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5 Vulpeculae

5 Vulpeculae
Map of the constellation Vulpecula
5 Vul in the constellation Vulpecula (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Vulpecula
Right ascension 19h 26m 13.2463s[1]
Declination +20° 05′ 51.8394″[1]
Apparent magnitude (V) 5.65±0.010[2]
Characteristics
Spectral type A0 V[3]
Apparent magnitude (U) 5.62±0.012[2]
Apparent magnitude (B) 5.66±0.011[2]
Astrometry
Radial velocity (Rv)−20.9±2.9[4] km/s
Proper motion (μ) RA: +3.395±0.114[1] mas/yr
Dec.: −34.787±0.137[1] mas/yr
Parallax (π)13.8921 ± 0.0900 mas[1]
Distance235 ± 2 ly
(72.0 ± 0.5 pc)
Absolute magnitude (MV)1.29[5]
Details[3]
Mass2.33±0.02 M☉
Radius2.7[6] R☉
Luminosity34±2 L☉
Surface gravity (log g)4.0[7] cgs
Temperature9,840+91
−90 K
Rotational velocity (v sin i)154 km/s
Age198[7] Myr
Other designations
5 Vul, BD+19° 4015, HD 182919, HIP 95560, HR 7390, SAO 104831[8]
Database references
SIMBADdata

5 Vulpeculae is a single,[9] white-hued star in the northern constellation of Vulpecula.[8] It is situated amidst a random concentration of bright stars designated Collinder 399,[10] 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.[4] Based upon an annual parallax shift of 13.8921±0.0900 mas,[1] it is located around 235 light years from the Sun. It is moving closer with a heliocentric radial velocity of −21 km/s,[4] and will make its closest approach in 2.5 million years at a separation of around 120 ly (36.89 pc).[5]

This is a young A-type main-sequence star with a stellar classification of A0 V.[3] It is a rapidly rotating star[11] with a projected rotational velocity of 154 km/s.[3] The star has an estimated 2.33[3] times the mass of the Sun and about 2.7[6] times the Sun's radius. It is radiating 34 times the Sun's luminosity from its photosphere at an effective temperature of 8,940 K.[3]

A warm debris disk was detected by the Spitzer Space Telescope at a temperature of 206 K (−89 °F; −67 °C), orbiting 13 Astronomical units from the host star.[12] Although this finding has not been directly detected, the emission signature indicates the disk is in the form of a thin ring. The emission displays weak transient absorption features that are indicative of kilometer-sized exocomets that are undergoing evaporation as they approach the host star.[11] These absorption features have been observed to vary on time scales of hours, days, or months.[13]

References

  1. ^ a b c d e f 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. ^ a b c Harmanec, P.; et al. (2020). "A new study of the spectroscopic binary 7 Vul with a Be star primary". Astronomy and Astrophysics. 639. Table A.1. arXiv:2005.11089. Bibcode:2020A&A...639A..32H. doi:10.1051/0004-6361/202037964. S2CID 218862853.
  3. ^ a b c d e f Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  4. ^ a b c 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:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  5. ^ a b 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, S2CID 119257644.
  6. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (2) (3rd ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  7. ^ a b Chen, Christine H.; et al. (2014), "The Spitzer Infrared Spectrograph Debris Disk Catalog. I. Continuum Analysis of Unresolved Targets", The Astrophysical Journal Supplement, 211 (3): 22, Bibcode:2014ApJS..211...25C, doi:10.1088/0067-0049/211/2/25, 25.
  8. ^ a b "5 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-04-13.
  9. ^ 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.
  10. ^ Baumgardt, H. (December 1998), "The nature of some doubtful open clusters as revealed by HIPPARCOS", Astronomy and Astrophysics, 340: 402–414, Bibcode:1998A&A...340..402B.
  11. ^ a b Montgomery, Sharon L.; Welsh, Barry Y. (October 2012), "Detection of Variable Gaseous Absorption Features in the Debris Disks Around Young A-type Stars", Publications of the Astronomical Society of the Pacific, 124 (920): 1042, Bibcode:2012PASP..124.1042M, doi:10.1086/668293
  12. ^ Morales, Farisa Y.; et al. (2009), "Spitzer mid-Ir Spectra of Dust Debris Around A and Late B Type Stars: Asteroid Belt Analogs and Power-Law Dust Distributions" (PDF), The Astrophysical Journal, 699 (2): 1067–1086, Bibcode:2009ApJ...699.1067M, doi:10.1088/0004-637X/699/2/1067, S2CID 45235873.
  13. ^ Montgomery, Sharon L.; Welsh, B.; Lallement, R.; Timbs, B. W. (January 2014), "Exocomet Gas: Now You See It, Now You Don't", American Astronomical Society, AAS Meeting #223, 223: 401.02, Bibcode:2014AAS...22340102M, 401.02.
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