42 Cancri
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cancer |
| Right ascension | 08h 40m 43.20572s[1] |
| Declination | +19° 43′ 09.5359″[1] |
| Apparent magnitude (V) | 6.83[2] |
| Characteristics | |
| Spectral type | A7III[3] |
| B−V color index | 0.202±0.004[2] |
| Astrometry | |
| Radial velocity (Rv) | +34.6±0.9[2] km/s |
| Proper motion (μ) | RA: −36.167±0.102[1] mas/yr Dec.: −12.105±0.063[1] mas/yr |
| Parallax (π) | 5.2981 ± 0.0548 mas[1] |
| Distance | 616 ± 6 ly (189 ± 2 pc) |
| Absolute magnitude (MV) | 0.56[2] |
| Details | |
| Mass | 2.39±0.03[4] M☉ |
| Radius | 4.22±0.27[4] R☉ |
| Luminosity | 51.5±0.7[1] L☉ |
| Temperature | 7,607+258 −313[1] K |
| Metallicity [Fe/H] | −0.08±0.03[4] dex |
| Rotational velocity (v sin i) | 195[5] km/s |
| Age | 603±28[4] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
42 Cancri is a single[7] star in the northern zodiac constellation of Cancer. With an apparent visual magnitude of 6.83,[2] it is dimmer than what is considered the normal lower limit for visibility with the naked eye. The star is located at a distance of approximately 616 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +35 km/s.[2] 42 Cancri is a member of the Beehive Cluster (NGC 2632).[7]
The stellar classification of this star is A7III,[3] matching an A-type star that is in the giant stage. However, this may be a misclassification of a main sequence star.[8] It has also been classified as a spectroscopic binary,[5] although no orbital elements are published. 42 Cancri is an estimated 603[4] million years old and is spinning rapidly with a projected rotational velocity of 195 km/s.[5] The star has 2.39 times the mass of the Sun and 4.2 times the Sun's radius.[4] It is radiating 51.5[1] times the luminosity of the Sun from its photosphere at an effective temperature of 7,607 K.[1]
References
- ^ a b c d e f g h i 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 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.
- ^ a b 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, Bibcode:2001AJ....121.2148G, doi:10.1086/319956.
- ^ a b c d e f Bochanski, John J.; et al. (April 2018), "Fundamental Properties of Co-moving Stars Observed by Gaia", The Astronomical Journal, 155 (4): 17, arXiv:1801.00537, Bibcode:2018AJ....155..149B, doi:10.3847/1538-3881/aaaebe, 149.
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ a b c Treanor, P. J. (1960), "Stellar rotation in galactic open clusters", Monthly Notices of the Royal Astronomical Society, 121: 503, Bibcode:1960MNRAS.121..503T, doi:10.1093/mnras/121.6.503.
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ "42 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-08.
- ^ a b Mason, Brian D.; et al. (August 1993), "ICCD Speckle Observations of Binary Stars. IX. A Duplicity Survey of the Pleiades, Praesepe, and IC 4665 Clusters", Astronomical Journal, 106: 637, Bibcode:1993AJ....106..637M, doi:10.1086/116669.
- ^ Clampitt, Lori; Burstein, David (August 1997), "Spectrophotometry of 237 Stars in 7 Open Clusters", Astronomical Journal, 114: 699–712, arXiv:astro-ph/9705160, Bibcode:1997AJ....114..699C, doi:10.1086/118504.
