adsabs/AstroCLIMB huggingface dataset:
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: Hab 2 results: time-mean surface temperature (K) in (a) ExoCAM, (b) LMD-G, (c) ROCKE-3D, and (d) the UM.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: Hab 2 results: vertical cross sections of the zonal mean zonal wind (m s−1). The gray dashed horizontal line marks the 250 hPa level shown in Figure 20.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: Hab 2 results: meridional-mean cross sections of (a)–(d) mass mixing ratio (MMR) of ice cloud particles (log[kg kg−1]), (e)–(h) MMR of liquid cloud particles (log[kg kg−1]), and (i)–(l) total cloud fraction (%).
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: The same as in Figure 11, but for Hab 2.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). II. Moist Cases—The Two Waterworlds
Authors: Denis E. Sergeev, Thomas J. Fauchez, Martin Turbet, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne
Figure caption: The same as in Figure 9, but for Hab 2.
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption: Time interval between impacts of a given energy for Didymos and Dimorphos, in years. The blue and yellow lines show the impact interval if Didymos and Dimorphos were impacted by only the NEO and MBA population, respectively. The green lines show the impact interval on Didymos and Dimorphos for a mixed-population model that considers the system’s current orbit that crosses the inner main belt. The vertical dotted line shows the DART impact energy (≈2 × 1010 J). The green band shows the energy required to induce shape changing on a cohesionless Dimorphos. The blue band shows the ﹩{Q}_{D}^{* }﹩ required to catastrophically disrupt a low-cohesion Dimorphos. The thickness of the band takes into account the uncertainty in the Q calculation and the mass of Dimorphos. The gray line shows the the ﹩{Q}_{D}^{* }﹩ required to catastrophically disrupt Didymos. The horizontal dotted magenta line shows the median dynamical NEA lifetime. Adapted from Richardson et al. (2022, this focus issue).
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption: Normalized ejected mass at speeds greater than v as a function of normalized ejection speed, v/U, for (a) impacts into targets with fixed f = 0.6 and varying Y 0 between 0 and 50 Pa and (b) impacts into cohesionless targets (Y 0 = 0) and varying f between 0.4 and 1.0. The slope of μ = 0.38 is plotted for comparison. The shaded area in panels (a) and (b) shows the power-law regime of the ejecta mass–velocity distribution (e.g., Housen & Holsapple 2011; Raducan et al. 2019). Panels (c) and (d) show the cumulative ejected momentum as a function of normalized vertical ejection velocity.
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption: Asteroid mass ejected and displaced on the target. (a) Total ejected mass at velocities above 5 cm s−1 (≈v esc), normalized by the projectile mass, m (left), and initial target mass, M  t , in % (right). (b) Total target mass below escape velocity that is displaced on the target, normalized by the initial target mass, M  t  (left), and projectile mass, m (right). The shaded area denotes the transition to the gravity-dominated cratering regime.
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption: Critical specific impact energies for catastrophic disruptions, ﹩{Q}_{D}^{* }﹩, and shape-changing collisions, Q reshape(20%), for cohesionless (Y 0 = 0 Pa) spherical and ellipsoidal targets. The DART specific impact energy is Q DART ≈ 3 ± 1 J kg−1, which is similar to the values of Q reshape(20%) in the spherical and ellipsoidal targets investigated.
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption: (Left) Offset vector between surface normal direction and ejecta velocity vector, ∣ ϵ ∣. Results from iSALE-3D simulations (Raducan et al. 2022a) are plotted for comparison. (Right) Schematic representation of the impact geometry in an oblique impact scenario, where ﹩{\bar{p}}_{e}﹩ is the ejecta momentum vector (at infinity), ﹩\hat{n}﹩ is the surface normal vector, θ is the impact angle, and α is the angle between the surface normal and the ejecta velocity vector, ﹩{\bar{v}}_{e}﹩. Adapted from Rivkin et al. (2021).
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption: (a) Normalized ejected mass at speeds greater than v as a function of normalized ejection speed, v/U, for three cohesionless (Y 0 = 0) target shapes: spheroid, oblate ellipsoid, and prolate ellipsoid. The slope of μ = 0.38 is plotted for comparison. (b) Cumulative ejected momentum as a function of normalized vertical ejection velocity.
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption: Asteroid target morphology after vertical (90°) and oblique (45°) impacts at T = 2 hr after the impact. Up to ≈20% of the target material is displaced, causing excavation of material from the asteroid interior, global deformation, and resurfacing. The color denotes the deformed (strain > 0.2) and displaced material. The white grid frame represents the initial geometry of the target. For better visualization of the impact effects, some of the targets have been rotated.
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption:  Momentum transfer efficiency, β, for different target cohesions, Y0 , and coefficients of internal friction, f. The shaded area denotes the transition to the gravity-dominated cratering regime at about 2 Pa.
Paper: Global-scale Reshaping and Resurfacing of Asteroids by Small-scale Impacts, with Applications to the DART and Hera Missions
Authors: Sabina D. Raducan, Martin Jutzi
Figure caption: Cumulative target mass that experiences a total strain, ϵ tot, larger than a specific value, normalized by the total target mass, after vertical (90°) and oblique (45°) impacts on spherical and elliptical cohesionless targets.
Paper: Limited Stability of Multicomponent Brines on the Surface of Mars
Authors: Vincent F. Chevrier, Alec B. Fitting, Edgard G. Rivera-Valentín
Figure caption: Deliquescence conditions at the Phoenix landing site. A. Minimum water activity (or relative humidity) as a function of temperature at which a liquid is stable (e.g., corresponding to the eutonic of the mixture) for model 1 (red), model 2 (purple) and model 3 (blue). Note that the results at 278 and 283 K for model 3 are not shown because the model did not converge at the lowest water activities (see Figure 1(C)), although they are likely identical to model 2.Because Model 1 has the lowest eutonic values, anything below these water activities is in the salt form (shaded red). Ice also limits the presence of liquid by forming at certain water activities represented by the black line. Any water activity above is frozen (shaded gray). Therefore, liquids are never stable below 200 K for models 2 and 3. We also plot the relative humidity vs. temperature data as measured by the Phoenix lander (gray dots). B. Same diagram as (A) but rescaled to the range of temperatures measured by the Phoenix TECP (∼188–245 K). The blue line represents a simplified version of Model 1 lowest water activity values. The blue shaded region is the stable liquid region. The colored dots represent various phases of water as determined or suggested by Stillman & Grimm (2011) based on the TECP electrical measurements: adsorbed water (red), Melted liquid (blue) and undefined between both (green).
Paper: Limited Stability of Multicomponent Brines on the Surface of Mars
Authors: Vincent F. Chevrier, Alec B. Fitting, Edgard G. Rivera-Valentín
Figure caption: Water activity for each precipitating mineral as a function of temperature during evaporation simulations of brine mixtures using Model 1 (A), Model 2 (B), and Model 3 (C) as described in Table S1. Each class of salt is represented by a color tone (blue for chlorates, purple and pink for perchlorates, green for chlorides, red, orange, and yellow for sulfates). Insoluble minerals precipitate at a water activity close to 1, while increasing solubility results in lower water activity. Therefore, highly soluble salts such as chlorates, perchlorates, and halides will deliquesce first, depending on the temperature.
Paper: Predictions for the Dynamical States of the Didymos System before and after the Planned DART Impact
Authors: Derek C. Richardson, Harrison F. Agrusa, Brent Barbee, William F. Bottke, Andrew F. Cheng, Siegfried Eggl, Fabio Ferrari, Masatoshi Hirabayashi, Özgür Karatekin, Jay McMahon, Stephen R. Schwartz, Ronald-Louis Ballouz, Adriano Campo Bagatin, Elisabetta Dotto, Eugene G. Fahnestock, Oscar Fuentes-Muñoz, Ioannis Gkolias, Douglas P. Hamilton, Seth A. Jacobson, Martin Jutzi, Josh Lyzhoft, Rahil Makadia, Alex J. Meyer, Patrick Michel, Ryota Nakano, Guillaume Noiset, Sabina D. Raducan, Nicolas Rambaux, Alessandro Rossi, Paul Sánchez, Daniel J. Scheeres, Stefania Soldini, Angela M. Stickle, Paolo Tanga, Kleomenis Tsiganis, Yun Zhang
Figure caption: Summary cartoons of dynamical excitation due to the DART impact. Panels (a) and (c) show a representation of the relaxed dynamics of the Didymos–Dimorphos system from a view above the orbit plane (a) and a view in the orbit plane (c). The DART impact is expected to excite the mutual orbit directly (b), causing the orbital period to change both in an average sense (by shrinking the orbit, in this case) and with fluctuations about the average (eccentric motion). It will likely also excite the libration of Dimorphos about different rotation axes, including: (d) yaw excitation, oriented along the rotation axis of Dimorphos—fluctuations in the rate of rotation during a given rotation and/or a change in the average rotation rate; (e) pitch excitation, oriented in and out of the orbit plane—a nodding of the face of Dimorphos from the perspective of Didymos; and (f) roll excitation, oriented about the axis connecting Dimorphos and Didymos—a rocking of the face of Dimorphos from the perspective of Didymos.
Paper: Predictions for the Dynamical States of the Didymos System before and after the Planned DART Impact
Authors: Derek C. Richardson, Harrison F. Agrusa, Brent Barbee, William F. Bottke, Andrew F. Cheng, Siegfried Eggl, Fabio Ferrari, Masatoshi Hirabayashi, Özgür Karatekin, Jay McMahon, Stephen R. Schwartz, Ronald-Louis Ballouz, Adriano Campo Bagatin, Elisabetta Dotto, Eugene G. Fahnestock, Oscar Fuentes-Muñoz, Ioannis Gkolias, Douglas P. Hamilton, Seth A. Jacobson, Martin Jutzi, Josh Lyzhoft, Rahil Makadia, Alex J. Meyer, Patrick Michel, Ryota Nakano, Guillaume Noiset, Sabina D. Raducan, Nicolas Rambaux, Alessandro Rossi, Paul Sánchez, Daniel J. Scheeres, Stefania Soldini, Angela M. Stickle, Paolo Tanga, Kleomenis Tsiganis, Yun Zhang
Figure caption: Dimorphos’s deformed shape and the resulting orbit period change as a function of the reshaping magnitude. (a) An example of the reshaping, where the horizontal axis (the y direction along the intermediate principal axis, in contrast to the z-axis along the maximum principal axis) corresponds to the leading side. (b) Orbital period change as a function of deformation along the leading direction. This change is in addition to any change in Dimorphos’s momentum due to the impact itself. The blue dots are derived from the FEM approach and the black line gives a linear approximation.
Paper: Predictions for the Dynamical States of the Didymos System before and after the Planned DART Impact
Authors: Derek C. Richardson, Harrison F. Agrusa, Brent Barbee, William F. Bottke, Andrew F. Cheng, Siegfried Eggl, Fabio Ferrari, Masatoshi Hirabayashi, Özgür Karatekin, Jay McMahon, Stephen R. Schwartz, Ronald-Louis Ballouz, Adriano Campo Bagatin, Elisabetta Dotto, Eugene G. Fahnestock, Oscar Fuentes-Muñoz, Ioannis Gkolias, Douglas P. Hamilton, Seth A. Jacobson, Martin Jutzi, Josh Lyzhoft, Rahil Makadia, Alex J. Meyer, Patrick Michel, Ryota Nakano, Guillaume Noiset, Sabina D. Raducan, Nicolas Rambaux, Alessandro Rossi, Paul Sánchez, Daniel J. Scheeres, Stefania Soldini, Angela M. Stickle, Paolo Tanga, Kleomenis Tsiganis, Yun Zhang
Figure caption: Didymos’s deformation process, based on DEM simulations, where the interior is modeled as a dense polydisperse packing of grains with a particle diameter distribution ranging between ∼4 m and ∼16 m. The bulk density is ∼2170 kg m−3 and the interparticle strength is ∼320 Pa (Zhang et al. 2021). The colors show the particle speeds. (a) The original shape at a spin period of 2.26 hr. (b) The deformed shape.
Paper: Predictions for the Dynamical States of the Didymos System before and after the Planned DART Impact
Authors: Derek C. Richardson, Harrison F. Agrusa, Brent Barbee, William F. Bottke, Andrew F. Cheng, Siegfried Eggl, Fabio Ferrari, Masatoshi Hirabayashi, Özgür Karatekin, Jay McMahon, Stephen R. Schwartz, Ronald-Louis Ballouz, Adriano Campo Bagatin, Elisabetta Dotto, Eugene G. Fahnestock, Oscar Fuentes-Muñoz, Ioannis Gkolias, Douglas P. Hamilton, Seth A. Jacobson, Martin Jutzi, Josh Lyzhoft, Rahil Makadia, Alex J. Meyer, Patrick Michel, Ryota Nakano, Guillaume Noiset, Sabina D. Raducan, Nicolas Rambaux, Alessandro Rossi, Paul Sánchez, Daniel J. Scheeres, Stefania Soldini, Angela M. Stickle, Paolo Tanga, Kleomenis Tsiganis, Yun Zhang
Figure caption: Didymos’s deformed shape and the resulting orbit period change as a function of the reshaping magnitude. (a) An example of reshaping making the shape more oblate along the maximum principal axis (corresponding to the spin axis, here the z-axis). The y-axis corresponds to the intermediate axis. (b) Orbital period change as a function of deformation along the leading direction. The blue dots are derived from the FEM approach and the black line gives a linear approximation.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: The mean-climate diagnostics in all experiments: (a) maximum equatorial zonal wind speed (x-axis; meters per second) and the latitude of the tropospheric jet (y-axis, degrees); (b) the ratio of the day–night to equator–pole temperature difference (x-axis) and the minimum surface temperature (y-axis, kelvin). Experiments that produce the SJ regime are shown in blue, DJ—in orange. Different marker shapes correspond to different groups of sensitivity experiments. Configuration labels are defined in Table 2. Also shown is the steady state of the (c) SJ and (d) DJ circulation regimes in the indicative simulations (Base and T0_280, respectively). Panels (c) and (d) show the vertical cross section of the zonal mean eastward wind (shading; meters per second) and zonal mean air temperature (contours, kelvin). Horizontal dashed lines in (c) and (d) show the corresponding pressure level of the horizontal cross sections of (red) temperature and (gray) winds and geopotential height shown in Figure 7. “Single jet” (SJ) and “double jet” (DJ) are short-hand descriptive terms rather than precise descriptions: the equatorial jet in the SJ regime exhibits a split at σ ≈ 0.5, and the DJ regime still has an equatorial superrotation, albeit weaker than that in the SJ regime.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Spin-up diagnostics for the (a) Base (b) T0_280 simulations: (brown) maximum zonal wind at the equator at 300 hPa and (cyan) the longitude of stationary Rossby wave crest. For reference, the wave crest longitude is also shown in Figures 7(c) and (d). An animation of the stationary wave pattern and zonal mean atmospheric structure during the first 500 days of the simulations is provided as Supplemental Video 1 (see also Figure 14).
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Spin-up diagnostics for the first 200 days of the (blue lines) Base and (orange lines) T0_280 simulations: (a) water vapor path, (b) shortwave radiative heating rate, (c) longwave radiative heating rate, (d) convective heating rate, (e) diabatic (radiative plus latent) heating rate, and (f) the Eady growth rate. The water vapor path is averaged over the day side, integrated vertically, and has units of kilograms per meter squared. The heating rates are averaged spatially over the day side and vertically over the troposphere and have units of kelvin per day. The Eady growth rate is averaged within ≈850–500 hPa in mid-latitudes (30°–80°) and has units of day−1.
Paper: Bistability of the Atmospheric Circulation on TRAPPIST-1e
Authors: Denis E. Sergeev, Neil T. Lewis, F. Hugo Lambert, Nathan J. Mayne, Ian A. Boutle, James Manners, Krisztian Kohary
Figure caption: Meridional profiles of the angular momentum budget terms (J m−3) in Equation (2) during the spin-up phase of the (left) Base and (right) T0_280 simulations: (orange) mean advection terms, (blue) stationary eddy terms, and (purple) transient eddy terms. The dashed black line shows the residual. The terms are averaged within the troposphere (≈1–20 km) and over the periods of (a) and (b) 0–20 days, (c) and (d) 20–80 days, (e) and (f) 80–200 days, and (g) and (h) 250–450 days. Note the jagged lines in the two top panels are due to a very short period of averaging (20 days).
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). I. Dry Cases—The Fellowship of the GCMs
Authors: Martin Turbet, Thomas J. Fauchez, Denis E. Sergeev, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne, Linda Sohl
Figure caption: Helmholtz decomposition of the horizontal wind at 250 hPa in the Ben 1 cases (quivers): (a)–(d) total wind, (e)–(h) zonal mean rotational component, (i–l) eddy rotational component, (m)–(p) divergent component. Note the different scaling of the eddy rotational and divergent components. Also shown is the upward wind velocity (shading, m s−1), with the 0.05 m s−1 highlighted by a black contour. Note that for ExoCAM only the pressure velocity (ω, Pa s−1) is available in the output, so the vertical velocity (w, m s−1) is approximated as w = − ω/ρ g, where ρ is air density and g is the acceleration due to gravity.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). I. Dry Cases—The Fellowship of the GCMs
Authors: Martin Turbet, Thomas J. Fauchez, Denis E. Sergeev, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne, Linda Sohl
Figure caption: Overturning circulation shown by the tidally locked mass stream function ΨTL (1011 kg s−1). The mass flux is clockwise where ΨTL is positive and counterclockwise where ΨTL is negative. The maximum of ΨTL in each GCM is shown in the upper left corner. The substellar point (SS) is at 90° latitude, and the antistellar point (AS) is at −90° latitude.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). I. Dry Cases—The Fellowship of the GCMs
Authors: Martin Turbet, Thomas J. Fauchez, Denis E. Sergeev, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne, Linda Sohl
Figure caption: Temporal variability of the surface temperatures (K) for the Ben 1 (top row) and Ben 2 (bottom row) simulations. Each column shows global mean, dayside mean, and nightside mean. Thin lines show the raw data; thick lines show a 2.5-orbit rolling mean.
Paper: The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). I. Dry Cases—The Fellowship of the GCMs
Authors: Martin Turbet, Thomas J. Fauchez, Denis E. Sergeev, Ian A. Boutle, Kostas Tsigaridis, Michael J. Way, Eric T. Wolf, Shawn D. Domagal-Goldman, François Forget, Jacob Haqq-Misra, Ravi K. Kopparapu, F. Hugo Lambert, James Manners, Nathan J. Mayne, Linda Sohl
Figure caption: Same as Figure 10, but for the Ben 2 simulations.
Paper: An Energy Balance Model for Rapidly and Synchronously Rotating Terrestrial Planets
Authors: Jacob Haqq-Misra, Benjamin P. C. Hayworth
Figure caption: Outgoing infrared radiative flux, F IR, as a function of temperature and CO2 partial pressure for a linear parameterization (top left, North et al. 1981), two polynomial parameterizations (top right, Williams & Kasting 1997; bottom left, Haqq-Misra et al. 2016), and the HEXTOR lookup table method (bottom right). The black region corresponds to numerically unstable solutions where CO2 condenses onto the surface. The lookup table method provides better representation of the underlying radiative–convective equilibrium model solutions for F IR, particularly at high temperatures.
Paper: An Energy Balance Model for Rapidly and Synchronously Rotating Terrestrial Planets
Authors: Jacob Haqq-Misra, Benjamin P. C. Hayworth
Figure caption: HEXTOR calculations of average temperature (T, top row) and planetary albedo (α, bottom row) for a TRAPPIST-1e-sized planet orbiting the Sun with 1 bar N2 and 400 ppm CO2. The left column shows results using a latitudinal EBM, and the right column shows results using a coordinate-transformed tidally locked EBM with maximum flux at the substellar point and zero flux at the night side. Results are shown for the Ben1 (lavender), Ben2 (red), Hab1 (blue), and Hab2 (orange) cases described by the THAI protocol.