 A visual band light curve for S Coronae Australis, adapted from Mundt (1979). [1] The error bar shown on the left-most point applies to all points. | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Corona Australis |
| Right ascension | 19h 01m 08.59709s [2] |
| Declination | −36° 57′ 19.8950″ [2] |
| Apparent magnitude (V) | 10.91 [2] |
| Characteristics | |
| Spectral type | G0Ve + K0Ve [3] |
| Variable type | T Tau [3] |
| Astrometry | |
| Radial velocity (Rv) | −33 ± 5 [4] km/s |
| Proper motion (μ) | RA: −2.6 ± 5.8 [2] mas/yr Dec.: −9.8 ± 2.3 [2] mas/yr |
| Distance | 460 ly (140 [3] pc) |
| Details | |
| Other designations | |
S CrA, S Coronae Australis, HH 82 | |
| Database references | |
| SIMBAD | data |
S Coronae Australis (S CrA), is a young binary star system estimated to be around 2 million years old located in the constellation Corona Australis. It is composed of a G-type main sequence star that is about as luminous as and just over twice as massive as the Sun, and a smaller K-type main sequence star that has around 50-60% of the Sun's luminosity and 1.3 times its mass. Both stars are T Tauri stars and both show evidence of having circumstellar disks. The system is around 140 parsecs distant. [3]
Johann Friedrich Julius Schmidt discovered that the star is a variable star, in 1866. It appeared with its variable star designation in Annie Jump Cannon's 1907 work Second Catalogue of Variable Stars. [5]
