HD 29697

From Wikipedia, the free encyclopedia
HD 29697
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 04h 41m 18.85634s[1]
Declination +20° 54′ 05.4456″[1]
Apparent magnitude (V) 7.94 - 8.33[2]
Characteristics
Spectral type K3 V[3]
U−B color index +0.94[4]
B−V color index +1.09[4]
Variable type BY Dra[5]
Astrometry
Radial velocity (Rv)+11[6] km/s
Proper motion (μ) RA: −232.38±1.05[1] mas/yr
Dec.: −254.28±0.69[1] mas/yr
Parallax (π)75.82 ± 1.14[1] mas
Distance43.0 ± 0.6 ly
(13.2 ± 0.2 pc)
Absolute magnitude (MV)+7.49[7]
Details
Mass0.75[8] M☉
Radius0.67[8] R☉
Luminosity0.15[8] L☉
Surface gravity (log g)4.50[5] cgs
Temperature4,454±11.4[9] K
Metallicity [Fe/H]0.01[5] dex
Rotational velocity (v sin i)9.73[5] km/s
Age49±37[8] Myr
Other designations
V834 Tau, BD+20° 802, GJ 174, Gliese 174, HD 29697, HIP 21818, SAO 76708.[10]
Database references
SIMBADdata
ARICNSdata

HD 29697 (Gliese 174, V834 Tauri) is a variable star of BY Draconis type in the constellation Taurus. It has an apparent magnitude around 8 and is approximately 43 ly away.

Description[]

HD 29697 is the Henry Draper Catalogue number of this star. It is also known by its designation in the Gliese Catalogue of Nearby Stars, Gliese 174, and its variable star designation V834 Tauri.

V834 Tauri is a BY Draconis variable with maximum and minium apparent magnitudes of 7.94 and 8.33 respectively,[2] so it is never visible to the naked eye.

The star has been examined for indications of a circumstellar disk using the Spitzer Space Telescope, but no statistically-significant infrared excess was detected.[8]

References[]

  1. ^ a b c d e van Leeuwen, F. (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, S2CID 18759600
  2. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. ^ Montes, D.; et al. (2001), "Late-type members of young stellar kinematic groups - I. Single stars" (PDF), Monthly Notices of the Royal Astronomical Society, 328 (1): 45–63, arXiv:astro-ph/0106537, Bibcode:2001MNRAS.328...45M, doi:10.1046/j.1365-8711.2001.04781.x, S2CID 55727428
  4. ^ a b Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M
  5. ^ a b c d Mishenina, T. V.; et al. (November 2012), "Activity and the Li abundances in the FGK dwarfs", Astronomy & Astrophysics, 547: 8, arXiv:1210.6843, Bibcode:2012A&A...547A.106M, doi:10.1051/0004-6361/201118412, S2CID 119287319, A106
  6. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. Determination of Radial Velocities and Their Applications. Vol. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E.
  7. ^ 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.
  8. ^ a b c d e Plavchan, Peter; et al. (June 2009), "New Debris Disks Around Young, Low-Mass Stars Discovered with the Spitzer Space Telescope", The Astrophysical Journal, 698 (2): 1068–1094, arXiv:0904.0819, Bibcode:2009ApJ...698.1068P, doi:10.1088/0004-637X/698/2/1068, S2CID 51417657
  9. ^ Kovtyukh, V. V.; et al. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics, 411 (3): 559–564, arXiv:astro-ph/0308429, Bibcode:2003A&A...411..559K, doi:10.1051/0004-6361:20031378, S2CID 18478960
  10. ^ "HD 29697". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 6 February 2018.
Retrieved from ""