14 Sagittae

14 Sagittae is a binary star[7] system in the equatorial constellation of Aquila.[10] 14 Sagittae is the Flamsteed designation. It appears as a sixth magnitude star, near the lower limit of visibility to the naked eye, having an apparent visual magnitude of 5.89.[2] The system is located 660 light years away, as determined from its annual parallax shift of 4.91 mas.[1] It is moving closer to the Earth with a heliocentric radial velocity of –22 km/s.[4]

14 Sagittae
Observation data
Epoch J2000      Equinox J2000
Constellation Aquila
Right ascension  20h 03m 30.01519s[1]
Declination +16° 01′ 52.5065″[1]
Apparent magnitude (V) 5.89[2]
Characteristics
Spectral type B9p HgMn[3]
U−B color index –0.44[2]
B−V color index –0.06[2]
Astrometry
Radial velocity (Rv)–21.7[4] km/s
Proper motion (μ) RA: +5.28[5] mas/yr
Dec.: –8.99[5] mas/yr
Parallax (π)4.9142 ± 0.0849[1] mas
Distance660 ± 10 ly
(203 ± 4 pc)
Absolute magnitude (MV)−0.72[6]
Orbit[7]
Period (P)61.541 d
Eccentricity (e)0.49
Periastron epoch (T)2440799.01 JD
Argument of periastron (ω)
(secondary)		345°
Semi-amplitude (K1)
(primary)		4.2 km/s
Details
14 Sge A
Luminosity291.53[6] L☉
Surface gravity (log g)3.60[3] cgs
Temperature13,200[3] K
Rotational velocity (v sin i)7.0±0.5[8] km/s
Other designations
14 Sge, BD+15° 4033, GC 27812, HD 190229, HIP 98754, HR 7664, SAO 105615[9]
Database references
SIMBADdata

This is a single-lined spectroscopic binary with an orbital period of 61.5 days and an eccentricity of 0.49.[7] The visible component is a chemically peculiar mercury-manganese star[11] with a stellar classification of B9p HgMn.[3] It is narrow-lined with a projected rotational velocity of 7 km/s.[8] The star is radiating 292[6] times the Sun's luminosity from its photosphere at an effective temperature of 13,200 K.[3]

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.
  2. Fernie, J. D. (May 1983), "New UBVRI photometry for 900 supergiants", Astrophysical Journal Supplement Series, 52: 7–22, Bibcode:1983ApJS...52....7F, doi:10.1086/190856.
  3. Smith, K. C.; Dworetsky, M. M. (July 1993), "Elemental Abundances in Normal Late B-Stars and Hgmn-Stars from Co-Added IUE Spectra - Part One - Iron Peak Elements", Astronomy and Astrophysics, 274 (2): 335, Bibcode:1993A&A...274..335S.
  4. Wilson, Ralph Elmer (1953), General Catalogue of Stellar Radial Velocities, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
  5. van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  6. 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.
  7. Pourbaix, D.; et al. (2004), "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits", Astronomy & Astrophysics, 424: 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213.
  8. Adelman, S. J.; et al. (June 2017), "Elemental abundance analyses with DAO spectrograms: XL", Astronomische Nachrichten, 338 (5): 584–597, Bibcode:2017AN....338..584A, doi:10.1002/asna.201613214.
  9. "4 Aql". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 27, 2018.
  10. Hoffleit, D.; Warren Jr., W. H. (1991), The Bright Star Catalogue (5th Revised [Preliminary Version] ed.), Astronomical Data Center, NSSDC/ADC, Bibcode:1964BS....C......0H.
  11. Adelman, S. J. (December 1988), "Elemental Abundance Analyses with Coadded DAO Spectrograms - Part Five - the Mercury-Manganese Stars Phi-Herculis 28-HERCULIS and HR:7664", Monthly Notices of the Royal Astronomical Society, 235 (3): 763, Bibcode:1988MNRAS.235..763A, doi:10.1093/mnras/235.3.763.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.