Data for "The Impact of Irradiation on the Radius and Thermal Evolution of Transiting Brown Dwarfs"

Overview These are the evolutionary models for irradiated (transiting) brown dwarfs presented in Mukherjee et al. 2026. The grid explores how the structure and evolution of brown dwarfs are altered by the incident stellar radiation they receive, the presence of a core, and an additional anomalous interior-heating term. The models are computed by coupling a interior structure and cooling model to irradiated cloud-free radiative-convective thermochemical equilibrium model atmospheres calculated with the open-source code PICASO. The parameters spanned by this grid are the incident stellar flux (log(F)), the heavy-element core mass (Mcore), and the anomalous heating efficiency (epsilon). The grid includes evolution tracks for object masses between ~10 to ~84 Jupiter masses. The ranges and increments of these parameters are described in the published paper. Model parameters Each evolutionary track corresponds to a unique combination of: log(F), i.e., log incident stellar flux in erg/s/cm^2 (6, 7, 8, 9, 9.5, 10); Mcore, i.e., core mass in Earth masses (0, 50, 100, 200, 300); epsilon, i.e., anomalous heating efficiency as a fraction of incident flux (0.0, 0.005, 0.01, 0.015, 0.02 fractions). The three parameter values are also written at the top of each file header. Columns M/Mjup, age(Gyr), logL/Lsun (intrinsic), logLnuc/Lsun (nuclear), logLtot/Lsun (total emitted, incl. reradiated stellar heat), Tint(K), logg_cgs, R/Rjup, Tc(K), Pc(bar).