Astronomy:TOI-6883
TOI-6883 is a wide double or binary star located in the constellation of Delphinus. It is composed of two Sun-like stars, TOI-6883A and TOI-6883B. The primary star is at a distance of approximately 94 parsecs (307 light-years) from Earth.
Characteristics
Both stars are classified as G-type main-sequence stars with masses and radii similar to that of the Sun. They are separated by approximately 6.5 arcseconds, corresponding to a projected separation of ~616 astronomical units (AU), assuming both stars are at the same distance.[1]
Gaia DR3, as accessed through VizieR or the Gaia Archive, shows significantly different parallaxes for the two stars, suggesting they are at different distances (about 30 light-years apart) and the system is an optical double.[2][3]
However, a 2025 paper by Conzo et al. published in Research Notes of the AAS (which is not peer-reviewed) claims a different parallax for star B, attributed to Gaia DR3, that is similar to that of star A (~10.6 mas). The paper argues that this, along with consistent proper motions, supports the idea that the two stars form a gravitationally-bound and dynamically stable binary system, with an orbital period of ~15,300 years.[1]
Planetary system
The TOI-6883 system has at least one planet: TOI-6883Ab is a hot Jupiter-type exoplanet orbiting the primary star TOI-6883A with a period of about 16.25 days. The planet was first detected via transit by the Transiting Exoplanet Survey Satellite (TESS) and later confirmed by ground-based photometric observations.[4] Based on their claim of the binary nature of the host star, Conzo et al. updated the planet's designation from TOI-6883b to TOI-6883Ab in accordance with IAU naming conventions for multiple stellar systems.[1]
With a radius of ~1.1 Jupiter radii, the planet produces a transit depth of about 1.3%. The presence of the secondary star TOI-6883B may influence the planet’s long-term orbital evolution via dynamical mechanisms such as Kozai–Lidov oscillations.[1]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 4.34±0.15 MJ | 0.1291+0.0021 −0.0022 |
16.24921+0.00010 −0.00011 |
0.6058±0.0023 | 89.57+0.30 −0.38° |
1.087+0.023 −0.021 RJ |
References
- ↑ 1.0 1.1 1.2 1.3 Conzo, G.; Campos, F.; Conti, F.; Sharp, I. (June 2025). "Characterization of the Visual Binary TOI-6883AB and its Dynamical Implications for the Planetary Companion TOI-6883Ab". Research Notes of the AAS 9 (6): 139. doi:10.3847/2515-5172/ade25d. Bibcode: 2025RNAAS...9..139C.
- ↑ Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 4.0 4.1 Sgro, Lauren A. et al. (July 2024). "Confirmation and Characterization of the Eccentric, Warm Jupiter TIC 393818343 b with a Network of Citizen Scientists". The Astronomical Journal 168 (1): 26. doi:10.3847/1538-3881/ad5096. Bibcode: 2024AJ....168...26S.
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