HD 143346
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Apus
Right ascension 16h 05m 55.8193s[1]
Declination −72° 24′ 03.2428″[1]
Apparent magnitude (V) 5.68±0.01[2]
Characteristics
Evolutionary stage horizontal branch[3]
Spectral type K1.5 III CN1[4]
U−B color index +1.26[5]
B−V color index +1.17[5]
Astrometry
Radial velocity (Rv)49±0.9[6] km/s
Proper motion (μ) RA: −32.468 mas/yr
Dec.: +70.299 mas/yr
Parallax (π)11.3858 ± 0.0386 mas[1]
Distance286.5 ± 1.0 ly
(87.8 ± 0.3 pc)
Absolute magnitude (MV)+0.95[7]
Details
Mass1.18[8] M☉
Radius10.6[9] R☉
Luminosity52.6±0.4[1] L☉
Surface gravity (log g)2.43[8] cgs
Temperature4,520±90[10] K
Metallicity [Fe/H]+0.30±0.16[3] dex
Rotational velocity (v sin i)<1[11] km/s
Other designations
38 G. Apodis[12], CPD−72° 1902, FK5 3269, GC 21557, HD 143346, HIP 78868, HR 5955, SAO 257357[13]
Database references
SIMBADdata

HD 143346 (HR 5595) is a single[14] star in the southern circumpolar constellation of Apus. It is 28.5 minutes west and about 5° north of the yellow giant star Gamma Apodis, which is the second brightest star in the constellation of Apus.

This object has an orange hue and is visible to the naked eye as a dim point of light with an apparent visual magnitude of 5.68[2] It is located at a distance of approximately 286 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of 49 km/s. At that distance, the visual brightness of this star is diminished by an extinction of 0.174 due to interstellar dust.[3] The star has an absolute magnitude of 0.95.[7]

HD 1433456 has a stellar classification of K1.5III CN1,[4] indicating a red giant that has an anomalous overabundance of cyanogen in the spectrum. It is currently on the horizontal branch, generating fusion via a helium core. At present it has 118% the mass of the Sun but has expanded to 10.6 times the radius of the Sun.[9] The star is radiating 53 times the luminosity of the Sun[1] from its photosphere at an effective temperature of 4,520 K.[10] HD 1433456 is a member of the Milky Way's thick disk,[15] but is metal enriched.[3] It spins with a projected rotational velocity lower than 1 km/s.[11]

References

  1. 1 2 3 4 5 6 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. 1 2 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.
  3. 1 2 3 4 Jones, M. I.; Jenkins, J. S.; Rojo, P.; Melo, C. H. F. (December 2011). "Study of the impact of the post-MS evolution of the host star on the orbits of close-in planets: I. Sample definition and physical properties⋆⋆⋆". Astronomy & Astrophysics. 536: A71. arXiv:1110.6459. Bibcode:2011A&A...536A..71J. doi:10.1051/0004-6361/201117887. ISSN 0004-6361.
  4. 1 2 Keenan, Philip C.; McNeil, Raymond C. (October 1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373. eISSN 1538-4365. ISSN 0067-0049.
  5. 1 2 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. ↑ 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. 1 2 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.
  8. 1 2 Anders, F.; et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics. 628: A94. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. ISSN 0004-6361.
  9. 1 2 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. ISSN 0004-6256.
  10. 1 2 Charbonnel, C.; Lagarde, N.; Jasniewicz, G.; North, P. L.; Shetrone, M.; Krugler Hollek, J.; Smith, V. V.; Smiljanic, R.; Palacios, A.; Ottoni, G. (January 2020). "Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era". Astronomy & Astrophysics. 633: A34. arXiv:1910.12732. Bibcode:2020A&A...633A..34C. doi:10.1051/0004-6361/201936360. eISSN 1432-0746. ISSN 0004-6361.
  11. 1 2 De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (January 2014). "A catalog of rotational and radial velocities for evolved stars: V. Southern stars⋆⋆⋆". Astronomy & Astrophysics. 561: A126. arXiv:1312.3474. Bibcode:2014A&A...561A.126D. doi:10.1051/0004-6361/201220762. ISSN 0004-6361.
  12. ↑ Gould, B. A., Uranometria Argentina, Reprinted and updated by Pilcher, F, archived from the original on 2012-02-27, retrieved 2012-01-06
  13. ↑ "HD 143346". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-04.
  14. ↑ 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.
  15. ↑ Eggen, O. J. (July 1993). "Evolved GK stars near the sun. I - The old disk population". The Astronomical Journal. 106: 80. Bibcode:1993AJ....106...80E. doi:10.1086/116622.
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