Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
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 mas [1] |
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 AU from the star, and a cool component at 108±21 K with a separation of 22±8 AU. [5]