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Nu Fornacis

In this article, we will delve into the fascinating world of Nu Fornacis, exploring its many facets and its impact on various areas of daily life. Along these lines, we will analyze both its origin and its evolution over time, examining in detail its influence on current society. In addition, we will cover different perspectives and expert opinions on Nu Fornacis, with the aim of offering a comprehensive and complete vision of this exciting topic. From its relevance in science, culture and technology, to its impact on our daily lives, we will approach Nu Fornacis from different angles, with the purpose of enriching our reader's knowledge and understanding of this extremely important topic.

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Nu Fornacis
Location of ν Fornacis (circled in red)
Observation data
Epoch J2000      Equinox J2000
Constellation Fornax
Right ascension 02h 04m 29.43861s[1]
Declination −29° 17′ 48.5477″[1]
Apparent magnitude (V) 4.69[2] (4.68 – 4.73[3])
Characteristics
Spectral type B9.5IIIspSi[4]
U−B color index −0.51[2]
B−V color index −0.17[2]
Variable type α2 CVn[5]
Astrometry
Radial velocity (Rv)+18.50[6] km/s
Proper motion (μ) RA: +12.79[7] mas/yr
Dec.: +8.48[7] mas/yr
Parallax (π)8.79±0.26 mas[1]
Distance370 ± 10 ly
(114 ± 3 pc)
Absolute magnitude (MV)−0.60[8]
Details
Mass3.65±0.18[9] M☉
Radius3.44[10] R☉
Luminosity245[9] L☉
Temperature13,400[11] K
Rotation1.89[11] d
Rotational velocity (v sin i)50±5[11] km/s
Other designations
ν For, CD−29°706, FK5 1055, GC 2506, HD 12767, HIP 9677, HR 612, SAO 167532[7]
Database references
SIMBADdata

Nu Fornacis, Latinized from ν Fornacis, is a single,[12] variable star in the southern constellation of Fornax. It is blue-white in hue and faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.69.[2] This body is located approximately 370 light years distant from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +18.5 km/s.[6] It is a candidate member of the Pisces-Eridanus stellar stream, which suggests an age of 120 million years or less.[13]

A light curve for Nu Fornacis plotted from TESS data[14]

This object is an Ap star[15] with a stellar classification of B9.5IIIspSi[4] matching a late B-type giant star. The 'Si' suffix indicates an abundance anomaly of silicon. It is an Alpha2 Canum Venaticorum variable that ranges from magnitude 4.68 down to 4.73 with a period of 1.89 days – the same as its rotational period.[5][11] It is 3.65 times as massive and 245 times as luminous as the Sun,[9] with 3.44 times the Sun's diameter.[10]

References

  1. ^ a b c d 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. Vizier catalog entry
  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. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "General Catalogue of Variable Stars". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. ^ a b Abt, Helmut A.; Morrell, Nidia I. (July 1995). "The relation between Rotational Velocities and Spectral Peculiarities among A-type stars". The Astrophysical Journal Supplement Series. 99: 135–172. Bibcode:1995ApJS...99..135A. doi:10.1086/192182.
  5. ^ a b 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.
  6. ^ a b Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Washington. Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W. LCCN 54001336.
  7. ^ a b c "* nu. For". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-04-08.
  8. ^ 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.
  9. ^ a b c North, P. (1998). "Do SI stars undergo any rotational braking?". Astronomy and Astrophysics. 334: 181–87. arXiv:astro-ph/9802286. Bibcode:1998A&A...334..181N.
  10. ^ a b Shulyak, D.; et al. (2014). "Interferometry of chemically peculiar stars: Theoretical predictions versus modern observing facilities". Monthly Notices of the Royal Astronomical Society. 443 (2): 1629. arXiv:1406.6093. Bibcode:2014MNRAS.443.1629S. doi:10.1093/mnras/stu1259.
  11. ^ a b c d Leone, F.; et al. (2000). "A spectroscopic study of the magnetic chemically peculiar star nu Fornacis". Astronomy and Astrophysics. 359: 635–38. Bibcode:2000A&A...359..635L.
  12. ^ 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. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
  13. ^ Curtis, Jason L.; et al. (August 2019). "TESS Reveals that the Nearby Pisces─Eridanus Stellar Stream is only 120 Myr Old". The Astronomical Journal. 158 (2): 11. arXiv:1905.10588. Bibcode:2019AJ....158...77C. doi:10.3847/1538-3881/ab2899. S2CID 166228270. 77.
  14. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  15. ^ Chen, P. S.; et al. (May 2017). "A New Photometric Study of Ap and Am Stars in the Infrared". The Astronomical Journal. 153 (5): 28. Bibcode:2017AJ....153..218C. doi:10.3847/1538-3881/aa679a. 218.
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