RV Andromedae
Star in the constellation Andromeda
From Wikipedia, the free encyclopedia
RV Andromedae is a variable star in the constellation of Andromeda. It is classified as a semiregular variable pulsating giant star, and varies from an apparent visual magnitude of 11.5 at minimum brightness to a magnitude of 9.0 at maximum brightness, with a period of approximately 168.9 days.[3]
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 02h 11m 02.56581s[2] |
| Declination | 48° 56′ 45.0634″[2] |
| Apparent magnitude (V) | 9.0–11.5[3] |
| Characteristics | |
| Spectral type | M4e[3] |
| B−V color index | 1.607[4] |
| Variable type | Semi-regular[3] |
| Astrometry | |
| Radial velocity (Rv) | −10.0±2.0[5] km/s |
| Proper motion (μ) | RA: 10.456(48)[2] mas/yr Dec.: −0.958(56)[2] mas/yr |
| Parallax (π) | 1.0950±0.0483 mas[2] |
| Distance | 3,000 ± 100 ly (910 ± 40 pc) |
| Other designations | |
| BD+48 616, HIP 10192[5] | |
| Database references | |
| SIMBAD | data |
In 1904, English amateur astronomer Arthur Stanley Williams examined photographic plates taken during the previous two years and determined that RV Andromedae was a variable star whose period he estimated to be 182 days.[6] In 1907, Annie Jump Cannon listed it with its variable star designation in her Second Catalogue of Variable Stars.[7]
This is one of the Mira variables where mode switching of pulsations have been observed; amplitude and periods have been seen decreasing and subsequently increasing back to values near the previous ones.[8]
