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 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, assuming both stars are at the same distance.Gaia DR3, as accessed through VizieR or the Gaia Archive, shows significantly different parallaxes for the two stars, suggesting they are at different distances and the system is an optical double.
However, a 2025 paper by Conzo et al. published in Research Notes of the AAS claims a different parallax for star B, attributed to Gaia DR3, that is similar to that of star A. 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.
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 and later confirmed by ground-based photometric observations. 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.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.