Astronomy:14 Trianguli
Observation data Epoch J2000.0 Equinox (celestial coordinates) | |
---|---|
Constellation | Triangulum |
Right ascension | 02h 32m 06.16977s[1] |
Declination | +36° 08′ 50.1813″[1] |
Apparent magnitude (V) | 5.14±0.01[2] |
Characteristics | |
Spectral type | K5 III[3] |
U−B color index | +1.78[4] |
B−V color index | +1.47[4] |
Astrometry | |
Radial velocity (Rv) | −36.8±0.3[5] km/s |
Proper motion (μ) | RA: +45.066[1] mas/yr Dec.: +11.901[1] mas/yr |
Parallax (π) | 7.5319 ± 0.1060[1] mas |
Distance | 433 ± 6 ly (133 ± 2 pc) |
Absolute magnitude (MV) | −0.46[6] |
Orbit[7] | |
Primary | 14 Tri A |
Companion | 14 Tri B |
Period (P) | 6,257±73 d |
Eccentricity (e) | 0.22±0.04 |
Periastron epoch (T) | 2,448,284±166 JD |
Argument of periastron (ω) (secondary) | 40±11° |
Semi-amplitude (K1) (primary) | 2.27±0.09 km/s |
Details | |
Mass | 1.85±0.09[8] M☉ |
Radius | 40.5±2.1[9] R☉ |
Luminosity | 373±11[10] L☉ |
Surface gravity (log g) | 1.65[11] cgs |
Temperature | 3,957[12] K |
Metallicity [Fe/H] | −0.16[13] dex |
Rotational velocity (v sin i) | 2.1±1.2[14] km/s |
Other designations | |
Database references | |
SIMBAD | data |
14 Trianguli (14 Tri), also known as HD 15656, is a spectroscopic binary[16] located in the northern constellation Triangulum. It has an apparent magnitude of 5.14,[2] making it faintly visible to the naked eye in ideal conditions. Gaia DR3 parallax measurements place the system 433 light years away,[1] and it is currently approaching the Solar System with a heliocentric radial velocity of −37 km/s.[5] At its current distance, 14 Tri's brightness is diminished by 0.21 magnitude due to interstellar dust.[17] It has an absolute magnitude of −0.46.[6]
The visible component is an evolved red giant with a stellar classification of K5 III. It has 1.85 times the mass of the Sun,[8] but it has expanded to 40.5 times its girth.[9] It radiates 373 times the luminosity of the Sun[10] from its photosphere at an effective temperature of 3,957 K,[12] giving it an orangish-red hue. 14 Tri is slightly metal-deficient with [Fe/H] = −0.16,[13] and spins modestly with a projected rotational velocity of 2.1 km/s.[14] This is a single-lined spectroscopic binary that completes an eccentric orbit within 17 years. The secondary star has not been detected visually or in the spectrum and is expected to be a low-mass red dwarf or white dwarf.[7] 14 Tri may be part of the Wolf 630 moving group.[18]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H.
- ↑ Roman, Nancy G. (July 1952). "The Spectra of the Bright Stars of Types F5-K5.". The Astrophysical Journal 116: 122. doi:10.1086/145598. ISSN 0004-637X. Bibcode: 1952ApJ...116..122R.
- ↑ 4.0 4.1 Argue, A. N. (1 September 1966). "UBV Photometry of 550 F, G and K Type Stars". Monthly Notices of the Royal Astronomical Society 133 (4): 475–493. doi:10.1093/mnras/133.4.475. ISSN 0035-8711. Bibcode: 1966MNRAS.133..475A.
- ↑ 5.0 5.1 Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (January 2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics 430: 165–186. doi:10.1051/0004-6361:20041272. ISSN 0004-6361. Bibcode: 2005A&A...430..165F.
- ↑ 6.0 6.1 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A.
- ↑ 7.0 7.1 Griffin, R. F. (1994). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 117: 14 Trianguli". The Observatory 114: 167. Bibcode: 1994Obs...114..167G.
- ↑ 8.0 8.1 Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (21 December 2021). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics 657: A7. doi:10.1051/0004-6361/202142146. ISSN 0004-6361. Bibcode: 2022A&A...657A...7K.
- ↑ 9.0 9.1 Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (October 2004). "The angular sizes of dwarf stars and subgiants". Astronomy & Astrophysics 426 (1): 297–307. doi:10.1051/0004-6361:20035930. ISSN 0004-6361. Bibcode: 2004A&A...426..297K.
- ↑ 10.0 10.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ Maas, Z. G.; Pilachowski, C. A.; Hinkle, K. (28 November 2016). "Chlorine Abundances in Cool Stars". The Astronomical Journal 152 (6): 196. doi:10.3847/0004-6256/152/6/196. Bibcode: 2016AJ....152..196M.
- ↑ 12.0 12.1 di Benedetto, G. P. (November 1998). "Towards a fundamental calibration of stellar parameters of A, F, G, K dwarfs and giants". Astronomy and Astrophysics 339: 858–871. ISSN 0004-6361. Bibcode: 1998A&A...339..858D.
- ↑ 13.0 13.1 McWilliam, Andrew (December 1990). "High-resolution spectroscopic survey of 671 GK giants. I - Stellar atmosphere parameters and abundances". The Astrophysical Journal Supplement Series 74: 1075. doi:10.1086/191527. ISSN 0067-0049. Bibcode: 1990ApJS...74.1075M.
- ↑ 14.0 14.1 de Medeiros, J. R.; Mayor, M. (November 1999). "A catalog of rotational and radial velocities for evolvedstars". Astronomy and Astrophysics Supplement Series 139 (3): 433–460. doi:10.1051/aas:1999401. ISSN 0365-0138. Bibcode: 1999A&AS..139..433D.
- ↑ "*14 Tri". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A14+Tri.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (11 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. ISSN 0035-8711. Bibcode: 2008MNRAS.389..869E.
- ↑ Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017). "Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars". Monthly Notices of the Royal Astronomical Society 472 (4): 3805–3820. doi:10.1093/mnras/stx2219. ISSN 0035-8711. Bibcode: 2017MNRAS.472.3805G.
- ↑ McDonald, A. R. E.; Hearnshaw, J. B. (1 October 1983). "The Wolf 630 moving group of stars". Monthly Notices of the Royal Astronomical Society 204 (3): 841–852. doi:10.1093/mnras/204.3.841. ISSN 0035-8711. Bibcode: 1983MNRAS.204..841M.
Further reading
- Griffin, R.F. (August 1994). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 117: 14 Trianguli.". The Observatory 114: 167–171. Bibcode: 1994Obs...114..167G.
Original source: https://en.wikipedia.org/wiki/14 Trianguli.
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