A radiative-convective equilibrium model for young giant exoplanets

A radiative-convective equilibrium model for young
giant exoplanets: Applications to beta pictoris b
data.
Jean-Loup Baudino∗†1 , Bruno Bézard1 , Anthony Boccaletti1 , Mickaël Bonnefoy2 , and
Anne-Marie Lagrange2
1
Laboratoire d’études spatiales et d’instrumentation en astrophysique (LESIA) – Université Pierre et
Marie Curie [UPMC] - Paris VI, Observatoire de Paris, INSU, CNRS : UMR8109, Université Paris VII Paris Diderot, Université Pierre et Marie Curie (UPMC) - Paris VI – 5, place Jules Janssen 92190
MEUDON, France
2
Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) – OSUG, Université Joseph Fourier Grenoble I, INSU, CNRS : UMR5274 – 414, Rue de la Piscine BP 53 38041 Grenoble Cedex 9, France
Abstract
We developed a radiative-convective equilibrium model for young giant exoplanets, in the
context of direct imaging. Input parameters are the planet’s surface gravity (g), effective
temperature (Teff)
and elemental composition. Under the additional assumption of thermochemical equilibrium, the model predicts the equilibrium temperature profile and mixing ratio profiles of the
most important
gases. Opacity sources include the H2-He collision-induced absorption and molecular lines
from H2O, CO, CH4, NH3, VO, TiO, Na and K. Line opacity is modeled using k-correlated
coefficients precalculated over a fixed pressure-temperature grid. Absorption by iron and silicate cloud
particles is added above the expected condensation levels with a fixed scale height and a
given optical depth at
some reference wavelength. Model predictions are compared with the existing photometric and spectroscopic measurements of Beta Pictoris b.
∗
†
Speaker
Corresponding author: [email protected]
sciencesconf.org:betapic30:41919