TOI-6883

TOI-6883

Observation data Epoch J2000.0        Equinox J2000.0
Constellation	Delphinus [1]
A
Right ascension	20h 41m 10.067s [2]
Declination	+03° 38′ 19.25″ [2]
Apparent magnitude  (V)	9.48 [3]
B
Right ascension	20h 41m 10.300s [4]
Declination	+03° 38′ 24.88″ [4]
Apparent magnitude  (V)	11.20 [5]
Characteristics
A
Evolutionary stage	Main sequence [2]
Spectral type	G [6]
B
Evolutionary stage	Main sequence [6]
Spectral type	G [6]
Astrometry
A
Proper motion (μ)	RA: −56.677 mas/yr [2] Dec.: −89.096 mas/yr [2]
Parallax (π)	10.6121±0.0154  mas [2]
Distance	307.3 ± 0.4  ly (94.2 ± 0.1  pc)
B
Proper motion (μ)	RA: −53.136 mas/yr [4] Dec.: −101.579 mas/yr [4]
Parallax (π)	11.8192±0.1557  mas [4]
Distance	276 ± 4  ly (85 ± 1  pc)
Details
A
Mass	1.082+0.055 −0.056 [7]   M☉
Radius	1.086±0.020 [7]   R☉
Luminosity	1.168+0.065 −0.063 [7]   L☉
Surface gravity (log g)	4.402+0.013 −0.018 [7]   cgs
Temperature	5756+67 −66 [7]   K
Metallicity [Fe/H]	0.318±0.058 [7]   dex
Age	3.8+2.6 −2.1 [7]   Gyr
B
Mass	0.702 [8]   M☉
Radius	0.701 [8]   R☉
Luminosity	0.246 [8]   L☉
Surface gravity (log g)	4.60 [4]   cgs
Temperature	4,892 [8]   K
Other designations
BD+03 4397, TOI-6883
A: TIC 393818343
B: TIC 393818340 [6]
Database references
SIMBAD	A
	B
Exoplanet Archive	data

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. ^[6]

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] [4]}

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 published in Research Notes of the AAS (which is not peer-reviewed) claims a different parallax for star B, attributed to Gaia DR3, that is similar to that of star A (~10.6 mas).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. ^[6]

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. ^[7] 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. ^[6]

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. ^[6]

The TOI-6883A planetary system ^[7]

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. Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific . 99 (617): 695. Bibcode:1987PASP...99..695R. doi: 10.1086/132034 . Constellation record for this object at VizieR .
2. Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR .
3. Høg, E.; Fabricius, C.; et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics . 355: L27 –L30. Bibcode:2000A&A...355L..27H.
4. Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR .
5. Nascimbeni, V.; Piotto, G.; Ortolani, S.; Giuffrida, G.; Marrese, P. M.; Magrin, D.; Ragazzoni, R.; Pagano, I.; Rauer, H.; Cabrera, J.; Pollacco, D.; Heras, A. M.; Deleuil, M.; Gizon, L.; Granata, V. (2016). "An all-sky catalogue of solar-type dwarfs for exoplanetary transit surveys". Monthly Notices of the Royal Astronomical Society. 463 (4): 4210. arXiv: 1609.03037 . Bibcode:2016MNRAS.463.4210N. doi: 10.1093/mnras/stw2313 .
6. 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. arXiv: 2506.08798 . Bibcode:2025RNAAS...9..139C. doi: 10.3847/2515-5172/ade25d .
7. Sgro, Lauren A.; Dalba, Paul 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. arXiv: 2405.15021 . Bibcode:2024AJ....168...26S. doi: 10.3847/1538-3881/ad5096 .
8. Hardegree-Ullman, Kevin K.; Apai, Dániel; Bergsten, Galen J.; Pascucci, Ilaria; López-Morales, Mercedes (2023). "Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O₂ Levels in Nearby Transiting Habitable-zone Exoplanets". The Astronomical Journal. 165 (6): 267. arXiv: 2304.12490 . Bibcode:2023AJ....165..267H. doi: 10.3847/1538-3881/acd1ec .

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