Summary
TOI-1136 is a G-type main-sequence star 276 light-years (85 parsecs) away in the constellation Draco. It is slightly smaller than the Sun and similar in mass and temperature, but is much younger, with an age of about 700 million years. It hosts a system of at least six, and possibly seven, exoplanets.[3]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Draco[1] |
| Right ascension | 12h 48m 44.37261s[2] |
| Declination | +64° 51′ 19.1475″[2] |
| Apparent magnitude (V) | 9.534[3] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | G5[4] |
| Apparent magnitude (B) | 10.16±0.03[4] |
| Apparent magnitude (V) | 9.534±0.003[3] |
| Apparent magnitude (G) | 9.376±0.003[2] |
| Apparent magnitude (J) | 8.363±0.020[4] |
| Apparent magnitude (H) | 8.088±0.018[4] |
| Apparent magnitude (K) | 8.034±0.021[4] |
| Astrometry | |
| Radial velocity (Rv) | 7.51±0.20[2] km/s |
| Proper motion (μ) | RA: 1.216 mas/yr[2] Dec.: -10.045 mas/yr[2] |
| Parallax (π) | 11.8236 ± 0.0108 mas[2] |
| Distance | 275.9 ± 0.3 ly (84.58 ± 0.08 pc) |
| Details[3] | |
| Mass | 1.022±0.027 M☉ |
| Radius | 0.968±0.036 R☉ |
| Surface gravity (log g) | 4.47±0.04 cgs |
| Temperature | 5770±50 K |
| Metallicity [Fe/H] | 0.07±0.06 dex |
| Rotation | 8.42±0.09 d[5] |
| Rotational velocity (v sin i) | 6.7±0.6 km/s |
| Age | 700±150 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Planetary system edit
TOI-1136 was discovered to have six transiting planets in 2022 using the Transiting Exoplanet Survey Satellite (TESS), all orbiting closer to their star than Mercury is to the Sun.[3] All of them are Neptune-sized or mini-Neptunes, and their masses have been measured using a combination of radial velocity and transit-timing variations, showing them to have low densities.[5] The planets are in an orbital resonance, with period ratios near 3:2, 2:1, 3:2, 7:5, and 3:2.[3]
A possible single transit of a seventh planet was also identified. This candidate planet would also be sub-Neptune-sized, but its orbit is poorly constrained. If this is confirmed, it would make TOI-1136 one of the largest known planetary systems.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 3.50+0.8 −0.7 M🜨 |
0.05106±0.0009 | 4.1727±0.0003 | 0.027±0.009 | 86.44+0.27 −0.21° |
1.90+0.21 −0.15 R🜨 |
| c | 6.32+1.1 −1.3 M🜨 |
0.0669±0.0005 | 6.2574±0.0002 | 0.11±0.01 | 89.42+0.39 −0.55° |
2.879+0.060 −0.062 R🜨 |
| d | 8.35+1.8 −1.6 M🜨 |
0.1062±0.0008 | 12.5199±0.0004 | 0.042±0.004 | 89.41±0.28° | 4.627+0.077 −0.072 R🜨 |
| e | 6.07+1.09 −1.01 M🜨 |
0.139±0.002 | 18.801±0.001 | 0.0425±0.004 | 89.31+0.26 −0.18° |
2.639+0.072 −0.088 R🜨 |
| f | 9.7+3.9 −3.7 M🜨 |
0.174±0.002 | 26.321±0.001 | 0.001±0.001 | 89.38+0.22 −0.17° |
3.88±0.11 R🜨 |
| g | 5.6+4.1 −3.2 M🜨 |
0.229±0.003 | 39.545±0.002 | 0.04±0.01 | 89.65+0.18 −0.13° |
2.53+0.11 −0.12 R🜨 |
| h (unconfirmed) | <18.8 M🜨 | ~0.36 | ~77 | 0.04+0.05 −0.03 |
89.68±0.02° | 2.68+0.20 −0.18 R🜨 |
See also edit
References edit
- ^ "Finding the constellation which contains given sky coordinates". djm.cc. 2 August 2008. Archived from the original on 15 August 2019. Retrieved 11 December 2023.
- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f g Dai, Fei; Masuda, Kento; et al. (February 2023). "TOI-1136 is a Young, Coplanar, Aligned Planetary System in a Pristine Resonant Chain". The Astronomical Journal. 165 (2): 33. arXiv:2210.09283. Bibcode:2023AJ....165...33D. doi:10.3847/1538-3881/aca327.
- ^ a b c d e f "TOI-1136". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 10 December 2023.
- ^ a b c d Beard, Corey; Robertson, Paul; et al. (December 2023). "The TESS-Keck Survey XVII: Precise Mass Measurements in a Young, High Multiplicity Transiting Planet System using Radial Velocities and Transit Timing Variations". The Astronomical Journal. arXiv:2312.04635.