Summary
HD 94510 is a single[9] star in the southern constellation of Carina, positioned near the northern constellation border with Vela. It has the Bayer designation u Carinae; HD 94520 is the identifier from the Henry Draper Catalogue. This object has an orange hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +3.78.[2] The star is located at a distance of 95 light-years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +8 km/s.[2]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Carina |
| Right ascension | 10h 53m 29.65524s[1] |
| Declination | −58° 51′ 11.4163″[1] |
| Apparent magnitude (V) | +3.78[2] (3.75–3.80)[3] |
| Characteristics | |
| Evolutionary stage | subgiant[4] |
| Spectral type | K0IV[5] |
| B−V color index | +0.945±0.005[2] |
| Variable type | suspected |
| Astrometry | |
| Radial velocity (Rv) | +8.10±0.70[2] km/s |
| Proper motion (μ) | RA: +79.01±0.13[1] mas/yr Dec.: +38.47±0.12[1] mas/yr |
| Parallax (π) | 34.33 ± 0.13 mas[1] |
| Distance | 95.0 ± 0.4 ly (29.1 ± 0.1 pc) |
| Absolute magnitude (MV) | 1.46[2] |
| Details | |
| Mass | 1.60[4] M☉ |
| Radius | 7.55+0.93 −0.12[6] R☉ |
| Luminosity | 30.96±0.27[6] L☉ |
| Surface gravity (log g) | 3.00[7] cgs |
| Temperature | 4,955+41 −80[6] K |
| Metallicity [Fe/H] | −0.13[2] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
This is a K-type star in the subgiant[4] stage with a stellar classification of K0IV,[5] which indicates it has exhausted the supply of hydrogen at its core and is evolving into a giant. HD 94510 is a suspected variable star with a brightness that has been measured varying from magnitude 3.75 down to 3.80.[3] It has an estimated 1.60[4] times the mass of the Sun and has expanded to nearly eight[6] times the Sun's radius. The star is radiating 31 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,955 K.[6]
References edit
- ^ 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 f g 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 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.
- ^ a b c d Edvardsson, B. (January 1988), "Spectroscopic surface gravities and chemical compositions for 8 nearby single sub-giants.", Astronomy and Astrophysics, 190: 148–166, Bibcode:1988A&A...190..148E.
- ^ a b 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 c d e 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.
- ^ Alves, S.; et al. (April 2015), "Determination of the spectroscopic stellar parameters for 257 field giant stars", Monthly Notices of the Royal Astronomical Society, 448 (3): 2749–2765, arXiv:1503.02556, Bibcode:2015MNRAS.448.2749A, doi:10.1093/mnras/stv189.
- ^ "HD 94510". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-10.
- ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.