V488 Persei
From Wikipedia, the free encyclopedia
| 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[1] |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | K2–K2.5V[2] |
| Variable type | BY Draconis variable |
| Astrometry | |
| Radial velocity (Rv) | –1.02 ±0.88[3] km/s |
| Proper motion (μ) | RA: 23.370 ±0.013 mas/yr[3] Dec.: –25.879 ±0.013 mas/yr[3] |
| Parallax (π) | 5.7637±0.0121 mas[3] |
| Distance | 566 ± 1 ly (173.5 ± 0.4 pc) |
| Details[1] | |
| 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.[4] The star is a BY Draconis variable, which shows periodic variations due to starspots.[2] 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.[5]
Candidate wide companions around V488 Persei were identified in 2015.[6] Another work does point out problems with this approach, pointing out that wide companions cannot be distinguished from unrelated cluster members.[7]
