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50 Cancri

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Star in the constellation Cancer This article is about A Cancri. For other stars with this Bayer designation, see A Cancri.
50 Cancri
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cancer
Right ascension 08 46 56.01919
Declination +12° 06′ 35.8305″
Apparent magnitude (V) 5.89
Characteristics
Evolutionary stage main sequence
Spectral type A1 Vp
B−V color index 0.120±0.005
Variable type None
Astrometry
Radial velocity (Rv)23.3±2.9 km/s
Proper motion (μ) RA: −63.773 mas/yr
Dec.: −50.694 mas/yr
Parallax (π)17.7961 ± 0.0792 mas
Distance183.3 ± 0.8 ly
(56.2 ± 0.3 pc)
Absolute magnitude (MV)+1.82±0.01
Details
Mass2.1 M
Luminosity10.8±0.21 L
Surface gravity (log g)4.40 cgs
Temperature8,340±48 K
Rotational velocity (v sin i)18 km/s
Age264 Myr
Other designations
A Cancri, 50 Cnc, BD+12°1904, HD 74873, HIP 43121, HR 3481, SAO 98117
Database references
SIMBADdata

50 Cancri is a single star in the zodiac constellation of Cancer, located 183 light years away from the Sun. It has the Bayer designation A 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. 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.

This is a chemically peculiar A-type main-sequence star with a stellar classification of A1 Vp. It is a Lambda Boötis star displaying strongly-depleted iron peak and alpha process elements, but otherwise relatively normal solar abundances. The star shows no variability down to a detection limit of 1.6 millimagnitudes. It is 264 million years old with a relatively low projected rotational velocity of 18 km/s. 50 Cancri has 2.1 times the mass of the Sun and is radiating 11 times the Sun's luminosity from its photosphere at an effective temperature of 8,340 K.

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 AU from the star, and a cool component at 108±21 K with a separation of 22±8 AU.

References

  1. ^ 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.
  2. ^ 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.
  3. ^ Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement, 99: 135, Bibcode:1995ApJS...99..135A, doi:10.1086/192182.
  4. ^ 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, arXiv:astro-ph/0207488, Bibcode:2002MNRAS.336.1030P, doi:10.1046/j.1365-8711.2002.05865.x, S2CID 2389489.
  5. ^ 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, arXiv:1511.05919, Bibcode:2016MNRAS.456..459D, doi:10.1093/mnras/stv2696, S2CID 118343020.
  6. ^ 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, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  7. ^ Zorec, J.; et al. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  8. "50 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-06.
  9. 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, arXiv:1311.7141, Bibcode:2014MNRAS.437.1216D, doi:10.1093/mnras/stt1932, S2CID 88503488.
  10. 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, arXiv:astro-ph/0207494, Bibcode:2002A&A...392..515P, doi:10.1051/0004-6361:20020854, S2CID 54666586.
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