Eta Ursae Minoris

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Eta Ursae Minoris
Ursa Minor IAU.svg
Red circle.svg

Location of η Ursae Minoris (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Ursa Minor
Right ascension 16h 17m 30.28696s[1]
Declination +75° 45′ 19.1885″[1]
Apparent magnitude (V) +4.95[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type F5 V[4]
U−B color index +0.02[2]
B−V color index +0.35[2]
Astrometry
Radial velocity (Rv) −11.0±0.9[5] km/s
Proper motion (μ) RA: −90.30[1] mas/yr
Dec.: +257.66[1] mas/yr
Parallax (π) 33.63 ± 0.17[1] mas
Distance 97.0 ± 0.5 ly
(29.7 ± 0.2 pc)
Absolute magnitude (MV) +2.61[6]
Details
Mass 1.35[7] M
Surface gravity (log g) 4.15±0.14[7] cgs
Temperature 6,858±233[7] K
Metallicity [Fe/H] −0.02[8] dex
Rotational velocity (v sin i) 84.8[3] km/s
Age 1.061[7] Gyr
Other designations
η UMi, 21 Ursae Minoris, BD+76° 596, FK5 612, GC 21999, HD 148048, HIP 79822, HR 6116, SAO 8470, CCDM 16176+7545[9]
Database references
SIMBAD data

Eta Ursae Minoris, Latinized from η Ursae Minoris, is a yellow-white hued star in the northern circumpolar constellation of Ursa Minor. It has been called Anwar al Farkadain, from the Arabic نور الفرقدين ’anwar al-farqadayn, meaning "the brighter of the two calves". It is then paired with ζ Ursae Minoris as Ahfa al Farkadain, "the dimmer of the two calves". The names may originally refer to a pair of Ibexes, and are more properly applied to β UMi and γ UMi respectively, the brighter two stars in the rectangle of Ursa Minor.[10]

This is an F-type main-sequence star of stellar classification F5 V with an apparent magnitude of +4.95, making it faintly visible to the naked eye.[11] Based upon an annual parallax shift of 33.63 mas as seen from the Earth, it is located 97 light years from the Sun. The star is moving closer to the Sun with a radial velocity of −11 km/s,[5] and is traversing the sky with a relatively high proper motion of 0.271 arc seconds per year.[12]

Eta Ursae Minoris is about one billion years old and has an estimated 1.35 times the mass of the Sun.[7] It has a high rate of spin with a projected rotational velocity of 84.8 km/s.[3] These coordinates mark a source of X-ray emission with a luminosity of 11.5×1028 erg s−1.[6] Eta Ursae Minoris may form a wide binary system with a magnitude 15.3 companion star, located at an angular separation of 228.5 arc seconds.[4]

References[edit]

  1. ^ a b c d e van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752Freely accessible, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c Mermilliod, J.-C. (1986), Compilation of Eggen's UBV data, transformed to UBV (unpublished), Bibcode:1986EgUBV........0M.  See the SIMBAD Measurements entry for details.
  3. ^ a b c Schröder, C.; et al. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo", Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377. 
  4. ^ a b 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, Bibcode:2008MNRAS.389..869E, arXiv:0806.2878Freely accessible, doi:10.1111/j.1365-2966.2008.13596.x. 
  5. ^ a b Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, Bibcode:2006AstL...32..759G, arXiv:1606.08053Freely accessible, doi:10.1134/S1063773706110065. 
  6. ^ a b Pizzolato, N.; et al. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases", Astronomy and Astrophysics, 361: 614–628, Bibcode:2000A&A...361..614P. 
  7. ^ a b c d e David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, Bibcode:2015ApJ...804..146D, arXiv:1501.03154Freely accessible, doi:10.1088/0004-637X/804/2/146. 
  8. ^ Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics, 530: A138, Bibcode:2011A&A...530A.138C, arXiv:1103.4651Freely accessible, doi:10.1051/0004-6361/201016276. 
  9. ^ "eta UMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-14. 
  10. ^ Allen, Richard Hinckley (1899), Star-names and Their Meanings, G. E. Stechert, pp. 447–460. 
  11. ^ Kaler, James B., "Anwar al Farkadain", Stars, University of Illinois, retrieved 2014-06-21. 
  12. ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, Bibcode:2005AJ....129.1483L, arXiv:astro-ph/0412070Freely accessible, doi:10.1086/427854.