Astronomy:ADS 9731
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Corona Borealis |
| Right ascension | 15h 38m 12.91478s[1] |
| Declination | +36° 14′ 48.5597″[1] |
| Apparent magnitude (V) | 6.9 (total)[citation needed] |
| Characteristics | |
| Spectral type | F4V, F5V, G4V, F3V, F7V, M3V?[2] |
| Astrometry | |
| A | |
| Proper motion (μ) | RA: 73.197[3] mas/yr Dec.: −57.740[3] mas/yr |
| Parallax (π) | 9.0945 ± 0.0175[3] mas |
| Distance | 358.6 ± 0.7 ly (110.0 ± 0.2 pc) |
| B | |
| Proper motion (μ) | RA: 71.824[4] mas/yr Dec.: −54.140[4] mas/yr |
| Parallax (π) | 9.1101 ± 0.0307[4] mas |
| Distance | 358 ± 1 ly (109.8 ± 0.4 pc) |
| C | |
| Proper motion (μ) | RA: 75.165[5] mas/yr Dec.: −59.731[5] mas/yr |
| Parallax (π) | 9.0970 ± 0.0199[5] mas |
| Distance | 358.5 ± 0.8 ly (109.9 ± 0.2 pc) |
| D | |
| Proper motion (μ) | RA: 72.818[6] mas/yr Dec.: −58.281[6] mas/yr |
| Parallax (π) | 9.0870 ± 0.0322[6] mas |
| Distance | 359 ± 1 ly (110.0 ± 0.4 pc) |
| Orbit | |
| Other designations | |
| Database references | |
| SIMBAD | data |
ADS 9731 is a star system that consists of six stars, located in the constellation of Corona Borealis. Four of the stars are visually separate in the sky, forming a visual star system, which was resolved using adaptive optics in 1995.[7] 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]
| Aa | |||||||||||||||
| Period = 3.27 d | |||||||||||||||
| Ab | |||||||||||||||
| Period = 450 y | |||||||||||||||
| B | |||||||||||||||
| Period = 20,000 y | |||||||||||||||
| C | |||||||||||||||
| Period = 1000 y | |||||||||||||||
| Da | |||||||||||||||
| Period = 14.28 d | |||||||||||||||
| Db | |||||||||||||||
Hierarchy of orbits
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. Published apparent magnitudes for the components vary greatly and some are certainly in error,[2] but components A, B, C, and D are approximately of visual magnitude 8, 10, 9, and 9 respectively.[8] Models of all six components show that Aa and Ab have magnitudes 8.5 and 8.7 respectively while the faint secondary to component D is about 16th magnitude. The CD pair is slightly brighter than the AB pair, although component A is slightly brighter than component C.[2]
Gaia EDR3 catalogues parallaxes for the four resolved stars, all at a distance of 360 light-years (110 pc) with a statistical margin of error of less than a parsec.
The star system has been considered as a possible target for direct imaging searches for exoplanets,[9] but no planets have yet been detected in the system.
References
- ↑ 1.0 1.1 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Tokovinin, A. A.; Shatskii, N. I.; Magnitskii, A. K. (1998). "ADS 9731: A new sextuple system". Astronomy Letters 24 (6): 795. Bibcode: 1998AstL...24..795T.
- ↑ 3.0 3.1 3.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 4.0 4.1 4.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 5.0 5.1 5.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 6.0 6.1 6.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 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. doi:10.1086/176148. Bibcode: 1995ApJ...450..380D.
- ↑ Mason, B. D. et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode: 2001AJ....122.3466M. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/wds. Retrieved 2015-07-22.
- ↑ Janson, M. (2010). "The relevance of prior inclination determination for direct imaging of Earth-like planets". Monthly Notices of the Royal Astronomical Society 408 (1): 514–521. doi:10.1111/j.1365-2966.2010.17135.x. Bibcode: 2010MNRAS.408..514J.
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