14 Trianguli

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14 Trianguli
Triangulum constellation map.svg
Red circle.svg
Location of 14 Trianguli (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
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  mas/yr [1]
Dec.: +11.901  mas/yr [1]
Parallax (π)7.5319 ± 0.1060  mas [1]
Distance 433 ± 6  ly
(133 ± 2  pc)
Absolute magnitude  (MV)−0.46 [6]
Orbit [7]
Primary14 Tri A
Companion14 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 38.66±1.18 [9]   R☉
Luminosity 325±17 [9]   L☉
Surface gravity (log g)1.65 [10]   cgs
Temperature 3,991 [9]   K
Metallicity [Fe/H]−0.16 [11]   dex
Rotational velocity (v sin i)2.1±1.2 [12]  km/s
Other designations
14 Trianguli, AG+35°233, BD+35°497, FK5  1070, GC  3032, HD  15656, HIP  11784, HR  736, SAO  55635 [13]
Database references
SIMBAD data

14 Trianguli (14 Tri), also known as HD 15656, is a spectroscopic binary [14] 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. [15] 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 39 times its girth. It radiates 325 times the luminosity of the Sun from its photosphere at an effective temperature of 3,991  K , [9] giving it an orangish-red hue. 14 Tri is slightly metal-deficient with [Fe/H] = −0.16, [11] and spins modestly with a projected rotational velocity of 2.1  km/s . [12] 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. [16]

Related Research Articles

<span class="mw-page-title-main">Beta Trianguli</span> Binary star in the constellation Triangulum

Beta Trianguli is the Bayer designation for a binary star system in the constellation Triangulum, located about 127 light years from Earth. Although it is only a third-magnitude star, it is the brightest star in the constellation Triangulum.

μ1 Chamaeleontis, Latinized as Mu1 Chamaeleontis, is a single star in the southern circumpolar constellation Chamaeleon. It is dimly visible to the naked eye with an apparent visual magnitude of 5.53. Based upon parallax measurements, it is located approximately 403 light-years away from the Sun. The radial velocity is poorly constrained, but it appears to be drifting further away at the rate of about 16 km/s

Kappa<sup>2</sup> Coronae Australis Star in the constellation Corona Australis

Kappa2 Coronae Australis, Latinized from κ2 Coronae Australis, is the primary of a probable binary system located in the southern constellation Corona Australis. It is visible to the naked eye as a bluish-white hued star with an apparent visual magnitude of 5.59. The distance to this star is roughly 710 light years based on Gaia DR3 parallax measurements. The radial velocity is poorly constrained, but the star appears to be moving closer with a radial velocity of around −15 km/s. At its current distance, Kappa2 CrA's brightness is diminished by 0.45 magnitudes due to interstellar dust.

<span class="mw-page-title-main">Q Scorpii</span> High proper motion binary star system in the constellation of Scorpius

Q Scorpii, also designated as HD 159433, is an astrometric binary located in the southern zodiac constellation Scorpius. It has an apparent magnitude of 4.27, making it readily visible to the naked eye under ideal conditions. It lies in the tail of Scorpius, between the stars λ Scorpii and μ Scorpii and is located 7′ away from the faint globular cluster Tonantzintla 2. Based on parallax measurements from Gaia DR3, the system is estimated to be 158 light years distant, but is approaching the Solar System with a heliocentric radial velocity of −49 km/s.

HD 63399 is an orange hued star located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 6.45, placing it near the limit for naked eye visibility. Based on parallax measurements from Gaia DR3, the object is estimated to be 445 light years distant. It appears to be receding with a spectroscopic radial velocity of 28.5 km/s. At its current distance, HD 63399 is diminished by 0.29 magnitudes due to interstellar dust.

<span class="mw-page-title-main">2 Piscis Austrini</span> Star in the constellation Microscopium

2 Piscis Austrini, also known as HD 200763 or simply 2 PsA, is a solitary orange hued star located in the southern constellation Microscopium. It was once part of Piscis Austrinus, the southern fish. The object has an apparent magnitude of 5.2, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia satellite, it is estimated to be 354 light years away from the Solar System. However, it is receding with a poorly constrained heliocentric radial velocity of 3.1 km/s. At its current distance, 2 PsA's brightness is diminished by 0.11 magnitudes due to interstellar dust. It has an absolute magnitude of 0.19.

<span class="mw-page-title-main">3 Piscis Austrini</span> Star in the constellation Microscopium

3 Piscis Austrini, also known as HD 201901 or simply 3 PsA, is an astrometric binary located in the southern constellation Microscopium. It was once part of Piscis Austrinus, the southern fish. The system has a combined apparent magnitude of 5.39, making it faintly visible to the naked eye under ideal conditions. Gaia DR3 parallax measurements imply a distance of 404 light years and it is currently approaching the Solar System with a heliocentric radial velocity of −46.2 km/s. At its current distance, 3 PsA's brightness is diminished by 0.12 magnitudes due to extinction from interstellar dust and it has an absolute magnitude of +0.19.

HD 138867, also known as HR 5786, is a bluish-white hued star located in the southern circumpolar constellation Apus. It has an apparent magnitude of 5.94, making it faintly visible to the naked eye if viewed under ideal conditions. Based on parallax measurements from the Gaia spacecraft, it is estimated to be 417 light years away from Earth. However, it is receding with a heliocentric radial velocity of 1.1 km/s.

<span class="mw-page-title-main">10 Trianguli</span> Star in the constellation Triangulum

10 Trianguli, or simply 10 Tri is a solitary star located in the northern constellation Triangulum. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.29. Gaia DR3 parallax measurements imply a distance of 363 light-years and it is slowly receding with a heliocentric radial velocity of 0.4 km/s. At its current distance, 10 Tri's brightness is diminished by an interstellar extinction of 0.11 magnitudes and it has an absolute magnitude of −0.02.

HD 89571 is a binary star located in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye with a combined apparent magnitude of 5.51 and is estimated to be 142 light years away from the Solar System. However, it is receding with a heliocentric radial velocity of 3.5 km/s.

HD 10800, also known as HR 512 or Gliese 67.1, is a triple star located in the southern circumpolar constellation Octans. It has a combined apparent magnitude of 5.87, allowing it to be faintly seen with the naked eye. The system is relatively close at a distance of 88.1 light years but is drifting closer with a heliocentric radial velocity −1.1 km/s.

HD 208741, also known as HR 8380, is a yellowish-white hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.91, making it faintly visible to the naked eye. Parallax measurements place it at a distance of 211 light years, and it is currently receding with a heliocentric radial velocity of 8 km/s.

HD 183552, also known as HR 7411, is a probable spectroscopic binary located in the southern constellation Telescopium. The system has a combined apparent magnitude of 5.74, allowing it to be faintly visible to the naked eye. Based on parallax measurements from the Gaia spacecraft, it is estimated to be 337 light years distant. The value is horribly constrained, but it appears to receding with a radial velocity of 14 km/s.

HD 34255, also known HR 1720, is a star located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.60, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of about 1.65 kly but is approaching the Solar System with a heliocentric radial velocity of −7.7 km/s.

HD 43899, also designated as HR 2263, is a solitary, orange hued star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.53, allowing it to be faintly visible to the naked eye. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 284 light years distant. It appears to be rapidly receding with a heliocentric radial velocity of 66.5 km/s. Eggen (1993) lists HD 43899 as an old disk star and its kinematics match with that of the ζ Herculis moving group.

<span class="mw-page-title-main">8 Leonis Minoris</span> Star in the constellation of Leo Minor

8 Leonis Minoris is a solitary, red hued star located in the northern constellation Leo Minor. It has an apparent magnitude 5.37, making it faintly visible to the naked eye. Based on parallax measurements from the Gaia satellite, the object is estimated to be 492 light years distant. It is receding with a heliocentric radial velocity of 40 km/s. At its current distance, 8 LMi is diminshed by 0.12 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 201772</span> Star in the constellation Microscopium

HD 201772, also known as HR 8104, is a yellowish-white hued star located in the southern constellation Microscopium. It has an apparent magnitude of 5.26, making it one of the brighter members of this generally faint constellation. The object is located relatively close at a distance of 111 light-years based on Gaia DR3 parallax measurements but is approaching closer with a heliocentric radial velocity of −41 km/s. At its current distance, HD 201772's brightness is diminished by 0.11 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 26755</span> Binary star system in Camelopardalis

HD 26755, also known as HR 1313, is a spectroscopic binary located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.72, making it faintly visible to the naked eye under ideal conditions. Gaia DR3 parallax measurements place the system at a distance of 271 light years and is currently drifitng closer with a heliocentric radial velocity of −38 km/s. At its current distance, HD 26755's brightness is diminished by 0.19 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 22764</span> Double star; Camelopardalis

HD 22764, also known as HR 1112, is an orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.78, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of approximately 1,770 light years based on Gaia DR3 parallax measurements but is approaching the Solar System with a heliocentric radial velocity of −12.5 km/s. At its current distance, HD 22764's brightness is diminished by 0.66 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 197630</span> Star in the constellation of Microscopium

HD 197630, also known as HR 7933 or rarely 23 G. Microscopii, is a probable astrometric binary located in the southern constellation Microscopium. The visible component is a bluish-white hued star that is faintly visible to the naked eye with an apparent magnitude of 5.47. Based on parallax measurements from the Gaia satellite, the system is estimated to be 328 light years away. However, it is drifting closer with a heliocentric radial velocity of −30 km/s. At its current distance, HD 197630's brightness is diminished by 0.11 magnitudes due to interstellar dust. A 2012 multiplicity survey failed to confirm the velocity variations.

References

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  2. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361.
  3. ↑ Roman, Nancy G. (July 1952). "The Spectra of the Bright Stars of Types F5-K5". The Astrophysical Journal. 116: 122. Bibcode:1952ApJ...116..122R. doi: 10.1086/145598 . eISSN   1538-4357. ISSN   0004-637X.
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  5. 1 2 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. arXiv: astro-ph/0409579 . Bibcode:2005A&A...430..165F. doi: 10.1051/0004-6361:20041272 . eISSN   1432-0746. ISSN   0004-6361. S2CID   17804304.
  6. 1 2 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN   1562-6873. ISSN   1063-7737. S2CID   119257644.
  7. 1 2 Griffin, R. F. (1994). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 117: 14 Trianguli". The Observatory. 114: 167. Bibcode:1994Obs...114..167G.
  8. 1 2 Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (21 December 2021). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics. 657: A7. arXiv: 2109.10912 . Bibcode:2022A&A...657A...7K. doi: 10.1051/0004-6361/202142146 . eISSN   1432-0746. ISSN   0004-6361.
  9. 1 2 3 4 van Belle, Gerard T.; von Braun, Kaspar; Ciardi, David R.; Pilyavsky, Genady; Buckingham, Ryan S.; Boden, Andrew F.; Clark, Catherine A.; Hartman, Zachary; van Belle, Gerald; Bucknew, William; Cole, Gary (2021-12-01). "Direct Measurements of Giant Star Effective Temperatures and Linear Radii: Calibration against Spectral Types and V - K Color". The Astrophysical Journal. 922 (2): 163. arXiv: 2107.09205 . Bibcode:2021ApJ...922..163V. doi: 10.3847/1538-4357/ac1687 . ISSN   0004-637X. 14 Trianguli's database entry at VizieR.
  10. ↑ Maas, Z. G.; Pilachowski, C. A.; Hinkle, K. (28 November 2016). "Chlorine Abundances in Cool Stars". The Astronomical Journal. 152 (6): 196. arXiv: 1609.01626 . Bibcode:2016AJ....152..196M. doi: 10.3847/0004-6256/152/6/196 . eISSN   1538-3881.
  11. 1 2 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. Bibcode:1990ApJS...74.1075M. doi: 10.1086/191527 . eISSN   1538-4365. ISSN   0067-0049.
  12. 1 2 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. Bibcode:1999A&AS..139..433D. doi: 10.1051/aas:1999401 . eISSN   1286-4846. ISSN   0365-0138.
  13. ↑ "*14 Tri". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved February 8, 2023.
  14. ↑ 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. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x . eISSN   1365-2966. ISSN   0035-8711. S2CID   14878976.
  15. ↑ 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. arXiv: 1709.01160 . Bibcode:2017MNRAS.472.3805G. doi: 10.1093/mnras/stx2219 . eISSN   1365-2966. ISSN   0035-8711.
  16. ↑ 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. Bibcode:1983MNRAS.204..841M. doi: 10.1093/mnras/204.3.841 . eISSN   1365-2966. ISSN   0035-8711.

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