Jump to content

14 Vulpeculae

From Wikipedia, the free encyclopedia

This is an old revision of this page, as edited by Mike s (talk | contribs) at 19:43, 15 December 2020 (update distance and replace ref). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.

14 Vulpeculae
Map of the constellation Vulpecula
14 Vul in the constellation Vulpecula (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Vulpecula
Right ascension 19h 59m 10.5367s[1]
Declination +23° 06′ 04.604″[1]
Apparent magnitude (V) 5.68[2]
Characteristics
Spectral type F1 Vn[3]
B−V color index 0.345±0.004[2]
Astrometry
Radial velocity (Rv)−38.0±3.7[4] km/s
Proper motion (μ) RA: −68.157±0.100[1] mas/yr
Dec.: 6.926±0.125[1] mas/yr
Parallax (π)18.7753 ± 0.1714 mas[1]
Distance174 ± 2 ly
(53.3 ± 0.5 pc)
Absolute magnitude (MV)2.23[2]
Details
Mass1.52[5] M
Luminosity11.09[2] L
Surface gravity (log g)3.81±0.14[5] cgs
Temperature6,938±236[5] K
Metallicity [Fe/H]−0.36[4] dex
Rotational velocity (v sin i)150[6] km/s
Age1.743[5] Gyr
Other designations
14 Vul, BD+22° 3872, HD 189410, HIP 98375, HR 7641, SAO 88016[7]
Database references
SIMBADdata

14 Vulpeculae is a single,[8] yellow-white hued star in the northern constellation of Vulpecula and proximate to the Dumbbell Nebula (M 27) on the celestial sphere, although actually much closer to the Earth.[9] It is a dim star that is faintly visible to the naked eye with an apparent visual magnitude of 5.68.[2] The distance to 14 Vul, as determined from its annual parallax shift of 18.7753±0.1714,[1] is around 174 light years. It is moving nearer with a heliocentric radial velocity of about −38 km/s,[4] and will make its closest approach in a million years when comes to within about 62 ly (19.04 pc).[2]

This is an F-type main-sequence star with a stellar classification of F1 Vn,[3] where the 'n' notation indicates nebulous lines due to rapid rotation. At the estimated age of 1.7[5] billion years old, it is spinning with a projected rotational velocity of 150[6] km/s and has sub-solar metallicity.[4] The star has 1.5[5] times the mass of the Sun and is radiating 11[2] times the Sun's luminosity from its photosphere at an effective temperature of about 6,938 K.[5]

References

  1. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. ^ a b c d e f g 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. ^ a b Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement, 99: 135, Bibcode:1995ApJS...99..135A, doi:10.1086/192182.
  4. ^ a b c d Casagrande, L.; et al. (2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy & Astrophysics, 530 (A138): 21, arXiv:1103.4651, Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276.
  5. ^ a b c d e f g David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146.
  6. ^ a b Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1), Bibcode:1970CoAsi.239....1B.
  7. ^ "14 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-04-13.
  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.{{citation}}: CS1 maint: unflagged free DOI (link)
  9. ^ Benedict, G. Fritz; McArthur, B. E.; Fredrick, L. W.; Harrison, T. E.; et al. (2003), "Astrometry with The Hubble Space Telescope: A Parallax of the Central Star of the Planetary Nebula NGC 6853", Astronomical Journal, 126 (5): 2549–2556, arXiv:astro-ph/0307449, Bibcode:2003AJ....126.2549B, doi:10.1086/378603.