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Zeta Fornacis

From Wikipedia, the free encyclopedia

Zeta Fornacis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Fornax
Right ascension 02h 59m 36.18299s[1]
Declination −25° 16′ 26.8853″[1]
Apparent magnitude (V) 5.67[2]
Characteristics
Spectral type F4 V[3]
U−B color index +0.01[2]
B−V color index +0.39[2]
Astrometry
Radial velocity (Rv)+29.09±0.63[1] km/s
Proper motion (μ) RA: +181.005[1] mas/yr
Dec.: +84.641[1] mas/yr
Parallax (π)29.8975 ± 0.0856 mas[1]
Distance109.1 ± 0.3 ly
(33.45 ± 0.10 pc)
Absolute magnitude (MV)+3.14[4]
Details
Mass1.8[5] M☉
Radius1.62+0.02
−0.03[1] R☉
Luminosity4.77±0.02[1] L☉
Surface gravity (log g)4.16±0.14[5] cgs
Temperature6,699+65
−39[1] K
Metallicity [Fe/H]+0.02[3] dex
Rotational velocity (v sin i)84.9±4.2[4] km/s
Age1.5[5] Gyr
Other designations
ζ For, CD−25° 1191, HD 18692, HIP 13942, HR 901, SAO 168209.[6]
Database references
SIMBADdata

ζ Fornacis (often Latinised as Zeta Fornacis) is the Bayer designation for a star in the southern constellation of Fornax. It is faintly visible to the naked eye with an apparent visual magnitude of 5.67.[2] Based upon a measured annual parallax shift of 29.9 mas,[1] it is located at a distance of about 109 light-years from the Sun. The star is drifting further away with a radial velocity of +29 km/s.[1] Positioned about 1.3° to the southeast of Zeta Fornacis is the galaxy NGC 1232.[7]

This is an F-type main-sequence star with a stellar classification of F4 V.[3] With an estimated age of 1.5 billion years, it has 1.8[5] times the mass of the Sun and 1.6[1] times the Sun's radius. The star is radiating 4.77 times the luminosity of the Sun from its photosphere at an effective temperature of 6,699 K.[1] It is spinning with a projected rotational velocity of 84.9 km/s,[4] and has a near-solar metallicity—what astronomers term the abundance of elements other than hydrogen and helium.[3] This star is a probable member of the Hyades Stream[8]—a group of stars that share a common motion through space with the Hyades cluster.

Zeta Fornacis has a common proper motion companion, NLTT 9563, a magnitude 13.50[9] star with a classification of M 2.5.[10] As of 2004, this companion was positioned at an angular separation of 176.1 arcseconds along a position angle of 288.1°.[9]

References

  1. ^ a b c d e f g h i j k l m 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 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  3. ^ a b c d Gray, R. O.; et al. (2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–70, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  4. ^ a b c Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
  5. ^ 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.
  6. ^ "zet For". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-01-22.
  7. ^ Bakich, Michael E. (2010), 1,001 Celestial Wonders to See Before You Die: The Best Sky Objects for Star Gazers, The Patrick Moore Practical Astronomy Series, Springer Science & Business Media, p. 400, ISBN 978-1441917775.
  8. ^ Eggen, O. J. (June 1985), "A systematic search for members of the Hyades Supercluster. IV - The metallic-line stars and ultrashort-period Cepheids", Astronomical Journal, 90: 1046−1059, Bibcode:1985AJ.....90.1046E, doi:10.1086/113812.
  9. ^ a b Gould, Andrew; Chanamé, Julio (February 2004), "New Hipparcos-based Parallaxes for 424 Faint Stars", The Astrophysical Journal Supplement Series, 150 (2): 455−464, arXiv:astro-ph/0309001, Bibcode:2004ApJS..150..455G, doi:10.1086/381147, S2CID 8494577.
  10. ^ Scholz, R.-D.; et al. (October 2005), "Search for nearby stars among proper motion stars selected by optical-to-infrared photometry. III. Spectroscopic distances of 322 NLTT stars", Astronomy and Astrophysics, 442 (1): 211−227, arXiv:astro-ph/0507284, Bibcode:2005A&A...442..211S, doi:10.1051/0004-6361:20053004, S2CID 7013323.
This page was last edited on 14 May 2023, at 12:37
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