TOI-1136
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Draco[1] |
| Right ascension | 12h48m44.37261s[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:1.216mas/yr[2] Dec.:-10.045mas/yr[2] |
| Parallax(π) | 11.8236 ± 0.0108mas[2] |
| Distance | 275.9 ± 0.3ly (84.58 ± 0.08pc) |
| Details[3] | |
| Mass | 1.022±0.027M☉ |
| Radius | 0.968±0.036R☉ |
| Surface gravity(logg) | 4.47±0.04cgs |
| Temperature | 5770±50K |
| Metallicity[Fe/H] | 0.07±0.06dex |
| Rotation | 8.42±0.09d[5] |
| Rotational velocity(vsini) | 6.7±0.6km/s |
| Age | 700±150Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
TOI-1136is aG-type main-sequence star276light-years(85parsecs) away in the constellationDraco.It is slightly smaller than theSunand 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]
Planetary system
[edit]TOI-1136 was discovered to have sixtransitingplanets in 2022 using theTransiting Exoplanet Survey Satellite(TESS), all orbiting closer to their star thanMercuryis to the Sun.[3]All of them are Neptune-sized ormini-Neptunes,and their masses have been measured using a combination ofradial velocityandtransit-timing variations,showing them to have low densities.[5]The planets are in anorbital 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 −0.7M🜨 |
0.05106±0.0009 | 4.1727±0.0003 | 0.027±0.009 | 86.44+0.27 −0.21° |
1.90+0.21 −0.15R🜨 |
| c | 6.32+1.1 −1.3M🜨 |
0.0669±0.0005 | 6.2574±0.0002 | 0.11±0.01 | 89.42+0.39 −0.55° |
2.879+0.060 −0.062R🜨 |
| d | 8.35+1.8 −1.6M🜨 |
0.1062±0.0008 | 12.5199±0.0004 | 0.042±0.004 | 89.41±0.28° | 4.627+0.077 −0.072R🜨 |
| e | 6.07+1.09 −1.01M🜨 |
0.139±0.002 | 18.801±0.001 | 0.0425±0.004 | 89.31+0.26 −0.18° |
2.639+0.072 −0.088R🜨 |
| f | 9.7+3.9 −3.7M🜨 |
0.174±0.002 | 26.321±0.001 | 0.001±0.001 | 89.38+0.22 −0.17° |
3.88±0.11R🜨 |
| g | 5.6+4.1 −3.2M🜨 |
0.229±0.003 | 39.545±0.002 | 0.04±0.01 | 89.65+0.18 −0.13° |
2.53+0.11 −0.12R🜨 |
| h(unconfirmed) | <18.8M🜨 | ~0.36 | ~77 | 0.04+0.05 −0.03 |
89.68±0.02° | 2.68+0.20 −0.18R🜨 |
See also
[edit]References
[edit]- ^"Finding the constellation which contains given sky coordinates".djm.cc.2 August 2008.Archivedfrom the original on 15 August 2019.Retrieved11 December2023.
- ^abcdefVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData 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.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
- ^abcdefgDai, 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.
- ^abcdef"TOI-1136".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved10 December2023.
- ^abcdBeard, 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.
