Astronomy:17 Crateris
| Observation data {{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0 Equinox J2000.0 (ICRS)| Epoch J2000 [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}} | |
|---|---|
| Constellation | Hydra |
| 17 Crt A | |
| Right ascension | 11h 32m 16.40436s[1] |
| Declination | −29° 15′ 39.6740″[1] |
| Apparent magnitude (V) | 5.64[2] |
| 17 Crt B | |
| Right ascension | 11h 32m 16.03998s[1] |
| Declination | −29° 15′ 47.8935″[1] |
| Apparent magnitude (V) | 5.76[2] |
| Characteristics | |
| Spectral type | F8V + F8V[2] |
| B−V color index | 0.540±0.004[3] |
| Astrometry | |
| 17 Crt A | |
| Radial velocity (Rv) | +5.8±0.4[4] km/s |
| Proper motion (μ) | RA: −19.601[1] mas/yr Dec.: +144.524[1] mas/yr |
| Parallax (π) | 36.0601 ± 0.1266[1] mas |
| Distance | 90.4 ± 0.3 ly (27.73 ± 0.10 pc) |
| 17 Crt B | |
| Proper motion (μ) | RA: −22.025[1] mas/yr Dec.: +139.982[1] mas/yr |
| Parallax (π) | 35.9838 ± 0.1320[1] mas |
| Distance | 90.6 ± 0.3 ly (27.8 ± 0.1 pc) |
| Details[5] | |
| 17 Crt A | |
| Mass | 1.20 M☉ |
| Luminosity | 3.2 L☉ |
| Surface gravity (log g) | 4.17 cgs |
| Temperature | 6,240 K |
| Metallicity [Fe/H] | 0.04±0.15[6] dex |
| Rotational velocity (v sin i) | 10.0 km/s |
| Age | 3.95 Gyr |
| 17 Crt B | |
| Mass | 1.18 M☉ |
| Luminosity | 2.8 L☉ |
| Surface gravity (log g) | 4.20 cgs |
| Temperature | 6,269 K |
| Rotational velocity (v sin i) | 9.6 km/s |
| Age | 3.67 Gyr |
| Other designations | |
| 17 Crt A: {{{names1}}} | |
| 17 Crt B: {{{names2}}} | |
| Database references | |
| SIMBAD | data |
17 Crateris is a wide binary star[8] system in the equatorial constellation of Hydra, located 90.5 light years away from the Sun. It is visible to the naked eye as a faint, yellow-white hued star with a combined apparent visual magnitude of 4.93.[3] The system is traversing the celestial sphere with a relative proper motion of 24.9 mas/y,[9] and is moving away from the Earth with a heliocentric radial velocity of +5.8 km/s.[4]
The dual nature of this system was discovered by W. Herschel in 1783, when they showed an angular separation of 9.8″. As of 2015, the two components of this system had a separation of 9.60″ along a position angle of 210°.[10] This is equivalent to a projected separation of 241.3 astronomical unit|AU; wide enough that, thus far, their orbital track appears linear.[9] They are nearly identical F-type main-sequence stars with a stellar classification of F8V.[2] The primary is slightly brighter at magnitude 5.64, while the secondary is magnitude 5.76.[2]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.
- ↑ 2.0 2.1 2.2 2.3 2.4 Gray, R. O. et al. (2001), "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars", The Astronomical Journal 121 (4): 2148, doi:10.1086/319956, Bibcode: 2001AJ....121.2148G.
- ↑ 3.0 3.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 4.0 4.1 Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters 32 (11): 759–771, doi:10.1134/S1063773706110065, Bibcode: 2006AstL...32..759G.
- ↑ Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal 153 (1): 19, doi:10.3847/1538-3881/153/1/21, 21, Bibcode: 2017AJ....153...21L.
- ↑ Gáspár, András et al. (2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal 826 (2): 171, doi:10.3847/0004-637x/826/2/171, Bibcode: 2016ApJ...826..171G.
- ↑ "17 Crt". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=17+Crt.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 9.0 9.1 Tokovinin, A.; Kiyaeva, O. (February 2016), "Eccentricity distribution of wide binaries", Monthly Notices of the Royal Astronomical Society 456 (2): 2070−2079, doi:10.1093/mnras/stv2825, Bibcode: 2016MNRAS.456.2070T.
- ↑ Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M, http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/wds, retrieved 2015-07-22.
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