V488 Persei
V488 Persei (blue star in the middle) with the Zwicky Transient Facility | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 03h 28m 18.68s |
| Declination | +48° 39′ 48.19″ |
| Apparent magnitude (V) | 12.89 ±0.05 |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | K2–K2.5V |
| Variable type | BY Draconis variable |
| Astrometry | |
| Radial velocity (Rv) | –1.02 ±0.88 km/s |
| Proper motion (μ) | RA: 23.370 ±0.013 mas/yr Dec.: –25.879 ±0.013 mas/yr |
| Parallax (π) | 5.7637±0.0121 mas |
| Distance | 566 ± 1 ly (173.5 ± 0.4 pc) |
| Details | |
| Mass | 0.84 M☉ |
| Radius | 0.76 R☉ |
| Luminosity | 0.25 L☉ |
| Temperature | 4700 K |
| Rotation | 5.8 days |
| Rotational velocity (v sin i) | 4.5 ±1.5 km/s |
| Age | 80 Myr |
| Other designations | |
| Cl* Melotte 20 AP 70, 2MASS J03281868+4839482, TIC 410731676, V* V488 Per, WISEA J032818.69+483947.9, Gaia DR2 249236647249997696, AP J03281868+4839482, ATO J052.0779+48.6632 | |
| Database references | |
| SIMBAD | data |
V488 Persei is a variable star in the constellation Perseus. The star was first identified as a variable in 1985 from data of a 0.9 m telescope at Kitt Peak. The survey targeted stars of the Alpha Persei Cluster, for which the researchers found a few stars to be variable. The star AP 70, later called V488 Persei was found to be variable with a period of 123.5 hours. The star is a BY Draconis variable, which shows periodic variations due to starspots. In 2012 researchers found a debris disk with extreme infrared excess. The researchers suggested that this dust is the aftermath of the collision between two planetary embryos.
Candidate wide companions around V488 Persei were identified in 2015. Another work does point out problems with this approach, pointing out that wide companions cannot be distinguished from unrelated cluster members.