| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Equuleus |
| Right ascension | 20h 57m 16.28s [2] |
| Declination | +02° 58′ 44.6″ [2] |
| Apparent magnitude (V) | 9 - 13 [3] |
| Characteristics | |
| Evolutionary stage | (post?) AGB [4] |
| Spectral type | G - K III [4] |
| B−V color index | +1.6 [4] |
| Variable type | Lb [3] |
| Astrometry | |
| Radial velocity (Rv) | −75 [5] km/s |
| Proper motion (μ) | RA: 10.490 [6] mas/yr Dec.: −10.433 [6] mas/yr |
| Parallax (π) | 0.0985±0.0750 mas [6] |
| Distance | 3,340±700 [7] pc |
| Details | |
| Luminosity | 6,000 [7] L☉ |
| Temperature | 5,005 [6] K |
| Other designations | |
| IRAS 20547+0247, 2MASS J20571628+0258445, Gaia DR2 1731164844433296128 | |
| Database references | |
| SIMBAD | data |
U Equulei (U Equ / IRAS 20547+0247) is a variable star in the Equuleus constellation with an apparent magnitude of +14.50 in the B band. It lies at an estimated distance of 5,000 light-years (1,500 parsecs) from the Solar System.
U Equulei is, or was, an OH/IR star, and strong OH and H2O masers have been observed. These vary to a greater extent than almost any other star observed, and it is possible that the stage of maser activity is essentially finished. [8]
Lionel Siess and Mario Livio suggested that the accretion of a giant planet towards the increasing red giant has made the star's outer layers rotate fast enough to cause an outpouring equatorial- or disk-expansion, responsible for the star's peculiar environment. [9] The spectroscopic study has indicated the star is surrounded by the dust shell, but shape of the shell cannot be measured due to large distance to the star. [10]