| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Lyra |
| Right ascension | 18h 59m 45.48432s[1] |
| Declination | +26° 13′ 49.4487″[1] |
| Apparent magnitude (V) | 5.26[2] |
| Characteristics | |
| Spectral type | K2III[3] |
| B−V color index | 1.228±0.003[2] |
| Astrometry | |
| Radial velocity (Rv) | −22.56±0.13[1] km/s |
| Proper motion (μ) | RA: −85.671[1] mas/yr Dec.: −10.624[1] mas/yr |
| Parallax (π) | 12.2448 ± 0.0874 mas[1] |
| Distance | 266 ± 2 ly (81.7 ± 0.6 pc) |
| Absolute magnitude (MV) | 0.28[2] |
| Details | |
| Radius | 20.15+0.12 −0.99[1] R☉ |
| Luminosity | 128.0±1.6[1] L☉ |
| Surface gravity (log g) | 2.09[4] cgs |
| Temperature | 4,325+110 −13[1] K |
| Metallicity [Fe/H] | −0.28[4] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 176527 is a single[6] star in the northern constellation of Lyra, positioned near the southern constellation border with Vulpecula. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.26.[2] This object is located at a distance of approximately 266 light years from the Sun based on parallax,[1] and it has an absolute magnitude of 0.28.[2] It is drifting closer with a radial velocity of −22.6 km/s.[1]
This is an aging giant star with a stellar classification of K2III,[3] which indicates it has exhausted the supply of hydrogen at its core, then evolved away from the main sequence by cooling and expanding. At present it has 20[1] times the radius of the Sun. The star is radiating 128[1] times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,325 K.[1]
References
- ^ a b c d e f g h i j k l m n 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, S2CID 119257644.
- ^ a b Yoss, Kenneth M. (November 1961), "Spectral and Luminosity Classifications and Measurements of the Strength of Cyanogen Absorption for Late-Type Stars from Objective-Prism Spectra", Astrophysical Journal, 134: 809, Bibcode:1961ApJ...134..809Y, doi:10.1086/147209.
- ^ a b Jönsson, H.; et al. (February 2017), "Abundances of disk and bulge giants from high-resolution optical spectra. I. O, Mg, Ca, and Ti in the solar neighborhood and Kepler field samples", Astronomy & Astrophysics, 598: 11, arXiv:1611.05462, Bibcode:2017A&A...598A.100J, doi:10.1051/0004-6361/201629128, S2CID 49573306, A100.
- ^ "HD 176527". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-02-09.
- ^ 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.
This page was last edited on 14 May 2023, at 12:29