Model-Independent Stellar and Planetary Masses from Multi-Transiting Exoplanetary Systems

Abstract

Precise exoplanet characterization requires precise classification of exoplanet host stars. The masses of host stars are commonly estimated by comparing their spectra to those predicted by stellar evolution models. However, spectroscopically determined properties are difficult to measure accurately for stars that are substantially different from the Sun, such as M-dwarfs and evolved stars. Here, we propose a new method to dynamically measure the masses of transiting planets near mean-motion resonances and their host stars by combining observations of transit timing variations with radial velocity measurements. We derive expressions to analytically determine the mass of each member of the system and demonstrate the technique on the Kepler-18 system. We compare these analytic results to numerical simulations and find the two are consistent. We identify eight systems for which our technique could be applied if follow-up radial velocity measurements are collected. We conclude this analysis would be optimal for systems discovered by next generation missions similar to TESS or PLATO, which will target bright stars that are amenable to efficient RV follow-up.

9 pages, 1 figure, submitted to ApJ

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Cited by in corpus (4)

• Transit timing to first order in eccentricity
• The SDSS-III APOGEE Radial Velocity Survey of M dwarfs I: Description of Survey and Science Goals
• Absolute masses and radii determination in multiplanetary systems without stellar models
• Observations of the Kepler Field with TESS: Predictions for Planet Yield and Observable Features