13 Trianguli
13 Trianguli is the Flamsteed designation for a star in the northern constellation of Triangulum. It has an apparent visual magnitude of 5.86,[2] so according to the Bortle scale it is faintly visible from dark suburban skies. Measurements made with the Hipparcos spacecraft show an annual parallax shift of 0.03184″,[1] which is equivalent to a distance of around 102 ly (31 pc) from the Sun.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Triangulum |
| Right ascension | 02h 28m 48.49387s[1] |
| Declination | +29° 55′ 54.3315″[1] |
| Apparent magnitude (V) | 5.86[2] |
| Characteristics | |
| Spectral type | G0 V[1] |
| U−B color index | +0.01[2] |
| B−V color index | +0.58[2] |
| Astrometry | |
| Radial velocity (Rv) | +40.8[3] km/s |
| Proper motion (μ) | RA: –66.53[1] mas/yr Dec.: +71.93[1] mas/yr |
| Parallax (π) | 31.84 ± 0.40[1] mas |
| Distance | 102 ± 1 ly (31.4 ± 0.4 pc) |
| Absolute magnitude (MV) | 3.45[4] |
| Details | |
| Mass | 1.10 ± 0.03[4] M☉ |
| Luminosity | 3.72[4] L☉ |
| Temperature | 5,846[4] K |
| Metallicity [Fe/H] | –0.24[5] dex |
| Rotational velocity (v sin i) | 3[6] km/s |
| Age | 6.45[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
A stellar classification of G0 V[1] 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 and shines with 3.72 times the luminosity of the Sun. The stellar atmosphere has an effective temperature of 5,846[4] K, giving it the yellow hue of a G-type star.[7] It appears to be older than the Sun, with an estimated age of 6.45 billion years.[4]
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.[8] 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.[5]
References
- van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
- "13 Tri -- Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2013-10-13.
- 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.
- 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.
- 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.
- 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.
- "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 10, 2012, retrieved 2012-01-16.
- 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.