S Coronae Australis
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.[1]
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Corona Australis |
| Right ascension | 19h 01m 08.602s |
| Declination | −36° 57′ 19.95″ |
| Characteristics | |
| Spectral type | G0Ve+K0Ve |
| Astrometry | |
| Radial velocity (Rv) | −33 ± 5 km/s |
| Proper motion (μ) | RA: 7.8 ± 5.8 mas/yr Dec.: −21.9 ± 2.3 mas/yr |
| Details | |
| Other designations | |
S CrA, S Coronae Australis, HH 82 | |
| Database references | |
| SIMBAD | data |
References
- Carmona, A.; van den Ancker, M. E.; Henning, Th. (2007). "Optical spectroscopy of close companions to nearby Herbig Ae/Be and T Tauri stars". Astronomy and Astrophysics. 464 (2): 687–95. arXiv:astro-ph/0701208. Bibcode:2007A&A...464..687C. doi:10.1051/0004-6361:20065509. S2CID 14372262.
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