Eccentric warm Jupiters TOI-2147 b and TOI-6019 b characterized by researchers

Star system: TOI 6019 | Distance from the Sun: 862 light years

Warm Jupiters are gas giant planets with orbital periods between 10 and 200 days. Two such planets, TOI-2147 b and TOI-6019 b, have been identified and characterized. These planets exhibit high orbital eccentricity, meaning their paths around their host stars are more oval-shaped than circular. Their characteristics suggest they migrated to their current positions through processes involving high-eccentricity interactions.

The planetary nature of these candidates was confirmed by combining data from the Transiting Exoplanet Survey Satellite with ground-based observations. This included high-precision radial velocity measurements, which track the tiny wobbles of stars caused by the gravitational pull of orbiting planets, as well as imaging to confirm the planetary signatures.

TOI-2147 b orbits a G-type star every 26.2 days, while TOI-6019 b orbits a G-type sub-giant star every 14.5 days. Both planets have densities lower than Jupiter, indicating their atmospheres are somewhat puffed up. Models suggest that tidal heating—internal heat generated by gravitational stretching as the planets move along their eccentric orbits—likely causes this radius inflation.

Key findings
- TOI-2147 b orbits its host star every 26.2 days with a high orbital eccentricity.
- TOI-6019 b completes an orbit in 14.5 days around a sub-giant star with significant eccentricity.
- Both planets exhibit inflated radii likely caused by tidal heating from their non-circular orbits.
- No evidence for additional planets in these systems was found during the observations.

Scientific study

TOI-2147 b and TOI-6019 b: Two eccentric warm Jupiters detected and characterized with TESS and MaHPS (external link)