HD 23514, is a star in the Pleiades. It is a main-sequence star of class F6, and has been seen to have hot dust particles orbiting around it. These materials, otherwise known as planetesimals which orbit within a circumstellar disc, are evidence of possible planetary formation.[1] The debris disk shows evidence of being rich in silica.[2]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Taurus |
Right ascension | 03h 46m 38.3957s |
Declination | +22° 55′ 11.223″ |
Apparent magnitude (V) | 9.43 |
Characteristics | |
Spectral type | F6V |
U−B color index | 0.02 |
B−V color index | 0.50 |
Variable type | 13.14 |
Astrometry | |
Radial velocity (Rv) | 12.5 ± 02 km/s |
Proper motion (μ) | RA: 21.1 -43.0 mas/yr Dec.: 1.1 1.0 90 mas/yr |
Distance | 400 ly (122.641 pc) |
Details | |
Mass | 1.35 M☉ |
Radius | 1.28 R☉ |
Luminosity | 2.8 L☉ |
Temperature | 6400 K |
Metallicity | 9.95 |
Age | 0.1 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
The star system itself is very young, in the 35~100 million years range,[1] meaning that it is very well likely at the stage of forming planets.
HD 23514 has a brown dwarf companion (HD 23154 B), estimated to have a mass of about 0.06 ± 0.01 solar masses and a temperature of 2,600 ± 100K, and separated by about 360 AU from the primary.[1] The spectra of HD 23154 B have been found to have features typical of late-M dwarfs, including FeH absorption, strong CO bands and Na I absorption, and a near-infrared spectral type of M8 ± 1 has been proposed.[3]
The star will be continuously studied to confirm whether it may be a potential candidate for planetary formation.