| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Hercules |
| Right ascension | 16h 32m 36.29190s[1] |
| Declination | +11° 29′ 16.9479″[1] |
| Apparent magnitude (V) | 4.84[2] |
| Characteristics | |
| Evolutionary stage | giant |
| Spectral type | K4.5 III[3] |
| B−V color index | 1.495±0.002[2] |
| Variable type | suspected[4] |
| Astrometry | |
| Radial velocity (Rv) | +2.92±0.20[2] km/s |
| Proper motion (μ) | RA: -178.84[1] mas/yr Dec.: −79.27[1] mas/yr |
| Parallax (π) | 9.29 ± 0.26 mas[1] |
| Distance | 351 ± 10 ly (108 ± 3 pc) |
| Absolute magnitude (MV) | −0.17[5] |
| Details | |
| Mass | 1.19[6] M☉ |
| Radius | 42.05+0.45 −1.81[7] R☉ |
| Luminosity | 384±19[7] L☉ |
| Surface gravity (log g) | 1.79±0.28[8] cgs |
| Temperature | 3,958±25[6] K |
| Metallicity [Fe/H] | −0.18±0.09[8] dex |
| Rotational velocity (v sin i) | 5.4[9] km/s |
| Age | 6.53[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
29 Herculis is a single[11] star located around 351[1] light years away from the Sun in the northern constellation of Hercules, a few degrees away from Omega Herculis. It has the Bayer designation h Herculis, while 29 Herculis is the Flamsteed designation.[10] This star is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.84.[2] It is moving further from the Earth with a heliocentric radial velocity of +3 km/s.[2] The star has a relatively high proper motion, traversing the celestial sphere at the rate of 0.195 arc seconds per annum.[12]
This is an aging giant star with a stellar classification of K4.5 III.[3] It displays an enhanced abundance of elements generated through the alpha process, and, in particular, has a strong enhancement of silicon.[13] 29 Herculis is a suspected variable star of unknown type, and has been measured ranging in visual magnitude from 4.82 down to 4.85.[4] It is an estimated 6.53[6] billion years old with 1.19[6] times the mass of the Sun. Having exhausted the supply of hydrogen at its core, it has expanded to 42[7] times the Sun's radius. The star is radiating 384[7] times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,958 K.[6]
References
- ^ a b c d e f 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.
- ^ 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, S2CID 119257644.
- ^ 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 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.
- ^ Schiavon, Ricardo P. (July 2007), "Population Synthesis in the Blue. IV. Accurate Model Predictions for Lick Indices and UBV Colors in Single Stellar Populations", The Astrophysical Journal Supplement Series, 171 (1): 146–205, arXiv:astro-ph/0611464, Bibcode:2007ApJS..171..146S, doi:10.1086/511753, S2CID 13946698.
- ^ a b c d e f Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal, 150 (3), 88, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114.
- ^ a b c d 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 Koleva, M.; Vazdekis, A. (February 2012), "Stellar population models in the UV. I. Characterisation of the New Generation Stellar Library", Astronomy & Astrophysics, 538: A143, arXiv:1111.5449, Bibcode:2012A&A...538A.143K, doi:10.1051/0004-6361/201118065, S2CID 53999614.
- ^ Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209.
- ^ a b "h Her". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-06-12.
- ^ 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.
- ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv:astro-ph/0412070, Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID 2603568.
- ^ Franchini, M.; et al. (January 2004), "Synthetic Lick Indices and Detection of α-Enhanced Stars", The Astrophysical Journal, 601 (1): 485–499, Bibcode:2004ApJ...601..485F, doi:10.1086/380443.
This page was last edited on 22 October 2022, at 12:47