14 Andromedae

14 Andromedae, abbreviated 14 And, also named Veritate /ˌvɛrɪˈteɪtiː/,[7] is a single,[8] orange-hued giant star situated approximately 247 light-years away[1] in the northern constellation of Andromeda. It is dimly visible to the naked eye with an apparent visual magnitude of 5.22.[2] The star is moving closer to the Earth with a heliocentric radial velocity of −60 km/s.[2] In 2008 an extrasolar planet (designated 14 Andromedae b, later named Spe) was discovered to be orbiting the star.[3]

14 Andromedae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Andromeda
Right ascension  23h 31m 17.41273s[1]
Declination +39° 14′ 10.3105″[1]
Apparent magnitude (V) 5.22[2]
Characteristics
Spectral type K0 III[3]
B−V color index 1.029±0.003[2]
Variable type None[4]
Astrometry
Radial velocity (Rv)−59.99±0.20[2] km/s
Proper motion (μ) RA: 287.292[1] mas/yr
Dec.: -83.758[1] mas/yr
Parallax (π)13.2289 ± 0.1245[1] mas
Distance247 ± 2 ly
(75.6 ± 0.7 pc)
Absolute magnitude (MV)0.73[2]
Details[5]
Mass1.12±0.24 or 2.2[3] M☉
Radius10.49±0.51 R☉
Luminosity60.3+12.1
−10.2 L☉
Surface gravity (log g)2.60±0.01 cgs
Temperature4,743±31 K
Metallicity [Fe/H]−0.30±0.04 dex
Rotational velocity (v sin i)1.63±0.47 km/s
Age4.96±2.84 Gyr
Other designations
Veritate, 14 And, NSV 14599, BD+38° 5023, GC 32703, HD 221345, HIP 116076, HR 8930, SAO 73311, 2MASS J23311742+3914102[6]
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

This is a red clump[9] giant with a stellar classification of K0 III,[3] indicating it is on the horizontal branch and is generating energy through helium fusion at its core. The star has 1.12[5] (or 2.2[3]) times the mass of the Sun and has expanded to 10.5 times the Sun's radius. It is radiating 60.3 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,743 K.[5] This is thought it was formerly an A- or F-type main-sequence star earlier in its life, prior to evolving into a giant.

Nomenclature

14 Andromedae is the star's Flamsteed designation. Following its discovery the planet was designated 14 Andromedae b.

In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars.[10] The process involved public nomination and voting for the new names.[11] In December 2015, the IAU announced the winning names were Veritate for this star and Spe for its planet.[12]

The winning names were based on those submitted by the Thunder Bay Centre of the Royal Astronomical Society of Canada[13]); namely 'Veritas' and 'Spes', Latin for 'truth' and 'hope', respectively. (Veritas was also the Roman goddess of truth and Spes was the Roman goddess of hope.) The IAU substituted the ablative forms 'Veritate' and 'Spe', which mean 'where there is truth' and 'where there is hope', respectively. This was because 'Veritas' is the name of an asteroid important for the study of the solar system.[14]

In 2016, the IAU organized a Working Group on Star Names (WGSN)[15] to catalog and standardize proper names for stars. In its first bulletin of July 2016,[16] the WGSN explicitly recognized the names of exoplanets and their host stars approved by the Executive Committee Working Group Public Naming of Planets and Planetary Satellites, including the names of stars adopted during the 2015 NameExoWorlds campaign. This star is now so entered in the IAU Catalog of Star Names.[7]

Planetary system

In 2008, a planet was announced to be orbiting the star. The planet was found to have a minimum mass of 4.8 Jupiter masses and orbiting in a circular orbit that takes 186 days to complete. The planet is one of the few known planets to be orbiting an evolved intermediate-mass star and one of the innermost (such planets have only been discovered in clump giants).[3]

The 14 Andromedae planetary system[17]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (Spe) >5.33 ± 0.57 MJ 0.83[3] 185.84 ± 0.23 0 — —
gollark: Right now mesh networking is still quite early in its life and I don't think many of the problems have been worked out entirely yet.
gollark: They might be able to be once the stuff develops better and people work out exactly what works best.
gollark: I don't think you could make stuff compatible enough that you wouldn't need any intermediaries without it just essentially using the same networking stack.
gollark: The main issue, I think, is that they don't really work similarly at a *routing* level.
gollark: They don't need to be on the same frequency or anything, you could just have a device with multiple transceivers.

See also

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.
  3. Sato, Bun'ei; et al. (2008). "Planetary Companions to Evolved Intermediate-Mass Stars: 14 Andromedae, 81 Ceti, 6 Lyncis, and HD167042". Publications of the Astronomical Society of Japan. 60 (6): 1317–1326. arXiv:0807.0268. Bibcode:2008PASJ...60.1317S. doi:10.1093/pasj/60.6.1317.
  4. Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017), "General catalogue of variable stars: Version GCVS 5.1", Astronomy Reports, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085.
  5. Jofré, E.; Petrucci, R.; Saffe, C.; Saker, L.; de la Villarmois, E. Artur; Chavero, C.; Gómez, M.; Mauas, P. J. D. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574: A50. arXiv:1410.6422. Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474.
  6. "14 And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved September 19, 2018.
  7. "IAU Catalog of Star Names". Retrieved 28 July 2016.
  8. 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.
  9. Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv:astro-ph/0003329, Bibcode:2000ApJ...539..732A, doi:10.1086/309278.
  10. NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
  11. NameExoWorlds The Process
  12. Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
  13. Thunder Bay Amateur Astronomers Name a Planet
  14. NameExoWorlds The Approved Names
  15. "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  16. "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  17. Ligi, R.; et al. (2012). "A new interferometric study of four exoplanet host stars : θ Cygni, 14 Andromedae, υ Andromedae and 42 Draconis". Astronomy and Astrophysics. 545. A5. arXiv:1208.3895. Bibcode:2012A&A...545A...5L. doi:10.1051/0004-6361/201219467.

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