HD 127334
  | |
| Observation data Epoch J2000.0[1] Equinox J2000.0[1] | |
|---|---|
| Constellation | Boötes |
| Right ascension | 14h 29m 36.80877s |
| Declination | +41° 47′ 45.2854″ |
| Apparent magnitude (V) | 6.36[2] |
| Characteristics | |
| Spectral type | G5V CH0.3[3] |
| B−V color index | 1.010[2][4] |
| J−H color index | 0.258[5] |
| J−K color index | 0.369[5] |
| Astrometry | |
| Radial velocity (Rv) | −0.401±0.0007[6] km/s |
| Proper motion (μ) | RA: 161.373[1] mas/yr Dec.: −220.361[1] mas/yr |
| Parallax (π) | 42.7526 ± 0.0174 mas[1] |
| Distance | 76.29 ± 0.03 ly (23.390 ± 0.010 pc) |
| Details | |
| Mass | 1.02±0.02,[7] 1.07[8] M☉ |
| Surface gravity (log g) | 4.37±0.13[9] cgs |
| Temperature | 5758±76,[9] 5635±50[7] K |
| Metallicity [Fe/H] | 0.24±0.06,[9] 0.19±0.04[7] dex |
| Age | 8.6±1.3,[7] 10.5–10.7,[10] ~7.1[11] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 127334 is a solitary[8] Sun-like star in the northern constellation of Boötes. With an apparent magnitude of 6.36, it can be faintly seen by the naked eye from Earth as a yellow-hued dot of light. As such, it is listed in the Bright Star Catalogue as HR 5423. It is located at a distance of 76.29 light-years (23.39 parsecs) according to Gaia EDR3 parallax measurements.
Stellar properties
[edit]This is a G-type main-sequence star much like the Sun, with a spectral type of G5V CH0.3,[3] where the suffix notation indicates an anomalous overabundance of the methylidyne radical. It is slightly more massive than the Sun but marginally cooler at 5,758 K (5,485 °C; 9,905 °F) or 5,635 K (5,362 °C; 9,683 °F). The Sun's effective temperature, for comparison, is 5,772 K (5,499 °C; 9,930 °F).[12]
The star belongs to the thin disk population of the Milky Way[10] and is thought to be ancient: its age estimate varies between publications, but generally lies between 7–11 Gyr, much older than the Solar System (aged 4.568 Gyr[13]). Despite its old age, it is enriched in heavy elements, possessing a super-solar metallicity of 0.24±0.06 or 0.19±0.04 dex.
It has a low or very low level of surface activity, unlike some other similar stars such as Toliman (Alpha Centauri B).[2]
HD 127334 has been a long-term target of the California Planet Search,[14] but no exoplanets have been discovered to orbit the star.[9]
See also
[edit]References
[edit]- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c Rajpaul, V M; et al. (1 March 2020). "A robust, template-free approach to precise radial velocity extraction". Monthly Notices of the Royal Astronomical Society. 492 (3): 3960–3983. doi:10.1093/mnras/stz3599. ISSN 0035-8711.
- ^ a b Gray, R. O.; et al. (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I." The Astronomical Journal. 126 (4): 2048–2059. doi:10.1086/378365. ISSN 0004-6256.
- ^ Oja, T. (August 1991). "UBV photometry of stars whose positions are accurately known. VI". Astronomy & Astrophysics Supplement Series. 89: 415. Bibcode:1991A&AS...89..415O.
- ^ a b c "HD 127334". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 15 November 2024.
- ^ Soubiran, C.; et al. (2018). "Gaia Data Release 2: The catalogue of radial velocity standard stars". Astronomy & Astrophysics. 616: A7. doi:10.1051/0004-6361/201832795. ISSN 0004-6361.
- ^ a b c d Gonzalez, G. (1 January 2015). "Parent stars of extrasolar planets – XIV. Strong evidence of Li abundance deficit". Monthly Notices of the Royal Astronomical Society. 446 (1): 1020–1025. doi:10.1093/mnras/stu2156. ISSN 1365-2966.
- ^ a b Fuhrmann, K.; et al. (10 February 2017). "Multiplicity among Solar-type Stars". The Astrophysical Journal. 836 (1): 139. doi:10.3847/1538-4357/836/1/139. ISSN 0004-637X.
- ^ a b c d Lienhard, F; Mortier, A; Buchhave, L; Collier Cameron, A; López-Morales, M; Sozzetti, A; Watson, C A; Cosentino, R (26 May 2022). "Multi-mask least-squares deconvolution: extracting RVs using tailored masks". Monthly Notices of the Royal Astronomical Society. 513 (4): 5328–5343. doi:10.1093/mnras/stac1098. ISSN 0035-8711.
- ^ a b Ženovienė, R.; Tautvaišienė, G.; Nordström, B.; Stonkutė, E.; Barisevičius, G. (2015). "Stellar substructures in the solar neighbourhood: IV. Kinematic Group 1 in the Geneva-Copenhagen survey". Astronomy & Astrophysics. 576: A113. doi:10.1051/0004-6361/201425088. ISSN 0004-6361.
- ^ de Andrés, F. Llorente; de la Reza, R.; Cruz, P.; Cuenda-Muñoz, D.; Alfaro, E. J.; Chavero, C.; Cifuentes, C. (2024). "The evolution of lithium in FGK dwarf stars: Influence of planets and Galactic migration". Astronomy & Astrophysics. 684: A28. doi:10.1051/0004-6361/202346744. ISSN 0004-6361.
- ^ Prša, Andrej; Harmanec, Petr; Torres, Guillermo; et al. (1 August 2016). "NOMINAL VALUES FOR SELECTED SOLAR AND PLANETARY QUANTITIES: IAU 2015 RESOLUTION B3 * †". The Astronomical Journal. 152 (2): 41. arXiv:1510.07674. doi:10.3847/0004-6256/152/2/41. ISSN 0004-6256.
- ^ Bouvier, A.; Wadhwa, M. (2010). "The age of the Solar System redefined by the oldest Pb–Pb age of a meteoritic inclusion". Nature Geoscience. 3 (9): 637–641. Bibcode:2010NatGe...3..637B. doi:10.1038/NGEO941. S2CID 56092512.
- ^ Johnson, John Asher; Winn, Joshua N.; Albrecht, Simon; Howard, Andrew W.; Marcy, Geoffrey W.; Gazak, J. Zachary (2009). "A Third Exoplanetary System with Misaligned Orbital and Stellar Spin Axes". Publications of the Astronomical Society of the Pacific. 121 (884): 1104–1111. doi:10.1086/644604. ISSN 0004-6280.
