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Measuring the stellar and planetary parameters of the 51 Eridani system

Published online by Cambridge University Press:  18 September 2024

Ashley Elliott Open the ORCID record for Ashley Elliott [Opens in a new window] ,
Tabetha Boyajian Open the ORCID record for Tabetha Boyajian [Opens in a new window] ,
Tyler Ellis ,
Kaspar von Braun ,
Andrew W. Mann  and
Gail Schaefer
Ashley Elliott*
Affiliation:
Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA, USA
Tabetha Boyajian
Affiliation:
Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA, USA
Tyler Ellis
Affiliation:
Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA, USA
Kaspar von Braun
Affiliation:
Lowell Observatory, Flagstaff, AZ, USA
Andrew W. Mann
Affiliation:
Department of Physics and Astronomy, The University of North Carolina at Chapel Hill, Chapel Hill, NC, USA
Gail Schaefer
Affiliation:
The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, CA, USA
*
Corresponding author: Ashley Elliott; Email: aelli76@lsu.edu
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Abstract

In order to study exoplanets, a comprehensive characterisation 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 51 Eridani to be $\theta_\mathrm{LD} = 0.450\pm 0.006$ mas and combining with the Gaia zero-point corrected parallax, we get a stellar radius of $1.45 \pm 0.02$ R$_{\odot}$. We use the PARSEC isochrones to estimate an age of $23.2^{+1.7}_{-2.0}$ Myr and a mass of $1.550^{+0.006}_{-0.005}$ 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 $4.1\pm0.4$ M$_\mathrm{Jup}$ 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.

Keywords

Exoplanetsinterferometryfundamental propertiesyoung stars
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 41 , 2024 , e043
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of Astronomical Society of Australia

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