Chi1 Fornacis

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For other stars with a similar Bayer designation, see χ Fornacis.
χ1 Fornacis
Location of χ1 Fornacis (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Fornax
Right ascension 03h 25m 55.84196s[1]
Declination −35° 55′ 15.1876″[1]
Apparent magnitude (V) 6.39±0.01[2]
Characteristics
Evolutionary stage main sequence star[3]
Spectral type A1 IV[4]
B−V color index +0.08[5]
Astrometry
Radial velocity (Rv)19.0±0.5[6] km/s
Proper motion (μ) RA: +36.770 mas/yr[1]
Dec.: −4.641 mas/yr[1]
Parallax (π)9.6154 ± 0.0266 mas[1]
Distance339.2 ± 0.9 ly
(104.0 ± 0.3 pc)
Absolute magnitude (MV)+1.42[7]
Details
Mass2.05±0.08[8] M☉
Radius2.20±0.11[9] R☉
Luminosity31.24+3.43
−3.09[3] L☉
Surface gravity (log g)4.08±0.07[10] cgs
Temperature8,770+122
−120[3] K
Metallicity [Fe/H]0.00+0.02
−0.04[8] dex
Rotational velocity (v sin i)136[11] km/s
Age5.5±0.5[12] Myr
Other designations
χ1 For, 89 G. Fornacis[13], NSV 1162, CD−36°1290, CPD−36°350, GC 4097, HD 21573, HIP 15987, HR 1042, SAO 194289[14]
Database references
SIMBADFor data

Chi1 Fornacis, Latinised from χ1 Fornacis is a solitary white-hued star located in the southern constellation Fornax. Its barley visible to the naked eye with an apparent magnitude of 6.39,[2] which is near the limit for naked eye visibility. Gaia DR3 parallax measurements imply a distance of 339 light-years[1] and it is currently drifitng away with a heliocentric radial velocity of 19.0 km/s.[6] At its current distance, Chi1 Fornacis' brightness is diminshed by an interstellar extinction of 0.08 magnitudes[15] and it has an absolute magnitude of +1.42.[7]

Chi1 Fornacis has a stellar classification of A1 IV,[4] indicating that it is a slightly evolved A-type star that is ceasing hydrogen fusion at its core. Alternatively, it has been given a class of A1 Vbn,[16] indicating that it is instead a slightly less luminous A-type main-sequence star with broad or nebulous absorption lines due to rapid rotation. It has 2.05 times the mass of the Sun[8] and 2.20 times the radius of the Sun.[9] It radiates 31.24 times the luminosity of the Sun from its photosphere at an effective temperature of 8,870 K.[3] Chi1 Fornacis has a solar metallicity[8] and it is estimated to be only 5.5 million years old.[12] It spins rapidly with a projected rotational velocity of 136 km/s.[11]

It is the brightest star and titular member in the χ1 Fornacis cluster, a star cluster around 104 parsecs from Earth.[17]

χ1 Fornacis cluster[edit]

The χ1 Fornacis cluster, or Alessi 13,[18] is one of the four star clusters known within 110 parsecs from Earth. [17] Despite its closeness, the χ1 Fornacis cluster has barely been studied. Its age is 40 million years and its distance is 104 parsecs.[17] The χ1 Fornacis cluster appears to be closely related to the Tucana–Horologium and Columba associations.[17] A remarkable, unprecedented aspect of the cluster is the large percentage of M-type stars with warm excess infrared emission due to orbiting dust grains.[17]

References[edit]

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361. S2CID 17128864.
  3. ^ a b c d Zorec, J.; Royer, F. (January 2012). "Rotational velocities of A-type stars IV: Evolution of rotational velocities". Astronomy & Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. eISSN 1432-0746. ISSN 0004-6361. S2CID 55586789.
  4. ^ a b Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Declinations −40° to −26°. Vol. 3. Bibcode:1982mcts.book.....H.
  5. ^ Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99–110. Bibcode:1966CoLPL...4...99J.
  6. ^ a b Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN 1562-6873. ISSN 1063-7737. S2CID 119231169.
  7. ^ a b Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
  8. ^ a b c d Bochanski, John J.; Faherty, Jacqueline K.; Gagné, Jonathan; Nelson, Olivia; Coker, Kristina; Smithka, Iliya; Desir, Deion; Vasquez, Chelsea (12 March 2018). "Fundamental Properties of Co-moving Stars Observed byGaia". The Astronomical Journal. 155 (4): 149. arXiv:1801.00537. Bibcode:2018AJ....155..149B. doi:10.3847/1538-3881/aaaebe. eISSN 1538-3881. S2CID 119256051.
  9. ^ a b Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (October 2004). "The angular sizes of dwarf stars and subgiants. Surface brightness relations calibrated by interferometry". Astronomy & Astrophysics. 426 (1): 297–307. arXiv:astro-ph/0404180. Bibcode:2004A&A...426..297K. doi:10.1051/0004-6361:20035930. eISSN 1432-0746. ISSN 0004-6361. S2CID 6077801.
  10. ^ Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. eISSN 1538-3881. hdl:1721.1/124721. S2CID 166227927.
  11. ^ a b Royer, F.; Gerbaldi, M.; Faraggiana, R.; Gómez, A. E. (January 2002). "Rotational velocities of A-type stars. I. Measurement of vsini in the southern hemisphere". Astronomy & Astrophysics. 381 (1): 105–121. arXiv:astro-ph/0110490. Bibcode:2002A&A...381..105R. doi:10.1051/0004-6361:20011422. eISSN 1432-0746. ISSN 0004-6361.
  12. ^ a b Ujjwal, K.; Kartha, Sreeja S.; Mathew, Blesson; Manoj, P.; Narang, Mayank (Apr 1, 2020). "Analysis of Membership Probability in Nearby Young Moving Groups with Gaia DR2". The Astronomical Journal. 159 (4): 166. arXiv:2002.04801. Bibcode:2020AJ....159..166U. doi:10.3847/1538-3881/ab76d6. ISSN 0004-6256.
  13. ^ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  14. ^ "*chi01 Fornacis". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved May 3, 2024.
  15. ^ Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017). "Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars". Monthly Notices of the Royal Astronomical Society. 472 (4): 3805–3820. arXiv:1709.01160. Bibcode:2017MNRAS.472.3805G. doi:10.1093/mnras/stx2219. eISSN 1365-2966. ISSN 0035-8711. S2CID 118879856.
  16. ^ Paunzen, E.; Duffee, B.; Heiter, U.; Kuschnig, R.; Weiss, W. W. (July 2001). "A spectroscopic survey for λ Bootis stars". Astronomy & Astrophysics. 373 (2): 625–632. Bibcode:2001A&A...373..625P. doi:10.1051/0004-6361:20010630. eISSN 1432-0746. ISSN 0004-6361.
  17. ^ a b c d e Zuckerman, B.; Klein, Beth; Kastner, Joel (2019). "The Nearby, Young, χ1 Fornacis Cluster: Membership, Age, and an Extraordinary Ensemble of Dusty Debris Disks". The Astrophysical Journal. 887 (1). 87. arXiv:1909.08764. Bibcode:2019ApJ...887...87Z. doi:10.3847/1538-4357/ab45ea.
  18. ^ P. A. B. Galli; H. Bouy; J. Olivares; N. Miret-Roig; L. M. Sarro; D. Barrado; A. Berihuete (2021). "χ1 Fornacis cluster DANCe: Census of stars, structure, and kinematics of the cluster with Gaia-EDR3" (PDF). Astronomy and Astrophysics. 654. A122. doi:10.1051/0004-6361/202141366. Retrieved 28 November 2023.
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