| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 03h46m 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 | |
HD 23514, SAO 76178, BD+22° 550, TYC 1800-1574-1, EPIC 210996505 | |
| Database references | |
| SIMBAD | data |
HD 23514, is a star in the Pleiades. It is a main-sequence starofclass 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]
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.
