HD 143346
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Apus |
| Right ascension | 16h 05m 55.81809s[1] |
| Declination | −72° 24′ 03.2395″[1] |
| Apparent magnitude (V) | 5.70[2] |
| Characteristics | |
| Spectral type | K1.5III CN1[3] |
| B−V color index | 1.169±0.002[2] |
| Astrometry | |
| Radial velocity (Rv) | 49.0[2] km/s |
| Proper motion (μ) | RA: −32.116±0.094[1] mas/yr Dec.: +70.083±0.112[1] mas/yr |
| Parallax (π) | 11.5335 ± 0.0650 mas[1] |
| Distance | 283 ± 2 ly (86.7 ± 0.5 pc) |
| Absolute magnitude (MV) | 0.95[2] |
| Details[4] | |
| Mass | 1.95 M☉ |
| Radius | 10.77+0.16 −0.02[1] R☉ |
| Luminosity | 49.1±0.4[1] L☉ |
| Surface gravity (log g) | 2.38 cgs |
| Temperature | 4,655+5 −34[1] K |
| Metallicity [Fe/H] | 0.30±0.16 dex |
| Rotational velocity (v sin i) | 1.95 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
HR 5955 is a single[6] star in the far southern constellation of Apus. It is 28.5 minutes earlier than and about 5 deg. 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 5.70.[6] It is located at a distance of approximately 283 light years from the Sun based on parallax, and is drifting further away with a radial velocity of 49 km/s.[6] At that distance, the visual brightness of this star is diminished by an extinction of 0.174 due to interstellar dust.[4] The star has an absolute magnitude of 0.95.[2]
This is an aging giant star on the horizontal branch[4] with a stellar classification of K1.5III CN1.[3] This indicates it has exhausted the supply of hydrogen at its core and is currently fusing helium. The suffix notation means there is an anomalous overabundance of cyanogen in the spectrum. It has expanded to 10.8[1] times the radius of the Sun and nearly double the Sun's mass.[4] The star is radiating 49 times the luminosity of the Sun from its photosphere at an effective temperature of 4,655 K.[1]
References
- ^ a b c d e f g h i j 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.
- ^ a b c d e 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.
- ^ a b Keenan, Philip C.; McNeil, Raymond C. (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.
- ^ a b c d Jones, M. I.; et al. (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: 7. arXiv:1110.6459. Bibcode:2011A&A...536A..71J. doi:10.1051/0004-6361/201117887. A71.
- ^ "HD 143346". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-04.
- ^ a b c 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.
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