Iota Crateris
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Crater |
| Right ascension | 11h 38m 40.01668s[1] |
| Declination | −13° 12′ 06.9963″[1] |
| Apparent magnitude (V) | 5.48[2] |
| Characteristics | |
| Spectral type | F6.5 V[3] |
| B−V color index | +0.52[2] |
| Astrometry | |
| Radial velocity (Rv) | −26.6±0.3[4] km/s |
| Proper motion (μ) | RA: +99.52[1] mas/yr Dec.: +125.99[1] mas/yr |
| Parallax (π) | 37.41 ± 0.30 mas[1] |
| Distance | 87.2 ± 0.7 ly (26.7 ± 0.2 pc) |
| Absolute magnitude (MV) | +3.33[5] |
| Details | |
| ι Crt A | |
| Mass | 1.19+0.06 −0.02[6] M☉ |
| Surface gravity (log g) | 4.27±0.03[7] cgs |
| Temperature | 6,230±21[7] K |
| Metallicity [Fe/H] | −0.15±0.01[7] dex |
| Age | 4.45+0.32 −0.94[6] Gyr |
| ι Crt B | |
| Mass | 0.57[8] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
Iota Crateris (ι Crateris) is the Bayer designation for a binary star[10] system in the southern constellation of Crater. It is faintly visible to the naked eye with an apparent visual magnitude of 5.48.[2] According to the Bortle scale, this means it can be viewed from suburban skies at night. Based upon an annual parallax shift of 37.41 mas,[1] Iota Crateris is located 87 light years from the Sun.
This is an astrometric binary system with an estimated orbital period of roughly 79,000 years.[10] The primary, component A, is an F-type main sequence star with a stellar classification of F6.5 V,[3] which is generating energy through the thermonuclear fusion of hydrogen in its core region. It is around 4.45[6] billion years old with 1.19[6] times the mass of the Sun. The star is radiating energy from its outer atmosphere at an effective temperature of 6,230 K.[7]
The companion, component B, is a red dwarf star with a probable classification of M3, although its mass estimate of 0.57 solar would be more consistent with an M0 class star.[8] As of 2014, this magnitude 11.0 star had an angular separation of 1.10 arc seconds along a position angle of 248°.[11] It has a projected separation of 25 AU,[8] which means it is positioned at least this distance away from the primary.
References
- ^ 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.
- ^ a b c Corben, P. M.; Stoy, R. H. (1968), "Photoelectric Magnitudes and Colours for Bright Southern Stars", Monthly Notes of the Astronomical Society of Southern Africa, 27: 11, Bibcode:1968MNSSA..27...11C.
- ^ 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.
- ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, A61.
- ^ Lambert, David L.; Reddy, Bacham E. (April 2004), "Lithium abundances of the local thin disc stars", Monthly Notices of the Royal Astronomical Society, 349 (2): 757−767, arXiv:astro-ph/0401259, Bibcode:2004MNRAS.349..757L, doi:10.1111/j.1365-2966.2004.07557.x.
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ a b c d Ramírez, I.; et al. (September 2012), "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets", The Astrophysical Journal, 756 (1): 46, arXiv:1207.0499, Bibcode:2012ApJ...756...46R, doi:10.1088/0004-637X/756/1/46.
- ^ a b c d Adibekyan, V.; et al. (August 2016), "Abundance trend with condensation temperature for stars with different Galactic birth places", Astronomy & Astrophysics, 592: 12, arXiv:1606.04714, Bibcode:2016A&A...592A..87A, doi:10.1051/0004-6361/201628883, A87.
- ^ a b c Ehrenreich, D.; et al. (November 2010), "Deep infrared imaging of close companions to austral A- and F-type stars", Astronomy and Astrophysics, 523: 41, arXiv:1007.0002, Bibcode:2010A&A...523A..73E, doi:10.1051/0004-6361/201014763, A73.
- ^ "iot Crt -- Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-02-26.
- ^ a b Tokovinin, Andrei (2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 14, arXiv:1401.6827, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, 87.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122: 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
