ADS 9731
| Observation data Epoch Equinox J2000 | |
|---|---|
| Constellation | Corona Borealis |
| Right ascension | 15h 38m 12.91478s[1] |
| Declination | +36° 14′ 48.5597″[1] |
| Apparent magnitude (V) | 6.9 (total) |
| Characteristics | |
| Spectral type | F4V, F5V, G4V, F3V, F7V, M3V? [2] |
| Astrometry | |
| Parallax (π) | 8.52 ± 0.25 mas |
| Distance | 380 ± 10 ly (117 ± 3 pc) |
| Orbit | |
| Other designations | |
BD+36°2626, CCDM J15382+3615AB, HD 139691, WDS J15382+3615AB | |
| Database references | |
| SIMBAD | data |
ADS 9731 is a star system that consists of six stars. Four of the stars are visually separate in the sky, forming a visual star system, which was resolved using adaptive optics in 1995.[3] Two of these stars were themselves found to be spectroscopic binaries in 1998, resulting in a total of six known stars in the system.[2] It is one of very few multiple star systems known to have at least six members.[2] The components are organised thus: Aa and Ab are yellow-white main sequence stars of spectral types F4V and F5V and 1.35 and 1.32 solar masses respectively, which orbit each other every 3.27 days. This pair is in a 450-year orbit with star B, a star of spectral type G4V that has around the same mass as the Sun. Star C is a yellow white star of spectral type F3V around 1.41 times as massive as the sun, which has just started brightening and moving off the main sequence. It is in a 1000-year orbit with a pair of stars, Da and Db, a yellow-white main sequence star of spectral type F7V and a red dwarf of spectral type M3V. Da and Db take 14.28-days to orbit each other. Finally the system of stars C and Dab, and the system of stars Aab and B, take over 20,000 years to orbit each other.[2]
The combined light from the whole system results in an integrated V magnitude of 6.9. The parallax measured by the Hipparcos satellite indicates that the system is relatively nearby at around 110 parsecs (360 light-years) from the Sun.[1] However, this distance is highly uncertain because the multiple stars in the system prevented Hipparcos from accurately measuring the parallax; the system may instead be at a distance of about 200 pc (650 ly).[4]
The star system has been considered as a possible target for direct imaging searches for exoplanets,[5] but no planets have yet been detected in the system.
References
- 1 2 3 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
- 1 2 3 4 Tokovinin, A. A.; Shatskii, N. I.; Magnitskii, A. K. (1998). "ADS 9731: A new sextuple system". Astronomy Letters. 24: 795. Bibcode:1998AstL...24..795T.
- ↑ Drummond, Jack D.; Christou, Julian C.; Fugate, Robert Q. (1995). "Full Adaptive Optics Images of ADS 9731 and MU Cassiopeiae: Orbits and Masses". Astrophysical Journal. 450: 380. Bibcode:1995ApJ...450..380D. doi:10.1086/176148.
- ↑ Fabricius, C.; Makarov, V. V. (2000). "Hipparcos astrometry for 257 stars using Tycho-2 data". Astronomy and Astrophysics Supplement Series. 144: 45. Bibcode:2000A&AS..144...45F. doi:10.1051/aas:2000198.
- ↑ Janson, M. (2010). "The relevance of prior inclination determination for direct imaging of Earth-like planets". Monthly Notices of the Royal Astronomical Society. 408: 514. arXiv:1006.2941. Bibcode:2010MNRAS.408..514J. doi:10.1111/j.1365-2966.2010.17135.x.