Iota Phoenicis – Wikipedia

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Star in the constellation Phoenix

ι Phoenicis, Latinized as Iota Phoenicis, is a binary star[9] system in the southern constellation of Phoenix, near the constellation border with Grus. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude that fluctuates around 4.71.[2] This system lies approximately 254 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +19.4 km/s.[4]

The primary component is an Ap star on the main sequence with a stellar classification of A2VpSrCrEu,[3] where the suffix notation indicates abnormal abundances of strontium, chromium, and europium in the stellar atmosphere. It is an Alpha2 Canum Venaticorum variable; its apparent magnitude varies from 4.70 down to 4.75 with a period of 12.5 days.[3] A rotationally-modulated magnetic field has been measured, varying from −72±9 G to 57±9 G. It has an estimated rotation period of 5.98±0.06 d, although this is in need of further confirmation.[10]

The proper motion companion[11] is a magnitude 12.8 star at an angular separation of 6.7″.[9]

References[edit]

  1. ^ a b c d e f g h 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 d Ducati, J. R. (2002). “VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson’s 11-color system”. CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237….0D.
  3. ^ a b c d e f Samus, N. N.; et al. (2017), “General Catalogue of Variable Stars”, Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep…61…80S, doi:10.1134/S1063772917010085, S2CID 125853869, retrieved 2019-08-06.
  4. ^ a b Wilson, R. E. (1953). “General Catalogue of Stellar Radial Velocities”. Carnegie Institute Washington D.C. Publication. Carnegie Institution of Washington. Bibcode:1953GCRV..C……0W. ISBN 9780598216885. LCCN 54001336.
  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. S2CID 119257644. Vizier catalog entry
  6. ^ a b c d 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. arXiv:1501.03154. Bibcode:2015ApJ…804..146D. doi:10.1088/0004-637X/804/2/146. S2CID 33401607.
  7. ^ Gontcharov, G. A. (2012). “Dependence of kinematics on the age of stars in the solar neighborhood”. Astronomy Letters. 38 (12): 771–782. arXiv:1606.08814. Bibcode:2012AstL…38..771G. doi:10.1134/S1063773712120031. S2CID 118345778. Vizier catalog entry
  8. ^ “iot Phe”. SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-06.
  9. ^ a b Eggleton, P. P.; Tokovinin, A. A. (2008). “A catalogue of multiplicity among bright stellar systems”. Monthly Notices of the Royal Astronomical Society. 389 (2): 869. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
  10. ^ Sikora, J.; et al. (March 2019), “A volume-limited survey of mCP stars within 100 pc II: rotational and magnetic properties”, Monthly Notices of the Royal Astronomical Society, 483 (3): 3127–3145, arXiv:1811.05635, Bibcode:2019MNRAS.483.3127S, doi:10.1093/mnras/sty2895, S2CID 119415579.
  11. ^ Frankowski, A.; et al. (March 2007), “Proper-motion binaries in the Hipparcos catalogue. Comparison with radial velocity data”, Astronomy and Astrophysics, 464 (1): 377–392, arXiv:astro-ph/0612449, Bibcode:2007A&A…464..377F, doi:10.1051/0004-6361:20065526, S2CID 14010423