Measuring the Stellar and Planetary Properties of the 51 Eridani System

In order to study exoplanets, a comprehensive characterization of the fundamental properties of the host stars, such as angular diameter, temperature, luminosity, and age, is essential, as the formation and evolution of exoplanets are directly influenced by the host stars at various points in time. In this paper, we present interferometric observations taken of directly imaged planet host 51 Eridani at the CHARA Array. We measure the limb-darkened angular diameter of HD 29391 to be $\theta_{\rm LD} = 0.450\pm 0.004 \rm ~mas$ and combining with the Gaia zero-point corrected parallax, we get a stellar radius of $1.45 \pm 0.01 \rm~R_{\odot}$. We use the PARSEC isochrones to estimate an age of $23.2^{+1.7}_{-1.6} \rm ~Myr$ and a mass of $1.550 \pm 0.005 \rm ~M_{\odot}$. The age and mass agree well with values in the literature, determined through a variety of methods ranging from dynamical age trace-backs to lithium depletion boundary methods. We derive a mass of $4.1^{+0.5}_{-0.4} \rm ~M_{Jup}$ for 51 Eri b using the Sonora Bobcat models, which further supports the possibility of 51 Eri b forming under either the hot-start formation model or the warm-start formation model.