TOI-1227 b

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Coordinates: Sky map 12h 27m 04.31s, −72° 27′ 06.49″
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TOI-1227 b
Discovery
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

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

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

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]
Distance
328.089+1.87
−1.845 ly
(100.641+0.573
−0.566 pc)[3]
Absolute magnitude (MV)11.986[b]
Details
Myr
UCAC4 088-032065, WISE J122704.24-722706.5, WISEA J122704.22-722706.5[2]
Database references
SIMBADdata

TOI-1227 was first identified as a

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

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

  1. ^
    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. ^
    S2CID 119343278
    .
  5. S2CID 119078481
    .
  6. ^
    S2CID 234790391
    .
  7. 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.
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