Astronomy:50 Cancri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cancer |
| Right ascension | 08h 46m 56.01919s[1] |
| Declination | +12° 06′ 35.8305″[1] |
| Apparent magnitude (V) | 5.89[2] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | A1 Vp[3] |
| B−V color index | 0.120±0.005[2] |
| Variable type | None[4] |
| Astrometry | |
| Radial velocity (Rv) | 23.3±2.9[2] km/s |
| Proper motion (μ) | RA: −63.773[1] mas/yr Dec.: −50.694[1] mas/yr |
| Parallax (π) | 17.7961 ± 0.0792[1] mas |
| Distance | 183.3 ± 0.8 ly (56.2 ± 0.3 pc) |
| Absolute magnitude (MV) | +1.82±0.01[4] |
| Details | |
| Mass | 2.1[5] M☉ |
| Luminosity | 10.8±0.21[5] L☉ |
| Surface gravity (log g) | 4.40[6] cgs |
| Temperature | 8,340±48[5] K |
| Rotational velocity (v sin i) | 18[7] km/s |
| Age | 264[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
50 Cancri is a single[9] star in the zodiac constellation of Cancer, located 183 light years away from the Sun.[1] It has the Bayer designation A2 Cancri; 50 Cancri is the Flamsteed designation. It is faintly visible to the naked eye as a white-hued star with an apparent visual magnitude of 5.89.[2] The star is moving away from the Earth with a heliocentric radial velocity of 23 km/s, having come to within 118 light-years some 1.2 million years ago.[2]
This is a chemically peculiar A-type main-sequence star with a stellar classification of A1 Vp.[3] It is a Lambda Boötis star displaying strongly-depleted iron peak and alpha process elements, but otherwise relatively normal solar abundances.[5] The star shows no variability down to a detection limit of 1.6 millimagnitudes.[10] It is 264[6] million years old with a relatively low projected rotational velocity of 18 km/s.[7] 50 Cancri has 2.1[5] times the mass of the Sun and is radiating 11[5] times the Sun's luminosity from its photosphere at an effective temperature of 8,340 K.[5]
50 Cancri has an infrared excess, which most likely indicates a debris disk in orbit around the host star. A blackbody model of the emission shows a two component fit, with the warm section having a temperature of 246±91 K at a radius of 4±3 astronomical unit|AU from the star, and a cool component at 108±21 K with a separation of 22±8 AU.[5]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement 99: 135, doi:10.1086/192182, Bibcode: 1995ApJS...99..135A.
- ↑ 4.0 4.1 Paunzen, E. et al. (November 2002), "The status of Galactic field λ Bootis stars in the post-Hipparcos era", Monthly Notices of the Royal Astronomical Society 336 (3): 1030–1042, doi:10.1046/j.1365-8711.2002.05865.x, Bibcode: 2002MNRAS.336.1030P.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 Draper, Z. H. et al. (2016), "IR excesses around nearby Lambda Boo stars are caused by debris discs rather than ISM bow waves", Monthly Notices of the Royal Astronomical Society 456 (1): 459, doi:10.1093/mnras/stv2696, Bibcode: 2016MNRAS.456..459D.
- ↑ 6.0 6.1 6.2 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ 7.0 7.1 Zorec, J. et al. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics 537: A120, doi:10.1051/0004-6361/201117691, Bibcode: 2012A&A...537A.120Z.
- ↑ "50 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=50+Cnc.
- ↑ De Rosa, R. J. et al. (2014), "The VAST Survey - III. The multiplicity of A-type stars within 75 pc", Monthly Notices of the Royal Astronomical Society 437 (2): 1216, doi:10.1093/mnras/stt1932, Bibcode: 2014MNRAS.437.1216D.
- ↑ Paunzen, E. et al. (September 2002), "On the Period-Luminosity-Colour-Metallicity relation and the pulsational characteristics of lambda Bootis type stars", Astronomy and Astrophysics 392 (2): 515–528, doi:10.1051/0004-6361:20020854, Bibcode: 2002A&A...392..515P.
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