Summary
HD 24496 is a binary star[9] system in the equatorial constellation of Taurus. The combined apparent visual magnitude of the pair is 6.81,[2] which is too faint to be readily visible to the normal human eye. The system is located at a distance of 66.8 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +19 km/s.[2] It is traversing the celestial sphere with a proper motion of 0.276″ per year.[10]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 03h 54m 28.03326s[1] |
| Declination | +16° 36′ 57.7897″[1] |
| Apparent magnitude (V) | 6.81[2] (6.9 + 11.1)[3] |
| Characteristics | |
| Spectral type | G7V[4] + M2V[5] |
| Apparent magnitude (B) | 7.529[2] |
| Apparent magnitude (R) | 6.40[2] |
| Apparent magnitude (I) | 6.000[2] |
| Apparent magnitude (J) | 5.384±0.024[2] |
| Apparent magnitude (H) | 5.102±0.026[2] |
| Apparent magnitude (K) | 4.995±0.017[2] |
| B−V color index | 0.719±0.001[2] |
| Astrometry | |
| Radial velocity (Rv) | +18.99±0.09[2] km/s |
| Proper motion (μ) | RA: +214.191[1] mas/yr Dec.: −167.336[1] mas/yr |
| Parallax (π) | 48.8107 ± 0.0474 mas[1] |
| Distance | 66.82 ± 0.06 ly (20.49 ± 0.02 pc) |
| Absolute magnitude (MV) | 5.26[2] |
| Details[6] | |
| A | |
| Mass | 0.956+0.030 −0.036 M☉ |
| Radius | 0.91±0.03 R☉ |
| Luminosity | 0.705+0.073 −0.076 L☉ |
| Surface gravity (log g) | 4.52+0.03 −0.04 cgs |
| Temperature | 5,572±44 K |
| Metallicity [Fe/H] | −0.01±0.03 dex |
| Rotational velocity (v sin i) | 0.0±0.5 km/s |
| Age | 3.316+3.88 −3.16 Gyr |
| B | |
| Mass | 0.53[7] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
The magnitude 6.9[3] primary star, designated component A, is a G-type main-sequence star with a stellar classification of G7V.[4] It is around three billion years old with a low projected rotational velocity. The star has 96% of the mass of the Sun and 91% of the Sun's radius. The metallicity, what astronomers term the abundance of heavier elements, is about the same as in the Sun. The star is radiating 71% of the luminosity of the Sun from its photosphere at an effective temperature of 5,572 K.[6]
The secondary companion, component B, is a magnitude 11.1[3] red dwarf of class M2V[5] that shares a common proper motion with the primary.[11] They have an angular separation of 2.7″ along a position angle of 256°, which is equivalent to a physical projected separation of 55.2 AU.[5] Their orbital period is around 123,000 years.[7]
References edit
- ^ a b c d e f 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 f g h i j k l 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 c Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
- ^ a b Koen, C.; et al. (2010), "UBV(RI)C JHK observations of Hipparcos-selected nearby stars", Monthly Notices of the Royal Astronomical Society, 403 (4): 1949, Bibcode:2010MNRAS.403.1949K, doi:10.1111/j.1365-2966.2009.16182.x.
- ^ a b c Raghavan, Deepak; et al. (September 2010), "A Survey of Stellar Families: Multiplicity of Solar-type Stars", The Astrophysical Journal Supplement, 190 (1): 1–42, arXiv:1007.0414, Bibcode:2010ApJS..190....1R, doi:10.1088/0067-0049/190/1/1, S2CID 368553.
- ^ a b Marsden, S. C.; et al. (November 2014), "A BCool magnetic snapshot survey of solar-type stars", Monthly Notices of the Royal Astronomical Society, 444 (4): 3517–3536, arXiv:1311.3374, Bibcode:2014MNRAS.444.3517M, doi:10.1093/mnras/stu1663, S2CID 53988884.
- ^ a b Tokovinin, Andrei (2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 87, arXiv:1401.6827, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, S2CID 56066740.
- ^ "HD 24496". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-10.
- ^ Fuhrmann, K.; et al. (February 2017), "Multiplicity among Solar-type Stars", The Astrophysical Journal, 836 (1): 23, Bibcode:2017ApJ...836..139F, doi:10.3847/1538-4357/836/1/139, 139.
- ^ 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.
- ^ Abt, Helmut A.; Willmarth, Daryl (January 2006), "The Secondaries of Solar-Type Primaries. I. The Radial Velocities", The Astrophysical Journal Supplement Series, 162 (1): 207–226, Bibcode:2006ApJS..162..207A, doi:10.1086/498095, S2CID 123629445.