Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Camelopardalis |
Right ascension | 05h 22m 33.5306s [1] |
Declination | +79° 13′ 52.143″ [1] |
Apparent magnitude (V) | 5.08 [2] |
Characteristics | |
Spectral type | F7V [3] |
U−B color index | −0.13 |
B−V color index | 0.506±0.002 [2] |
Astrometry | |
Radial velocity (Rv) | −11.09(13) [1] km/s |
Proper motion (μ) |
RA: −78.661(67)
mas/
yr
[1] Dec.: 162.098(77) mas/ yr [1] |
Parallax (π) | 48.1098 ± 0.0727 mas [1] |
Distance | 67.8 ± 0.1
ly (20.79 ± 0.03 pc) |
Absolute magnitude (MV) | 3.59 [4] |
Details | |
Mass | 1.29 [5] M☉ |
Radius | 1.51+0.02 −0.06 [6] R☉ |
Luminosity | 3.428±0.017 [6] L☉ |
Surface gravity (log g) | 4.22 [5] cgs |
Temperature | 6,396+135 −36 [6] K |
Metallicity [Fe/H] | 0.14 [5] dex |
Rotational velocity (v sin i) | 14.3 [5] km/s |
Age | 1.80 [5] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
HD 33564 (K Camelopardalis) is a single [7] star with an exoplanetary companion in the northern constellation of Camelopardalis. It has an apparent visual magnitude of 5.08, [2] which means it is a 5th magnitude star that is faintly visible to the naked eye. The system is located at a distance of 68 light years from the Sun based on parallax, and it is drifting closer with a radial velocity of −11 km/s. [1] It is a candidate member of the Ursa Major Moving Group. [8]
This is an ordinary F-type main-sequence star with a stellar classification of F7V, [3] indicating that the star is hotter and more massive than the Sun, giving it a yellow-white hue. The star is about two [5] billion years old and is chromospherically quiet, [9] with a projected rotational velocity of 14.3 km/s. It has about 1.5 [6] times the radius and 1.3 [5] times the mass of the Sun. The star is radiating 3.4 times the luminosity of the Sun from its photosphere at an effective temperature of 6,396 K. [5]
In September 2005, a massive planet was found on an eccentric orbit about the star, based on radial velocity variations measured by the ELODIE spectrograph. An infrared excess had been detected at a wavelength of 60 μm, suggesting the star may host a circumstellar disk. However, the existence of a disk is unlikely because the infrared radiation is coming from a background galaxy. [9]
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | >9.1 MJ | 1.1 | 388 ± 3 | 0.34 ± 0.02 | — | — |