14 Vulpeculae

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14 Vulpeculae
Vulpecula IAU.svg
Red circle.svg
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]
Distance 174 ± 2  ly
(53.3 ± 0.5  pc)
Absolute magnitude  (MV)2.23 [2]
Details
Mass 1.52 [5]   M☉
Luminosity 11.09 [2]   L☉
Surface gravity (log g)3.81±0.14 [5]   cgs
Temperature 6,938±236 [5]   K
Metallicity [Fe/H]−0.36 [4]   dex
Rotational velocity (v sin i)150 [6]  km/s
Age 1.743 [5]   Gyr
Other designations
14 Vul, BD+22° 3872, HD  189410, HIP  98375, HR  7641, SAO  88016 [7]
Database references
SIMBAD data

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]

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ν Tauri, Latinized as Nu Tauri, is a single star in the zodiac constellation of Taurus. It is a white-hued star and is visible to the naked eye with an apparent visual magnitude of +3.91. This object is located 117 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −6 km/s. It is predicted to come to within roughly 18.4 ly of the Sun in around five million years.

23 Andromedae, abbreviated 23 And, is a presumed single star in the constellation Andromeda, although it has been a suspected spectroscopic binary. 23 Andromedae is the Flamsteed designation. Its apparent visual magnitude is 5.71, which indicates it is dimly visible to the naked eye under good viewing conditions. The distance to 23 And, as determined from its annual parallax shift of 26.8 mas, is 121.6 light years. The star is moving further from the Earth with a heliocentric radial velocity of −27 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.191″ per year.

4 Arietis is a single star in the northern constellation of Aries, the ram. 4 Arietis is the Flamsteed designation. It is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of 5.86. The star has an annual parallax shift of 11.46±0.15 mas, which is equivalent to a distance of 285 light-years from the Sun. It is moving further from the Earth with a heliocentric radial velocity of +6 km/s.

<span class="mw-page-title-main">23 Vulpeculae</span> Star in the constellation Vulpecula

23 Vulpeculae is a triple star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.52 and it is located approximately 327 light years away from the Sun based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +1.47 km/s.

<span class="mw-page-title-main">29 Vulpeculae</span> Binary star system in the constellation Vulpecula

29 Vulpeculae is a suspected astrometric binary star system in the northern constellation Vulpecula. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.82. The system lies approximately 209 light years away from the Sun based on parallax, and is a member of the IC 2391 supercluster. It is moving closer to the Earth with a heliocentric radial velocity of −17 km/s.

<span class="mw-page-title-main">12 Vulpeculae</span> Star in the constellation Vulpecula

12 Vulpeculae is a star in the northern constellation of Vulpecula, located approximately 630 light years away based on parallax. It has the variable star designation V395 Vul; 12 Vulpeculae is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 4.928. It is moving closer to the Earth with a heliocentric radial velocity of -25 km/s.

<span class="mw-page-title-main">9 Vulpeculae</span> Star in the constellation Vulpecula

9 Vulpeculae is a star in the northern constellation of Vulpecula, located about 560 light years away based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.01. The star is moving further from the Earth with a heliocentric radial velocity of +5 km/s.

17 Vulpeculae is a single, blue-white hued star in the northern constellation of Vulpecula. The distance to this star can be estimated from its annual parallax shift of 6.8168±0.1430, which yields a separation of roughly 480 light years. It is moving nearer with a heliocentric radial velocity of −8 km/s, and will make its closest approach in around 6.1 million years at a distance of about 419 ly (128.36 pc). The star is faintly visible to the naked eye with an apparent visual magnitude of 5.08.

16 Lyrae is a suspected astrometric binary star system in the constellation Lyra, located 126 light years away from the Sun based on parallax. It is visible to the naked eye as a dim, white-hued star with a combined apparent visual magnitude of 5.00. The system is moving further away from the Earth with a heliocentric radial velocity of +5 km/s. It is a suspected member of the Ursa Major Moving Group stream.

4 Vulpeculae is a single, orange-hued star in the northern constellation of Vulpecula. It forms part of the asterism, formerly thought to be an open cluster, called the coathanger or Brocchi's Cluster. The star is faintly visible to the naked eye with an apparent visual magnitude of 5.16. The distance to this star, based upon an annual parallax shift of 12.5320±0.1008 mas, is around 260 light years.

<span class="mw-page-title-main">21 Vulpeculae</span> Star in the constellation Vulpecula

21 Vulpeculae is a single, white-hued star in the northern constellation of Vulpecula. Its distance can be estimated from the annual parallax shift of 10.4302±0.0696 mas, yielding a separation of 313 light years. The star is faintly visible to the naked eye at night, having an apparent visual magnitude of 5.19. It is moving further away with a heliocentric radial velocity of about +7 km/s, having come within 243 ly (74.53 pc) around 4.2 million years ago.

16 Vulpeculae is a binary star system in the northern constellation Vulpecula. It has a combined apparent visual magnitude of 5.787, which is near the lower limit of visibility to the naked eye. Based upon an annual parallax shift of 14.71±0.50 as seen from Earth's orbit, it is located about 222 light years away. The system is moving closer to the Sun with a heliocentric radial velocity of about −37 km/s. It will make its closest approach in about 0.9 million years, coming within 155 light-years (47.42 pc).

24 Vulpeculae is a single, yellow-hued star in the northern constellation of Vulpecula. It is faintly visible to the naked eye with an apparent visual magnitude of 5.30. The distance to this star can be estimated from its annual parallax shift of 7.9700±0.0674, which yields a separation of roughly 409 light years. It is moving further away with a heliocentric radial velocity of +15 km/s.

35 Vulpeculae is a single, white-hued star in the northern constellation of Vulpecula. It is faintly visible to the naked eye with an apparent visual magnitude of 5.39. An annual parallax shift of 16.9162±0.0681 mas provides a distance estimate of about 193 light years. It is moving closer with a heliocentric radial velocity of −8 km/s.

<span class="mw-page-title-main">5 Vulpeculae</span> Star in the constellation Vulpecula

5 Vulpeculae is a single, white-hued star in the northern constellation of Vulpecula. It is situated amidst a random concentration of bright stars designated Collinder 399, or Brocchi's Cluster. This is a faint star that is just visible to the naked eye with an apparent visual magnitude of 5.60. Based upon an annual parallax shift of 13.8921±0.0900 mas, it is located around 235 light years from the Sun. It is moving closer with a heliocentric radial velocity of −21 km/s, and will make its closest approach in 2.5 million years at a separation of around 120 ly (36.89 pc).

<span class="mw-page-title-main">27 Vulpeculae</span> Star in the constellation Vulpecula

27 Vulpeculae is a single, blue-white star in the northern constellation of Vulpecula. It is a dim star, visible to the naked eye, with an apparent visual magnitude of 5.59. An annual parallax shift of 10.6692±0.0483 mas provides a distance estimate of about 306 light-years. It is moving closer with a heliocentric radial velocity of −22 km/s, and will make perihelion passage at a distance of around 119 ly (36.56 pc) in 3.75 million years.

16 Comae Berenices is a single star in the northern constellation of Coma Berenices. 16 Comae Berenices is the Flamsteed designation. It is a member of the Coma Star Cluster and is visible to the naked eye with an apparent visual magnitude of 4.96. Based upon an annual parallax shift of 11.7 mas, it is located about 279 light years away.

57 Persei, or m Persei, is a suspected triple star system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08. The annual parallax shift of 16.4 mas provides a distance measure of 199 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23 km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).

59 Persei is a suspected astrometric binary star system in the northern constellation of Perseus. It is visible to the naked eye as a dim, white-hued star with an apparent magnitude of 5.30. The star is located around 256 light years distant from the Sun, based on parallax, and is drifting further away with a radial velocity of +13 km/s.

<span class="mw-page-title-main">BW Vulpeculae</span> Star in the constellation Vulpecula

BW Vulpeculae or BW Vul, is a variable star in the northern constellation of Vulpecula. It is near the lower limit of visibility to the naked eye with a typical apparent visual magnitude of 6.54. Based on an annual parallax shift of 1.15 mas, the distance to BW Vul is about 2,800 light years. It is moving closer to the Earth with a baseline heliocentric radial velocity of around −6 km/s.

References

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  4. 1 2 3 4 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, S2CID   56118016.
  5. 1 2 3 4 5 6 7 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, S2CID   33401607.
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  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 , S2CID   14878976.
  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, S2CID   8562211.
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