AA Tauri
 Artist's impresion of AA Tauri and possible substellar companion | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 34m 55.42s |
| Declination | +24° 28′ 53.2″ |
| Apparent magnitude (V) | 12.82 |
| Characteristics | |
| Spectral type | K7V |
| Variable type | T Tauri-type? |
| Astrometry | |
| Distance | ≈456.4 ly (≈140 pc) |
| Details | |
| Mass | 0.76[1] M☉ |
| Radius | 1.81[1] R☉ |
| Luminosity | 0.8[1] L☉ |
| Temperature | 4060[1] K |
| Age | 2.4[1] million years |
| Other designations | |
V* AA Tau, GCRV 55202, Kim 2-79, XEST 25-026, AN 196.1930, GSC 01833-00851, 2MASS J04345542+2428531, [ABG2007] 1651, CSI+24-04319, HBC 63, MHA 259-17, [FK83] LDN 1529 44, 2E 0431.8+2422, IRAS 04318+2422, UBV 4396, [GBA2007] 1766, 2E 1098 IRAS F04318+2422, XEST 25-OM-003 | |
AA Tauri is a young star in the constellation of Taurus, located in the young Taurus-Auriga Star Forming Region, roughly at 460 light years away from the Sun.
A possible planetary system
In their paper of 2003, Grinin et al. invoke the possible presence of a substellar object to explain peculiar and periodic eclipses occurring to the young star every 8.3 days.[2] They infer a mass of 20 times that of Jupiter for the perturbing object and an orbital separation of 0.08 Astronomical Units.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | ≤20 MJ | 0.08 | 8.5 | 0 | — | — |
References
- 1 2 3 4 5 Güdel; et al. (2007). "The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST)". Astronomy and Astrophysics. 468 (2): 353–377. arXiv:astro-ph/0609160
. Bibcode:2007A&A...468..353G. doi:10.1051/0004-6361:20065724. - ↑ Bouvier; et al. (2003). "Eclipses by circumstellar material in the T Tauri star AA Tau. II. Evidence for non-stationary magnetospheric accretion". Astronomy and Astrophysics. 409: 169–192. arXiv:astro-ph/0306551. Bibcode:2003A&A...409..169B. doi:10.1051/0004-6361:20030938.
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