| |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 01h57m 48.97759s[2] |
| Declination | −21° 54′ 05.3411″[2] |
| Apparent magnitude (V) | 8.00[3] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | G4V[3] |
| Variable type | BY Dra |
| Astrometry | |
| Radial velocity (Rv) | +5.7±0.3[4] km/s |
| Proper motion (μ) | RA: +103.633[2] mas/yr Dec.: −50.437[2] mas/yr |
| Parallax (π) | 24.2053 ± 0.0243 mas[2] |
| Distance | 134.7 ± 0.1 ly (41.31 ± 0.04 pc) |
| Absolute magnitude (MV) | 5.03[5][6] |
| Details | |
| Mass | 1.02[7] M☉ |
| Radius | 1.0[2] R☉ |
| Luminosity | 0.89[8] L☉ |
| Surface gravity (log g) | 4.39[2] cgs |
| Temperature | 5,585[5][6] K |
| Metallicity [Fe/H] | −0.28[5][6] dex |
| Rotational velocity (v sin i) | 15.2[9] km/s |
| Age | 7.5−8[8] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 12039, also known as DK Ceti, is a variable star in the constellationofCetus at a distance of 135 ly (41 pc). It is categorized as a BY Draconis variable because of luminosity changes caused by surface magnetic activity coupled with rotation of the star.[10] The stellar classification G4V is similar to the Sun, indicating this is a main sequence star that is generating energy at its core through the thermonuclear fusion of hydrogen. The effective temperature of 5,585 K[5] gives the star a yellow hue. It has about the same mass as the Sun, but only emits 89% of the Sun's luminosity. This is a young star with age estimates ranging from 7.5−8 million years[11] to 30 million years.[7]
In 2006, a debris field was discovered in orbit around this star using infrared observations by the Spitzer Space Telescope. This debris is thought to be an asteroid belt. The measured temperature of the debris is 110 K, which places it in an orbit between 4 and 6 AU from the star, or about the same distance where Jupiter orbits the Sun.[12] This debris disk may have been created by the breakup of a single, 100 km diameter planetesimal through a collision.[13] The star system does not show any excess emission at 70 μm, indicating it does not have a cold outer dust disk.[14]
The star was examined for the presence of an extrasolar planet with a mass in the range 2-10 Jupiter masses and an orbital distance of 3-15.5 AU. Instead, in 2007, a close stellar companion was likely discovered. This object is separated from the primary by 0.15 arcseconds, making it unlikely to be a background object.[15]
This star has been proposed as a member of the Tucana-Horologium association (Tuc-Hor), a stream of young stars with a common motion through space. The Tuc-Hor association is about 30 million years old.[16][17] The space velocity components of this star are [U, V, W] = [−0.6, −16.3, 5.0] km/s.[11] It is orbiting the Milky Way galaxy with an orbital eccentricity of 0.06, with a distance that varies from 7.11−8.01 kpc of the galactic core. The inclination of its orbit carries it as far as 90 parsecs above the galactic plane.[6]
