Draft:HD 332231
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Submission declined on 31 January 2026 by Stuartyeates (talk). These are primary sources.
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Comment: Possibly AI-gen? I've never heard the phrase "literature solutions", sounds like a possible tortured phrase to me. Shocksingularity (talk) 06:06, 20 September 2026 (UTC)
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| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 20h 26m 57.92s[1] |
| Declination | +33° 44′ 40.02″[1] |
| Apparent magnitude (V) | 8.558 ± 0.002[2] |
| Characteristics | |
| Evolutionary stage | Main sequence[1] |
| Spectral type | F8V[3] |
| Astrometry | |
| Proper motion (μ) | RA: -36.8687 mas/yr[2] Dec.: -14.6514 mas/yr[2] |
| Parallax (π) | 12.3678±0.0292 mas[2] |
| Distance | 263.7 ± 0.6 ly (80.9 ± 0.2 pc) |
| Details | |
| Mass | 1.127 ± 0.077[3] M☉ |
| Radius | 1.277+0.039 −0.036[3] R☉ |
| Surface gravity (log g) | 4.279+0.027 −0.034[3] cgs |
| Temperature | 6089+97 −96[3] K |
| Metallicity [Fe/H] | 0.036+0.059 −0.058[3] dex |
| Age | 4.3+2.5 −1.9[3] Gyr |
| Other designations | |
| TOI-1456, TIC 199376584, TYC 2689-70-1, 2MASS J20265791+3344401, Gaia DR3 2056007995732413312[1] | |
| Database references | |
| SIMBAD | data |
HD 332231 is an F-type main-sequence star in the constellation Cygnus, about 80.7 parsecs (263 light-years) from the Solar System.[1] [2] It hosts the confirmed transiting exoplanet HD 332231 b, also known as TOI-1456 b, which has an orbital period of about 18.7 days.[4][2]
Planetary system
[edit]Discovery and properties
[edit]HD 332231 b was discovered using observations from the Transiting Exoplanet Survey Satellite (TESS). TESS observed the star during Sectors 14 and 15 of its primary mission, with a transit detected in Sector 15.[5] Radial-velocity observations subsequently confirmed that the transit was caused by a planet.[5] The discovery was announced in 2020, and NASA classifies HD 332231 b as a gas-giant exoplanet.[4]
Dalba and collaborators described the planet as a warm sub-Saturn and derived a mass of 0.244 ± 0.021 Jupiter masses and a radius of approximately 0.87 Jupiter radii.[5] They estimated its equilibrium temperature to be 876 ± 17 K.[5][2] The NASA Exoplanet Archive contains several different solutions for the physical and orbital parameters of the system from the different studies of this planetary system.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| b | 0.244 ± 0.021 MJ | 0.1436+0.0032 −0.0033 |
18.71204 ± 0.00043 | 0.032+0.030 −0.022 |
89.68+0.22 −0.28 |
0.867+0.027 −0.025 RJ |
Orbital alignment
[edit]The orientation of the orbit of HD 332231 b relative to the rotation of its host star has been investigated using the Rossiter–McLaughlin effect. Two observing campaigns initially produced different estimates of the planet's sky-projected orbital obliquity, usually denoted λ.
Sedaghati and collaborators observed a transit with the CARMENES spectrograph and measured λ = −42.0+11.3
−10.6°, which they interpreted as a moderately misaligned orbit.[6] Knudstrup and Albrecht independently observed the system with HARPS-N and obtained λ = −2 ± 6°, consistent with an aligned orbit.[3] The curated TEPCat orbital-obliquity catalogue lists both published determinations.[7]
HD 332231 was also included in the sample compiled for a 2022 review of stellar obliquities in exoplanetary systems by Albrecht, Dawson and Winn. The review incorporated the Knudstrup and Albrecht measurement into its vetted compilation of projected-obliquity measurements.[8]
The discrepancy between the original Rossiter–McLaughlin measurements was revisited by Maciejewski in 2026 as part of an analysis that accounted for the system's transit-timing variations. Reanalysis of both the HARPS-N and CARMENES observations yielded projected obliquities consistent with 0°, supporting an aligned-orbit interpretation.[9] Maciejewski noted that the inferred obliquity can be affected by the adopted transit ephemeris and by systematic trends in the radial-velocity observations.[9]
Transit-timing variations
[edit]Knudstrup and Albrecht found that the observed transit times did not follow a simple linear ephemeris and reported a timing offset of approximately 20 minutes in their analysis. They suggested gravitational perturbations from an additional body as one possible explanation.[3]
A longer time baseline was analysed by Maciejewski in 2026 using TESS photometry together with ground-based transit observations. The analysis identified a coherent transit-timing variation (TTV) signal with a period of approximately 6.7 years and an amplitude of about 45 minutes.[9] Numerical simulations showed that numerous orbital configurations for an additional planet could reproduce the observed timing variations. Models containing an exterior planet with an orbital period longer than about 60 days produced a modest improvement in likelihood when the available photometric and radial-velocity constraints were considered.[9]
The proposed additional planet has not been independently confirmed, and the 2026 analysis did not determine a unique mass or orbit for the possible perturber. Continued transit-timing and radial-velocity observations were identified as necessary to determine the origin of the variations.[9] TEPCat subsequently adopted a revised orbital period of approximately 18.71254 days based on the 2026 ephemeris.[10]
See also
[edit]References
[edit]- 1 2 3 4 5 "HD 332231". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 September 2026.
- 1 2 3 4 5 6 7 8 "HD 332231 Overview". NASA Exoplanet Archive. California Institute of Technology. Retrieved 17 September 2026.
- 1 2 3 4 5 6 7 8 9 Knudstrup, Emil; Albrecht, Simon H. (2022). "Orbital alignment of HD 332231 b: The warm Saturn HD 332231 b/TOI-1456 b travels on a well-aligned, circular orbit around a bright F8 dwarf". Astronomy & Astrophysics. 660: A99. arXiv:2111.14968. Bibcode:2022A&A...660A..99K. doi:10.1051/0004-6361/202142726.
- 1 2 "HD 332231 b". NASA Science. National Aeronautics and Space Administration. Retrieved 17 September 2026.
- 1 2 3 4 5 Dalba, Paul A.; et al. (2020). "The TESS–Keck Survey. I. A Warm Sub-Saturn-mass Planet and a Caution about Stray Light in TESS Cameras". The Astronomical Journal. 159 (5): 241. arXiv:2003.10451. Bibcode:2020AJ....159..241D. doi:10.3847/1538-3881/ab84e3.
- ↑ Sedaghati, Ehsan; et al. (2022). "A moderately misaligned orbit of the warm sub-Saturn HD 332231 b". Astronomy & Astrophysics. 659: A44. arXiv:2110.10282. Bibcode:2022A&A...659A..44S. doi:10.1051/0004-6361/202142471.
- ↑ "TEPCat: Orbital obliquity observations for transiting planetary systems". TEPCat. Keele University. Retrieved 17 September 2026.
- ↑ Albrecht, Simon H.; Dawson, Rebekah I.; Winn, Joshua N. (2022). "Stellar Obliquities in Exoplanetary Systems". Publications of the Astronomical Society of the Pacific. 134 (1038): 082001. arXiv:2203.05460. doi:10.1088/1538-3873/ac6c09.
- 1 2 3 4 5 Maciejewski, Gracjan (2026). "Detection of periodic transit timing variations in the warm sub-Saturn planet HD 332231 b". Astronomy & Astrophysics. 708: A285. arXiv:2603.10497. Bibcode:2026A&A...708A.285M. doi:10.1051/0004-6361/202557788.
- ↑ "TEPCat: Basic observable properties of transiting planets". TEPCat. Keele University. Retrieved 17 September 2026.
External links
[edit]- NASA Exoplanet Archive: HD 332231
- HD 332231 b at NASA Science
- HD 332231 at SIMBAD