21 Aug, 2019

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13 Trianguli
13 Trianguli is the Flamsteed designation for a star in the northern constellation of Triangulum. It has an apparent visual magnitude of 5.89, so according to the Bortle scale it is faintly visible from dark suburban skies. The star is located at a distance of 103 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +41 km/s. It made a close approach to the Sun some 665,000 years ago at an estimated separation of 34.3 light-years.

A stellar classification of G0 V indicates this is a main sequence star that is generating energy by fusing hydrogen into helium at its core. It has about 110% of the Sun's mass, 186% of the Sun's radius, and shines with 3.72 times the luminosity of the Sun. The stellar atmosphere has an effective temperature of 5,846 K, giving it the yellow hue of a G-type star. It appears to be older than the Sun, with an estimated age of 6.45 billion years.

In 1994, an astrometric companion was reported at an angular separation of 0.020″. However, follow-up observations reported in 2005 not only failed to recover this object but also returned a null result on a search for planetary companions. The star has been examined for an infrared excess that could indicate the presence of an orbiting debris disk, but no such excess was found.

References

  1. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  3. ^ "13 Tri -- Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2013-10-13.
  4. ^ Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14,000 F and G dwarfs", Astronomy and Astrophysics, 418 (3): 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
  5. ^ Takeda, Yoichi (April 2007), "Fundamental Parameters and Elemental Abundances of 160 F-G-K Stars Based on OAO Spectrum Database", Publications of the Astronomical Society of Japan, 59 (2): 335–356, Bibcode:2007PASJ...59..335T, doi:10.1093/pasj/59.2.335.
  6. ^ Maldonado, J.; et al. (May 2012). "Metallicity of solar-type stars with debris discs and planets". Astronomy & Astrophysics. 541: A40. arXiv:1202.5884. Bibcode:2012A&A...541A..40M. doi:10.1051/0004-6361/201218800. S2CID 46328823.
  7. ^ Takeda, Yoichi; et al. (February 2005), "High-Dispersion Spectra Collection of Nearby F--K Stars at Okayama Astrophysical Observatory: A Basis for Spectroscopic Abundance Standards", Publications of the Astronomical Society of Japan, 57 (1): 13–25, Bibcode:2005PASJ...57...13T, doi:10.1093/pasj/57.1.13.
  8. ^ "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.
  9. ^ van Belle, G. T.; et al. (May 2008). "The Palomar Testbed Interferometer Calibrator Catalog". The Astrophysical Journal Supplement Series. 176 (1): 276–292. arXiv:0711.4194. Bibcode:2008ApJS..176..276V. doi:10.1086/526548. S2CID 10713221.
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