17 Vulpeculae

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17 Vulpeculae
Observation data
Epoch J2000      Equinox J2000
Constellation Vulpecula
Right ascension 20h 06m 53.40787s[1]
Declination +23° 36′ 51.9294″[1]
Apparent magnitude (V) 5.08[2]
Spectral type B3 V[3]
B−V color index −0.162±0.002[2]
Radial velocity (Rv) −7.6±0.8[4] km/s
Proper motion (μ) RA: +15.59[1] mas/yr
Dec.: +0.31[1] mas/yr
Parallax (π) 6.47 ± 0.27[1] mas
Distance 500 ± 20 ly
(155 ± 6 pc)
Absolute magnitude (MV) −0.86[2]
Mass 6.1±0.1[5] M
Radius 3.9[6] R
Luminosity 573.30[2] L
Temperature 15,648[7] K
Metallicity [Fe/H] −0.14±0.04[2] dex
Rotational velocity (v sin i) 115[8] km/s
Age 10.7±1.9[5] Myr
Other designations
17 Vul, BD+23° 3896, FK5 3611, HD 190993, HIP 99080, HR 7688, SAO 88212[9]
Database references

17 Vulpeculae is a single,[10] blue-white hued star in the northern constellation of Vulpecula. The distance to this star can be estimated from its annual parallax shift of 6.47±0.27,[1] which yields a separation of roughly 500 light years. It is moving nearer with a heliocentric radial velocity of −8 km/s,[4] and will make its closest approach in around 6.1 million years at a distance of about 419 ly (128.36 pc).[2] The star is faintly visible to the naked eye with an apparent visual magnitude of 5.08.[2]

This is an ordinary B-type main-sequence star with a stellar classification of B3 V.[3] It is just 11[5] million years old with a high projected rotational velocity of 115 km/s.[8] The star has an estimated 6.1[5] times the mass of the Sun and around 3.9[6] times the Sun's radius. It is radiating 573[2] times the Sun's luminosity from its photosphere at an effective temperature of 15,648 K.[7]


  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d e f g h Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971Freely accessible, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015. 
  3. ^ a b Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement, 17: 371, Bibcode:1968ApJS...17..371L, doi:10.1086/190179. 
  4. ^ a b Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053Freely accessible, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065. 
  5. ^ a b c d Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883Freely accessible, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x. 
  6. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics (3rd ed.), 367 (2): 521–524, arXiv:astro-ph/0012289Freely accessible, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451. 
  7. ^ a b McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037Freely accessible, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x 
  8. ^ a b Strom, Stephen E.; et al. (2005), "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?", The Astronomical Journal, 129 (2): 809–828, arXiv:astro-ph/0410337Freely accessible, Bibcode:2005AJ....129..809S, doi:10.1086/426748. 
  9. ^ "17 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-04-21. 
  10. ^ 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:0806.2878Freely accessible, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x.