19 Vulpeculae

19 Vulpeculae is star located approximately 1,690[1] light years from Earth in the northern constellation of Vulpecula.[9] It is a probable member of the open cluster NGC 6882.[4] This object is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.40.[2] It is moving closer to the Earth with a heliocentric radial velocity of −19 km/s.[4]

19 Vulpeculae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Vulpecula
Right ascension 20h 11m 47.9738s[1]
Declination 26° 48′ 32.3736″[1]
Apparent magnitude (V) 5.40[2]
Characteristics
Spectral type K2 IIIa[3]
B−V color index 1.40[4]
Astrometry
Radial velocity (Rv)−19.33±0.11[4] km/s
Proper motion (μ) RA: 1.619±0.119[1] mas/yr
Dec.: −10.600±0.122[1] mas/yr
Parallax (π)1.9328 ± 0.0779[1] mas
Distance1,690 ± 70 ly
(520 ± 20 pc)
Absolute magnitude (MV)−2.60[5]
Details
Mass4.94±0.53[6] M☉
Radius100.3+1.7
−3.0[1] R☉
Luminosity2,889±145[1] L☉
Surface gravity (log g)1.40[7] cgs
Temperature4,200[7] K
Metallicity [Fe/H]−0.01[7] dex
Rotational velocity (v sin i)< 3.4[8] km/s
Other designations
19 Vul, BD+26° 3825, HD 192004, HIP 99518, HR 7718, SAO 88330[9]
Database references
SIMBADdata

This is an aging giant star with a stellar classification of K2 IIIa,[3] having already consumed the hydrogen at its core and evolved away from the main sequence. It has nearly five[6] times the mass of the Sun but has expanded to around 100[1] times the Sun's radius. The star is radiating 2,889[1] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,200 K.[7]

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. Fernie, J. D. (1983). "New UBVRI photometry for 900 supergiants". Astrophysical Journal Supplement Series. 52: 7. Bibcode:1983ApJS...52....7F. doi:10.1086/190856.
  3. Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. Mermilliod, J. C.; et al. (2008). "Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters". Astronomy & Astrophysics. 485 (1): 303–314. Bibcode:2008A&A...485..303M. CiteSeerX 10.1.1.30.7545. doi:10.1051/0004-6361:200809664.
  5. 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.
  6. Hohle, M.M.; et al. (2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331 (4): 349. arXiv:1003.2335. Bibcode:2010AN....331..349H. doi:10.1002/asna.200911355.
  7. Luck, R. Earle (March 1994). "Open Cluster Chemical Composition. I. Later Type Stars in Eight Clusters". Astrophysical Journal Supplement. 91: 309. Bibcode:1994ApJS...91..309L. doi:10.1086/191940.
  8. De Medeiros, J. R.; et al. (November 2000). "Rotation and lithium in single giant stars". Astronomy and Astrophysics. 363: 239–243. arXiv:astro-ph/0010273. Bibcode:2000A&A...363..239D.
  9. "19 Vulpeculae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-11-18.
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