Computational modeling study reveals tighter true mass limits for radial-velocity exoplanets, indicating dynamical stability strongly constrains orbital inclination in compact systems.
Key Points
Constrain the inclinations and true masses of non-transiting radial-velocity exoplanets in compact multi-planet systems by leveraging requirements of dynamical orbital stability.
Developed CINEMAS, a Bayesian statistical framework incorporating dynamical stability constraints to break the mass-inclination degeneracy in flat multi-planet architectures.
Applied the stability-based Bayesian framework to five compact multi-planet systems, including Barnard’s Star and HD 184010.
Reduced upper limits on the true masses of planets across five compact systems by as much as 45%.
Constrained the true masses of all four Barnard’s Star exoplanets to below 0.6 Earth masses with at least 95% confidence.
Determined that the three gas giants orbiting HD 184010 have true masses intermediate between Saturn and Jupiter.