HD 125072
HD 125072 is a star in the southern constellation of Centaurus. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.637.[2] The star is located at a distance of 38.6 light years from the Sun based on parallax.[1] It is drifting closer with a radial velocity of −14.9 km/s.[5] The components of the space velocity for this star are U=−18.5, V=−6.9 and W=−26.9 km/s.[7]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 14h 19m 04.83414s[1] |
| Declination | −59° 22′ 44.5272″[1] |
| Apparent magnitude (V) | 6.637[2] |
| Characteristics | |
| Spectral type | K3 IV[3] |
| U−B color index | +0.905[4] |
| B−V color index | +1.025[4] |
| Astrometry | |
| Radial velocity (Rv) | −14.9[5] km/s |
| Proper motion (μ) | RA: −454.895[1] mas/yr Dec.: −810.729[1] mas/yr |
| Parallax (π) | 84.4535 ± 0.0349 mas[1] |
| Distance | 38.62 ± 0.02 ly (11.841 ± 0.005 pc) |
| Absolute magnitude (MV) | 6.28[2] |
| Details | |
| Mass | 0.806±0.017[6] M☉ |
| Radius | 0.83+0.02 −0.01[1] R☉ |
| Luminosity | 0.347±0.001[1] L☉ |
| Surface gravity (log g) | 4.48[3] cgs |
| Temperature | 4,858+47 −59[1] K |
| Metallicity [Fe/H] | −0.70[7] dex |
| Rotational velocity (v sin i) | 3.97[8] km/s |
| Age | 9.98[7] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The stellar classification of this star is K3 IV,[3] matching a K-type subgiant that is evolving into a giant. It has 81%[6] of the Sun's mass and 83%[1] of the radius of the Sun. The star is radiating 34.7% of the Sun's luminosity from its photosphere at an effective temperature of 4,858 K.[1] Based on the composition and kinematics of this star, it has an estimated age of about 10 billion years.[7] It is spinning with a projected rotational velocity of 4 km/s.[8]
References edit
- ^ a b c d e f g h i j k 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 Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511
- ^ a b c Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992
- ^ a b Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M
- ^ a b Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E
- ^ a b Tsantaki, M.; et al. (July 2013), "Deriving precise parameters for cool solar-type stars. Optimizing the iron line list", Astronomy & Astrophysics, 555: A150, arXiv:1304.6639, Bibcode:2013A&A...555A.150T, doi:10.1051/0004-6361/201321103, S2CID 118388752.
- ^ a b c d Lachaume, R.; et al. (1999). "Age determinations of main-sequence stars: combining different methods". Astronomy and Astrophysics. 348: 897–909. Bibcode:1999A&A...348..897L.
- ^ a b Martínez-Arnáiz, R.; et al. (September 2010). (PDF). Astronomy and Astrophysics. 520: A79. arXiv:1002.4391. Bibcode:2010A&A...520A..79M. doi:10.1051/0004-6361/200913725. S2CID 43455849. Archived from the original (PDF) on 2017-09-22. Retrieved 2018-11-04.
- ^ "HD 125072". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-11-08.