adsabs/AstroCLIMB huggingface dataset:
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: Evolution during boil-off for two 3.6 M ⊕ models both starting at the same entropy, which gives an initial Kelvin–Helmholtz timescale of a few megayears, but with different initial H/He envelope mass fractions (30% in black and 10% in gray). In 102 yr, the 30% model experiences a significant entropy drop owing to its fast advective cooling rate, while the entropy for the 10% model remains unchanged (bottom left). As a result, the 30% model has a cooler interior by 106 yr, ending boil-off with a slightly larger final mass fraction (top right). After ∼102 yr, the mass-loss rate (top left), RCB radius (middle left), intrinsic (radiative) luminosity (middle right, dashed line), and advective luminosity (middle right, solid line) for the two models converge, essentially meaning that the advective luminosity has a negligible impact on the later evolution. For both mass fractions, after ∼106 yr, the radiative cooling timescale (bottom right, solid line) becomes shorter than the mass-loss timescale (bottom right, dashed line), and the outflow transitions into the long-lived mass-loss phase.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show the final mass fraction as a function of core mass and stellar bolometric flux (color-coded) after boil-off (triangles) and after 3 Gyr (crosses) evolution of the post-boil-off Parker wind (bolometric driven), with the model setups similar to those in Figure 10. Note that the post-boil-off mass fractions are calculated using a 10% default initial mass fraction, while the final mass fractions after 3 Gyr of evolution under the long-lived wind employ the same scaling function ﹩f=0.05{({M}_{c}/{M}_{\oplus })}^{1/2}﹩ developed in GSS18 as an initial condition (the initial mass fraction is shown by the dotted line). The long-lived Parker wind is inefficient, only being able to remove the last few × 10−4 of envelope mass after boil-off.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: To examine how different initial conditions impact the evolution of low-mass sub-Neptunes, we show the evolution tracks of two planets with low mass (3 M ⊕; left panels) and intermediate mass (5 M ⊕; right panels) receiving 100 F ⊕ stellar radiation. We show three tracks, with the only difference being how we initialize the evolution. All curves already have the relevant physics improved (i.e., a decoupled isothermal Parker wind with the mass-loss-driven energy-loss term ﹩{\dot{E}}_{\mathrm{adv}}﹩ included). The black curve shows the evolution from the fully analytical GSS18 approach, but now including a boil-off phase. The gray curve represents the evolution from the semianalytical approach with the initial conditions calculated self-consistently from our numerical boil-off model (with the evolution before 1 Myr shown by the dashed line). See Sections 4.6.2 and 4.6.3 for discussion.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We compare two models (both with 3.6 M ⊕ and 10 F ⊕) with (black) and without core luminosity (gray), both incorporating advective cooling and starting at the same initial entropy and initial mass fractions (top right). The core heat capacity keeps the planet warm and slightly more inflated (top left) compared to the model without core luminosity, leading to a slightly enhanced mass loss. The core-enhanced mass loss only happens after the transition phase (black dotted line) starts (Equation (29)), when the mass loss (black dashed line in the bottom-left panel) becomes coupled with the core-luminosity-dominated thermal evolution (dotted red line). Note that, before the transition phase, the core luminosity (dotted red line) also constitutes the majority of the interior cooling (dashed and solid black line in the bottom-right panel), but the mass loss is not core enhanced owing to the decoupling effect.