TOI-1227 b
| Discovery[1] | |
|---|---|
| Discovered by | Mann et al. (THYME) |
| Discovery date | 2022 |
| Transit method | |
| Orbital characteristics | |
| 0.0886+0.0054 −0.0057 AU | |
| Inclination | 88.571+0.062 −0.093 ° |
| Star | TOI-1227 (Gaia DR2 5842480953772012928) |
| Physical characteristics | |
| 0.854+0.067 −0.052 RJ | |
TOI-1227 b is one of the youngest transiting exoplanets discovered (as of September 2022), alongside K2-33b and HIP 67522 b. The exoplanet TOI-1227 b is about 11±2 million years old[a] and currently 9.6 R🜨 large. It will become a 3-5 R🜨 planet in about 1 billion years, because the planet is still contracting. TOI-1227 b orbits its host star every 27.36 days.[1]
Characteristics
[edit ]TOI-1227 b has a size that is 85% that of Jupiter, or 9.6 times that of Earth. No other Jupiter-sized planet was detected around mid- to late M-dwarfs, despite the deep transits such a planet would create. The researchers find that the planet is still hot from its formation and this heat, combined with a hydrogen-dominated primary atmosphere makes the atmosphere of TOI-1227 b inflated. Evolutionary models suggest that TOI-1227 b will eventually evolve into a sub-Neptune within the next billion years.[1]
Future research
[edit ]Radial velocity follow-up to determine the mass of TOI-1227 b is not possible in the optical, but might be possible in the near-infrared. A less challenging follow-up would be the measurement of the Spin-Orbit-Alignment via the Rossiter–McLaughlin effect.[1]
Host star
[edit ]| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Musca [note 1] |
| Right ascension | 12h 27m 4.31s[2] |
| Declination | −72° 27′ 6.5″[2] |
| Apparent magnitude (V) | 17±1.133[3] |
| Characteristics | |
| Evolutionary stage | Pre-main sequence star [1] |
| Spectral type | M4.5V-M5V[1] |
| Astrometry | |
| Radial velocity (Rv) | 13.3±0.3[1] km/s |
| Proper motion (μ) | RA: −40.2658±0.0972 mas/yr [3] Dec.: −10.6417±0.0807 mas/yr [3] |
| Parallax (π) | 9.9079±0.0558 mas [3] |
| Distance | 328.089+1.87 −1.845 ly (100.641+0.573 −0.566 pc)[3] |
| Absolute magnitude (MV) | 11.986[b] |
| Details[1] | |
| Mass | 0.17±0.015 M☉ |
| Radius | 0.56±0.03 R☉ |
| Luminosity | 0.0251 L☉ |
| Surface gravity (log g) | 4.7893±0.0058[3] cgs |
| Temperature | 3072±74 K |
| Rotation | 1.65±0.04 d |
| Rotational velocity (v sin i) | 16.65±0.24 km/s |
| Age | 11±2 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
TOI-1227 was first identified as a pre-main-sequence star (PMS star) with the Gaia satellite.[4] [5] [6] Without this prior identification as a PMS star the exoplanet signal of TOI-1227 b would have been disregarded as an eclipsing binary due to the V-shape of the transit signal.[1]
The star is located north of the globular cluster NGC 4372, but it is much closer to earth than this cluster of stars, at a distance of about 101 parsecs (330 light-years).[1] NGC 4372 is 5,800 parsecs (19,000 ly) away.[7]
The host star TOI-1227 is part of a subgroup of the Lower Centaurus Crux OB association, sometimes called B,[6] A0[4] and called Musca group by the scientists that discovered TOI-1227 b. This group was called Musca after the constellation Musca in which most of its members are located.[1]
TOI-1227 has a spectral type of M4.5V to M5V, a mass 17% of the Sun and a radius 56% of the Sun. The host star is relative faint for a TOI with a visual magnitude of about 17.[1] The right ascension of 12h 27m 4.31s and the declination −72° 27′ 6.5″ implies that it is located in the Musca constellation.[2] [c] The host star shows Lithium in its atmosphere, which should be depleted within 10-200 million years for M-dwarfs.[1]
References
[edit ]- ^ a b c d e f g h i j k l m Mann, Andrew W.; Wood, Mackenna L.; Schmidt, Stephen P.; Barber, Madyson G.; Owen, James E.; Tofflemire, Benjamin M.; Newton, Elisabeth R.; Mamajek, Eric E.; Bush, Jonathan L.; Mace, Gregory N.; Kraus, Adam L.; Thao, Pa Chia; Vanderburg, Andrew; Llama, Joe; Johns-Krull, Christopher M. (2022年04月01日). "TESS Hunt for Young and Maturing Exoplanets (THYME). VI. An 11 Myr Giant Planet Transiting a Very-low-mass Star in Lower Centaurus Crux". The Astronomical Journal. 163 (4): 156. arXiv:2110.09531 . Bibcode:2022AJ....163..156M. doi:10.3847/1538-3881/ac511d . ISSN 0004-6256. S2CID 239024522.
- ^ a b c d e "TOI-1227". simbad.cds.unistra.fr. Retrieved 2024年02月14日.
- ^ a b c d e f "TOI-1227 | NASA Exoplanet Archive". exoplanetarchive.ipac.caltech.edu. Retrieved 2024年02月14日.
- ^ a b Goldman, Bertrand; Röser, Siegfried; Schilbach, Elena; Moór, Attila C.; Henning, Thomas (2018年11月01日). "A Large Moving Group within the Lower Centaurus Crux Association". The Astrophysical Journal. 868 (1): 32. arXiv:1807.02076 . Bibcode:2018ApJ...868...32G. doi:10.3847/1538-4357/aae64c . ISSN 0004-637X. S2CID 119343278.
- ^ Zari, E.; Hashemi, H.; Brown, A. G. A.; Jardine, K.; de Zeeuw, P. T. (2018年12月01日). "3D mapping of young stars in the solar neighbourhood with Gaia DR2". Astronomy and Astrophysics. 620: A172. arXiv:1810.09819 . Bibcode:2018A&A...620A.172Z. doi:10.1051/0004-6361/201834150. ISSN 0004-6361. S2CID 119078481.
- ^ a b Kerr, Ronan M. P.; Rizzuto, Aaron C.; Kraus, Adam L.; Offner, Stella S. R. (2021年08月01日). "Stars with Photometrically Young Gaia Luminosities Around the Solar System (SPYGLASS). I. Mapping Young Stellar Structures and Their Star Formation Histories". The Astrophysical Journal. 917 (1): 23. arXiv:2105.09338 . Bibcode:2021ApJ...917...23K. doi:10.3847/1538-4357/ac0251 . ISSN 0004-637X. S2CID 234790391.
- ^ Boyles, Jason; Lorimer, Duncan R.; Turk, Phil J.; Mnatsakanov, Robert; Lynch, Ryan S.; Ransom, Scott M.; Freire, Paulo C.; Belczynski, Khris (2011年11月20日). "Young Radio Pulsars in Galactic Globular Clusters". The Astrophysical Journal. 742 (1): 51. arXiv:1108.4402 . doi:10.1088/0004-637X/742/1/51. ISSN 0004-637X.
- ^ For comparison, the Solar System is about 4.6 billion years old.
- ^ Calculated using an apparent magnitude of 17 and a distance of 100.641 parsecs [3] in the equation Mapp = Mabs - 5 + 5 * log(distance (parsecs))
- ^ The constellation can be obtained by the right ascension and declination in this website.