adsabs/AstroCLIMB huggingface dataset:
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Comparison between the former emissivity (0.9, left) and the new one (0.99 over the lake and 0.95 over the land, right). The simulation shown in the middle is an intermediate case, with the emissivity set to 0.95 over the lake and the land. Rows, from top to bottom: surface temperature, horizontal wind at 2 m above the surface, TKE at 2 a.m., and TKE at 2 p.m.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Horizontal wind at 2 a.m. at different seasons. (a) Autumn, (b) winter, (c) spring, and (d) summer. The black arrows represent the wind speed and direction to show the relative strength of the wind in the general circulation and close to the lake.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: (a) Horizontal wind at 2 m above the surface. (b) Relative humidity at 2 a.m.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Modern-day Earth estimates of reservoirs and fluxes of the slow carbon system considered in our model, in units of gigatonnes of carbon (GtC, 1012kg C) from C.-T. Lee et al. (2019). There is significant uncertainty in modern-day flux values. Carbon in continental crust (∼42 × 106 GtC), continental lithospheric mantle (≲48 × 106 GtC), and oceanic crust/lithospheric mantle (∼14 × 106 GtC) are not tracked in our simulations, as they are much larger than surface reservoirs and are treated as functionally inexhaustible.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Top: SiO2 weathering flux as a function of globally averaged surface temperature for various soil ages determined by the “mountainous” (tectonically active/high erosion) Dw = 0.3 m yr−1 (blue), “global average” 0.03 m yr−1 (green), and “cratonic” (tectonically inactive/low erosion) 0.01 m yr−1 (orange) values from K. Maher & C. P. Chamberlain (2014) Fluxes are calculated assuming a latitude of Φ = 0°; most weathering occurs at low latitude in our model. Bottom: climate feedback strength α as a function of global temperature. A higher value of α represents a climate more stable to perturbations in weathering or outgassing fluxes. MAC model values are presented alongside the WHAK formulation (Equation (5); black). Wiggles in feedback strength are due to the nonlinear dependence of temperature as a function of pCO2 in our model. The gray triangle represents an estimate for the modern-day globally averaged value of α from S. L. Brantley et al. (2023), which is very close to the value calculated for the global average Dw.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: An example run of the base DISKWORLD model spanning 4 Gyr, showing disk configurations and localized weathering fluxes at three select times. Arrows represent disk velocities. Here t1 shows how the introduction of colliding disks leads to a gradual decrease in atmospheric pCO2 and global temperatures. At t2, although there are no currently colliding disks, the high pCO2 and global temperatures lead to increased global weathering fluxes owing to the carbonate–silicate weathering feedback (see Figure 2), which is strong enough even in “cratonic” soils to prevent massive CO2 buildup. Here t3 represents an example state with large amounts of colliding disks near the equator, greatly increasing global weathering fluxes, potentially leading to a future snowball event.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Snowball and catastrophic warming rates over 4 Gyr for variable outgassing trials explained in Section 4.3. Crosses indicate scenarios sampled. These trials reveal that planets with lower land fractions, while stable to tectonic noise, are highly susceptible to climate catastrophes caused by volcanic outgassing variability. In addition, longer-term and higher-amplitude outgassing perturbations spell doom for an Earth-like (N = 8, Aland = Aland,⊕; panel (b)) setup. Note that the apparent decrease in snowball rate at long relaxation timescales is caused by an accompanying increase in catastrophic warming, and thus the total survival rate does not increase.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Output (pCO2/average surface temperature, global weathering, weatherability, average land latitude, and colliding area) for 10,000 model runs of the collisional case, where soil age is solely controlled by disk collisions (Section 4.1). In these model runs, frequent disk collisions are required to generate the high resurfacing rates needed to stabilize the climate over geologic timescales. All trials that begin with no colliding disks quickly reach catastrophic warming as their soils become leached of cations available for weathering. Differences in the time to catastrophe for these trials are dictated by their prescribed CO2 outgassing rates, which are generally proportional to trial land area.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Survival rates over 4 Gyr as a function of disk number and total land area for trials with evolving solar luminosity and evolving outgassing (based on geothermal heat flux; Section 4.4). Low survival rates for both low number of disks and low land area augment similar results from varying outgassing fluxes (Figure 8) and suggest that frequent collisions are required for long-term habitability.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Output for 10,000 trials where collisions reset the local effective soil age and soils retain a minimum fraction of fresh minerals for weathering approximating the effects of nontectonic processes on weathering (Section 4.2). Despite large (≳2×) perturbations in weatherability, the silicate weathering feedback is able to stabilize climate in the vast majority of trials. Most catastrophic warming events in these trials were triggered by previously colliding disks breaking up, causing soils to age and weathering fluxes to decrease drastically.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: A comparison of modern-day Earth precipitation estimates (black; from the Climate Prediction Center Merged Analysis of Precipitation; P. Xie & P. A. Arkin 1997) to our simplified latitudinal dependence of precipitation (green; Equation (13)). Red and blue dotted lines indicate effects of a 10°C warming and cooling, respectively.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Survival rates for the 4 Gyr collisional DISKWORLD model runs, where collisions form mountain belts endowed with young, highly weatherable soils. Black crosses indicate the scenarios sampled. The survival rate for the Earth-like case (A = A⊕, Ndisk = 8) is 10% (panel (a)) and 97% (panel (b)).
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Output for 5000 trials including evolving solar luminosity and outgassing fluxes as described in Section 4.4.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Model runs showing the time variability of pCO2 for a wide variety of tectonic setups, including pCO2/temperature-dependent SFW as discussed in Section 4.5 based on J. Krissansen-Totton et al. (2018), omitting luminosity evolution and outgassing variation. In these trials, SFW acts as an extremely stabilizing negative feedback, showing only small variations in pCO2 over Gyr timescales. These results suggest that SFW may be an additional important stabilizing negative feedback in the slow carbon cycle.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Survival rates over 4 Gyr for an Earth-like tectonic setup (Aland = Aland,⊕, N = 8) with a variety of starting global average temperatures assuming present-day solar luminosity. “Seafloor Weathering” trials include pCO2/temperature-dependent SFW as discussed in Section 4.5, “Only Tectonic Noise” trials do not include the maximum soil age discussed in Section 4.2, and “Variable Outgassing” trials use the “moderate” values for stochastic outgassing variation (τ = 30 Myr, σ = 2 × 10−4 Tmol yr−1; Section 4.3).
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Model output for 1000 trials with evolving solar luminosity including pCO2/temperature-dependent SFW as described in Section 4.5. Similar to Figure 12, these trials, when compared to the low survival rate of Figure 9, further suggest that SFW acts as an additional important stabilizing feedback to the slow carbon system. Climate catastrophes in these trials are exclusively caused by the sudden introduction of large amounts of weatherable material at low latitudes.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Top: SiO2 weathering flux as a function of globally averaged surface temperature for various soil ages following Figure 2. Solid lines include the temperature and pCO2 dependencies derived in M. J. Winnick & K. Maher (2018) assuming that soil pCO2 is in equilibrium with atmospheric pCO2 (Equations (9) and (10)), while dashed lines represent the original formulation of K. Maher & C. P. Chamberlain (2014). Bottom: climate feedback strength α as a function of global temperature following Figure 2.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Climate feedback strength α as a function of solar luminosity for a fixed global average temperature of ﹩\bar{T}=13^\circ {{\rm{C}}}﹩ (assuming 0° latitude). For a fixed global temperature, lower luminosity entails higher pCO2 concentrations. Climates with higher pCO2 show a lower climate feedback strength owing to the pCO2 dependency of weathering in the WHAK and MAC models.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Output for 5000 trials including evolving solar luminosity with a fixed outgassing flux. High pCO2 initial states at lower luminosities lead to high initial weathering and outgassing rates. If these outgassing rates do not decrease owing to evolving geothermal heat fluxes, the carbonate–silicate weathering feedback is not strong enough to prevent catastrophic warming in a large number of these trials.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Model results from 2000 trials assuming a fixed luminosity of L = 0.9 L⊙. These trials show much higher catastrophe rates than trials run at modern-day luminosity (Section 4.2; snowballs: 6% vs. 0.2%; catastrophic warming: 23% vs. 4.5%) owing to weaker climate feedback strength in high pCO2 climates (Figure 15).
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Silica discharge rates and carbon consumption rates associated with various rivers presented in J. Gaillardet et al. (1999). The size of each point represents the total discharge of dissolved solids and associated weights for each river in our slope determination. The line represents the linear relationship of slope 1.087 used in our model.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Example trajectories of four disk centers over 4 Gyr, assuming an initial (and constant) velocity distribution of V = 4 ± 2 cm yr−1.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Effects of ocean volume on carbon partitioning in our model, showing the long-term response of atmospheric/ocean CO2 content, globally average surface temperature, and ocean pH to carbon perturbations up to 10 TtC (teratonnes of carbon (1 TtC = 1000 GtC)), 10 TtC is about 25% of the current ocean–atmosphere reservoir, based on methods outlined in Section A.3. Blue lines represent an Earth-like ocean volume, whereas green and orange represent half and twice that volume, respectively. RC is the ratio of carbon stored in the atmosphere to carbon stored in the ocean. Dashed lines represent initial conditions. Initial states were created assuming a pCO2 of 280 μbar, resulting in ﹩\sim \frac{1}{2}﹩ and ∼2 times the total carbon reservoir for the shallow and deep ocean scenarios, respectively. The climates of planets with smaller oceans are more sensitive to a given CO2 perturbation. Increasing RC values for CO2 injections show that the ocean carbon sink becomes less effective as more carbon is added to the system.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: pCO2 curves for 4000 trials using a 10× (a) slower and (b) faster average disk velocity than our base trials. While both trials show relatively high survival rates, initial collision states (disk configurations) determine long-term behavior for slower disk velocities, whereas faster velocities introduce more variability in pCO2 and higher collision frequency.
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Model output pCO2 for 2000 trials with (a) half of Earth’s current ocean depth and (b) twice Earth’s current ocean depth. As suggested in Figure A4, larger ocean volumes act as a stronger buffer to perturbations in the slow carbon cycle and show lower climate catastrophe rates (3.8% vs. 20.3%).
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Climate feedback strength α as a function of globally averaged temperature for varying effective soil age and activation energy of mineral dissolution Ea, similar to Figure 2. The gray triangle represents the global estimate from S. L. Brantley et al. (2023).
Paper: The Role of Tectonic Luck in Long-term Habitability of Abiotic Earth-like Planets
Authors: Brandon Park Coy, Edwin S. Kite, R. J. Graham
Figure caption: Model output for 1000 trials including artificially increased weathering fluxes, as described in Appendix B.4. Runs show similar behavior and catastrophe rates to results shown in Section 4.2 (Figure 6).
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: List of the simulations used in this work. z0: roughness length, α: albedo, and I thermal inertia. Bold highlights the parameters changes compared to the reference simulation. The topography shape is described in more detail in Section 2.2, and the terrain relief is 300 m in each case.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Diagram of the model domain. (a) To scale. (b) Magnification of the center of the domain. Bottom right: values for some important parameters, left constant for this study. Remark: 16 s corresponds to 1 Titan second.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Horizontal background wind used for the season runs (from the TAM model at 74°N; J. M. Lora et al. 2022). For the background wind runs, the autumn profile is used.
Paper: The Role of Ammonia in the Distribution of Volatiles in the Primordial Hydrosphere of Europa
Authors: Alizée Amsler Moulanier, Olivier Mousis, Alexis Bouquet, Christopher R. Glein
Figure caption: Evolution at T = 300 K of the final distribution of species in the atmosphere and ocean at equilibrium as a function of ﹩{y}_{{\rm{N}}{{\rm{H}}}_{3}}^{{\rm{i}}{\rm{n}}{\rm{i}}}﹩, the initial mole fraction of NH3 incorporated into the atmosphere. The initial mole fractions of all other species remain constant. Only the three most abundant ions—HCO﹩{}_{3}^{-}﹩, NH﹩{}_{4}^{+}﹩, and NH2COO−—are displayed in this figure. The dashed gray line corresponds to the pH of the ocean calculated as a function of ﹩{y}_{{\rm{N}}{{\rm{H}}}_{3}}^{{\rm{i}}{\rm{n}}{\rm{i}}}﹩.
Paper: The Role of Ammonia in the Distribution of Volatiles in the Primordial Hydrosphere of Europa
Authors: Alizée Amsler Moulanier, Olivier Mousis, Alexis Bouquet, Christopher R. Glein
Figure caption: Model scheme representation. The model represents the dissolution of volatiles from the primordial atmosphere into the ocean. The liquid–vapor equilibrium of the volatile species is coupled to a chemical equilibrium model that considers the speciation of H2O, CO2, and NH3. This coupled approach allows the partitioning of the volatiles between the atmosphere and the ocean to be determined, taking into account both physical and chemical equilibrium. This model does not account for water–rock interactions between the ocean and silicate mantle.
Paper: The Role of Ammonia in the Distribution of Volatiles in the Primordial Hydrosphere of Europa
Authors: Alizée Amsler Moulanier, Olivier Mousis, Alexis Bouquet, Christopher R. Glein
Figure caption: Volatile abundances at equilibrium in the primordial atmosphere and ocean of Europa at T = 300 K. Two initial distributions are considered: Case 1a (solid), based on the composition of Comet 67P; and Case 1b (hatched), derived from a high-CO2 end-member composition. Final atmospheric fractions are expressed as partial pressures (Pascal), while dissolved volatile fractions are presented as mole fractions. The percentage share of each species in each phase is displayed above each vertical bar. The figure highlights only the two most abundant ions: HCO﹩{}_{3}^{-}﹩ and NH﹩{}_{4}^{+}﹩.
Paper: The Role of Ammonia in the Distribution of Volatiles in the Primordial Hydrosphere of Europa
Authors: Alizée Amsler Moulanier, Olivier Mousis, Alexis Bouquet, Christopher R. Glein
Figure caption: Volatile abundances at equilibrium in the primordial atmosphere and ocean of Europa at T = 300 K. Two initial distributions are considered: one with ﹩{P}_{{\rm{C}}{{\rm{O}}}_{2}}﹩ initially set to 1 bar (Case 2a, solid) and another with ﹩{P}_{{\rm{C}}{{\rm{O}}}_{2}}﹩ initially set to 10 bar (Case 2b, hatched). Atmospheric fractions are represented as partial pressures (Pascal), while dissolved volatile fractions are shown as mole fractions. The figure displays only the two most abundant ions, HCO﹩{}_{3}^{-}﹩ and NH﹩{}_{4}^{+}﹩.
Paper: The Role of Ammonia in the Distribution of Volatiles in the Primordial Hydrosphere of Europa
Authors: Alizée Amsler Moulanier, Olivier Mousis, Alexis Bouquet, Christopher R. Glein
Figure caption: Evolution of final partial pressures and mole fractions in the ocean at equilibrium as a function of temperature. Not all dissolved ions in the ocean are displayed in the figure, even though they are present in the mixture.
Paper: History and Habitability of the LP 890-9 Planetary System
Authors: Rory Barnes, Laura N. R. do Amaral, Jessica Birky, Ludmila Carone, Peter Driscoll, Joseph R. Livesey, David Graham, Juliette Becker, Kaiming Cui, Martin Schlecker, Rodolfo Garcia, Megan Gialluca, Arthur Adams, MD Redyan Ahmed, Paul Bonney, Wynter Broussard, Chetan Chawla, Mario Damasso, William C. Danchi, Russell Deitrick, Elsa Ducrot, Emeline F. Fromont, Brandt A. L. Gaches, Sakshi Gupta, Michelle L. Hill, James A. G. Jackman, Estelle M. Janin, Mikołaj Karawacki, Matheus Daniel Koren, Roberto La Greca, Michaela Leung, Arturo Miranda-Rosete, Michael Kent A. Olohoy, Cecelia Ngo, Daria Paul, Chandan Kumar Sahu, Debajyoti Basu Sarkar, Mohammad Afzal Shadab, Edward W. Schwieterman, Melissa Sedler, Katie Texeira, Allona Vazan, Karen N. Delgado Vega, Rohit Vijayakumar, Jonathan T. Wojack
Figure caption: An example of the thermal and magnetic evolution of LP 890-9 b and c from the EqTide, ThermInt, and RadHeat modules. Both fiducial integrations are representative cases from the larger integration set presented in Figure 9, with the viscosity activation energies of Av,b = 2.9 · 105 and Av,c = 3.1 · 105 chosen so that both planets have approximately equal initial tidal Q ≈ 30. Both planets have initial eccentricities of e ~ 0.1, and masses of mb = 2.3M⊕ and mc = 2.9M⊕. The interior structures of both planets are otherwise assumed to be Earth-like. Throughout the integration, LP 890-9 c has a consistently higher volumed-averaged core temperature and generally has a higher volumed-averaged mantle temperature than LP 890-9 b. In the upper right panel, we see that LP 890-9 b's internal heat budget is driven by radiogenic heating for the full integration lifetime, while LP 890-9 c has a significant contribution from tidal heating, which increases in total power as its orbital eccentricity begins to decay by the end of the integration (bottom left panel). The tidal heating drives mantle heating, leading to higher sustained volume-averaged mantle temperatures for LP-890c. Both planets have nonzero magnetic moments for the majority of the integration, and experience declining eruption rates as the planets age.