Cannabaceae

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TOI-1227 b
Discovery[1]
Discovered byMann et al. (THYME)
Discovery date2022
Transit method
Orbital characteristics
0.0886+0.0054
−0.0057 AU
Inclination88.571+0.062
−0.093 °
StarTOI-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

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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

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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

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TOI-1227
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]
Distance328.089+1.87
−1.845 ly
(100.641+0.573
−0.566 pc)[3]
Absolute magnitude (MV)11.986[b]
Details[1]
Mass0.17±0.015 M☉
Radius0.56±0.03 R☉
Luminosity0.0251 L☉
Surface gravity (log g)4.7893±0.0058[3] cgs
Temperature3072±74 K
Rotation1.65±0.04 d
Rotational velocity (v sin i)16.65±0.24 km/s
Age11±2 Myr
Other designations
2MASS J12270432-7227064, Gaia DR2, 5842480953772012928, Gaia DR3 5842480953772012928, TIC 360156606, TOI-1227, UCAC4 088-032065, WISE J122704.24-722706.5, WISEA J122704.22-722706.5[2]

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

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  1. ^ 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. (2022-04-01). "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.
  2. ^ a b c d e "TOI-1227". simbad.cds.unistra.fr. Retrieved 2024-02-14.
  3. ^ a b c d e f "TOI-1227 | NASA Exoplanet Archive". exoplanetarchive.ipac.caltech.edu. Retrieved 2024-02-14.
  4. ^ a b Goldman, Bertrand; Röser, Siegfried; Schilbach, Elena; Moór, Attila C.; Henning, Thomas (2018-11-01). "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.
  5. ^ Zari, E.; Hashemi, H.; Brown, A. G. A.; Jardine, K.; de Zeeuw, P. T. (2018-12-01). "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.
  6. ^ a b Kerr, Ronan M. P.; Rizzuto, Aaron C.; Kraus, Adam L.; Offner, Stella S. R. (2021-08-01). "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.
  7. ^ Boyles, Jason; Lorimer, Duncan R.; Turk, Phil J.; Mnatsakanov, Robert; Lynch, Ryan S.; Ransom, Scott M.; Freire, Paulo C.; Belczynski, Khris (2011-11-20). "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.
  1. ^ For comparison, the Solar System is about 4.6 billion years old.
  2. ^ 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))
  3. ^ The constellation can be obtained by the right ascension and declination in this website.
  1. ^ Obtained with a right ascension of 12h 27m 4.31s and a declination of −72° 27′ 6.5″[2] on this website.
source: https://en.wikipedia.org/wiki/TOI_1227_b

One thought on “Cannabaceae”

  1. Well, that’s interesting to know that Psilotum nudum are known as whisk ferns. Psilotum nudum is the commoner species of the two. While the P. flaccidum is a rare species and is found in the tropical islands. Both the species are usually epiphytic in habit and grow upon tree ferns. These species may also be terrestrial and grow in humus or in the crevices of the rocks.
    View the detailed Guide of Psilotum nudum: Detailed Study Of Psilotum Nudum (Whisk Fern), Classification, Anatomy, Reproduction

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