adsabs/AstroCLIMB huggingface dataset:
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Snapshots of Theia’s mantle fragments with 50% 25 km and 50% 50 km radii.
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Time evolution of the entrainment rate of mixed-size Theia fragment volume over Earth’s 4.5 Gyr history.
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Snapshots of compositional (panels (a)–(d)) and corresponding viscosity (panels (e)–(h)) field for a case of higher initial temperature (T = 0.8) compared to the reference case.
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Snapshots of compositional (panels (a)–(d)) and corresponding viscosity (panels (e)–(h)) field for a model having higher temperature-dependent viscosity due to temperature change (A = 10.51) compared to the reference case.
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Snapshots of compositional (panels (a)–(d)) and corresponding viscosity (panels (e)–(h)) field for a case of different Rayleigh number (Ra = 7 × 107) compared to the reference case.
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Snapshots of Theia’s mantle fragments with 90% 25 km and 10% 50 km radii.
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Snapshots of Theia’s mantle fragments with 75% 25 km and 25% 50 km radii.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Volumetric water content of soil samples after the test. The experimental temperatures of (a)–(c) are −40°C, −100°C and −160°C respectively. In (a), the simulated lunar soil, loess, and montmorillonite are the same group of samples, which were simultaneously placed in the chamber and experienced the same temperature and environmental pressure process. Identical to (b) and (c). The montmorillonite samples in (d) at −40°C and the three soil samples in (a) were simultaneously placed in a chamber and underwent the same temperature and environmental pressure processes. The montmorillonite samples in (d) with −100°C and the three soil samples in (b) underwent the same temperature and environmental pressure processes. The montmorillonite samples in (d) with −160°C and the three soil samples in (c) underwent the same temperature and environmental pressure processes. The position marked ‘‘0 cm’’ corresponds to the soil at the bottom of the container, while “2.5 cm” refers to the soil at the top. The length of each vertical step in the plot represents the thickness of each soil layer during stratified sampling. Figures (a)–(c) correspond to samples with water ice placed at the bottom, as shown in Figure 6(a). Figure (d) presents the postexperiment volumetric water content of the montmorillonite sample from the test container without bottom ice, corresponding to the configuration shown in Figure 6(b).
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Overview of the environmental simulation chamber and sample position.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Moisture adsorption heat curve measured by the adsorption isobar method.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Sample container loaded with soil and ice.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Effective pore size distribution curve measured by mercury porosimetry.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Environmental pressure corresponds to soil temperature at different Knudsen number conditions. The vertical line corresponding to a soil temperature of ﹩273\,{\rm{K}}﹩ (approximately 0°C) is also shown.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Sample loading. (a) Frozen water sample. (b) Soil sample loading. (c) The ice and soil samples were combined and then frozen.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Cumulative size–frequency diagram for the soil used in this paper and the actual lunar soil (The lines of the lunar soil were referenced with G. H. Heiken et al. 1991).
Paper: The Mineralogical Connection between M- and K-type Asteroids as Indicated by Polarimetry
Authors: Joseph R. Masiero, Yuna G. Kwon, Elena Selmi, Manaswi Kondapally
Figure caption: The same as Figure 1, showing the combined data for M- and K-types, the best fits to these data, with the best-fit curve to the (21) Lutetia V-band data overlaid.
Paper: The Mineralogical Connection between M- and K-type Asteroids as Indicated by Polarimetry
Authors: Joseph R. Masiero, Yuna G. Kwon, Elena Selmi, Manaswi Kondapally
Figure caption: The best-fit V-, J-, and H-band curves shown in Figure 3 compared to laboratory measurements of troilite–olivine mixtures from R. Sultana et al. (2023b). FeS/Oliv = 90/10 is a mixture of 90% troilite and 10% olivine, while FeS/Oliv = 80/20 is an 80%/20% mixture. See R. Sultana et al. (2023a) for more details on the sample materials.
Paper: The Mineralogical Connection between M- and K-type Asteroids as Indicated by Polarimetry
Authors: Joseph R. Masiero, Yuna G. Kwon, Elena Selmi, Manaswi Kondapally
Figure caption: The same as Figure 1, showing polarimetric phase curves for M-type asteroid (21) Lutetia.
Paper: The Mineralogical Connection between M- and K-type Asteroids as Indicated by Polarimetry
Authors: Joseph R. Masiero, Yuna G. Kwon, Elena Selmi, Manaswi Kondapally
Figure caption: The same as Figure 1, showing polarimetric phase curves for K-type asteroids (89) Julia, (221) Eos, and (233) Asterope.
Paper: The Mineralogical Connection between M- and K-type Asteroids as Indicated by Polarimetry
Authors: Joseph R. Masiero, Yuna G. Kwon, Elena Selmi, Manaswi Kondapally
Figure caption: The same as Figure 1, showing polarimetric phase curves for S/L-type asteroid (12) Victoria.
Paper: The Mineralogical Connection between M- and K-type Asteroids as Indicated by Polarimetry
Authors: Joseph R. Masiero, Yuna G. Kwon, Elena Selmi, Manaswi Kondapally
Figure caption: The same as Figure 1, showing polarimetric phase curves for T-type asteroid (72) Feronia.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Environmental pressure of the chamber during the test.
Paper: Experimental Investigation of Soil Adsorption Effects on Water Migration in Simulated Lunar Conditions
Authors: Yasheng Li, Zhi Wen, Wei Ma, Mingli Zhang, Chengdan He
Figure caption: Effect of soil temperature on the water loss rate.
Paper: The Mineralogical Connection between M- and K-type Asteroids as Indicated by Polarimetry
Authors: Joseph R. Masiero, Yuna G. Kwon, Elena Selmi, Manaswi Kondapally
Figure caption: Polarimetric phase curves for M-type asteroids (16) Psyche, (55) Pandora, (135) Hertha, and (216) Kleopatra. J- and H-band observations were obtained using Palomar/WIRC+Pol, while the visible bands are from D. Lupishko (2022). Points show the measurements, while the lines are best-fit polarization phase curves based on theoretical scattering models. The light-blue and light-yellow lines show the best-fit curves to the NIR polarization-phase relationships for C-types at all wavelengths and S-complex objects at the H band (respectively, noted as “Ctype—std” and “Stype—H std”) as derived by J. Masiero et al. (2022) for comparison.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Conceptual phase diagrams illustrating (a) equilibrium features, (b) metastable features, and (c) glass transition features in an aqueous salt system. The x-axis represents increasing solute concentration, and the y-axis represents temperature. In panel (a), stable equilibrium boundaries are shown, including ice–liquid and liquid–solid solute phase fields, with the eutectic composition (Xe). In panel (b), the metastable regime appears below the equilibrium lines, where supercooled liquids and hyper- or hypoeutectic transitions occur, illustrating how solutions can bypass crystallization. In panel (c), the bulk vitrification Tg curve depicts the onset of glass formation, showing how supercooled liquids may eventually vitrify. The freeze concentrated solution will show a glass transition temperature between T′g,min and T′g,max, although the relative positions of these values with respect to the eutectic may change depending on the solute’s glass-forming ability. Below the liquidus curve, THom refers to the homogeneous nucleation temperature. In the hypoeutectic region, nonideal effects may prevent the linear extrapolation to the Tg of pure water; bulk vitrification is generally not possible in the unstable region defined by the theoretical Tg curve (shown by the dashed gray line). Instead, this region is often dominated by freeze concentration.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Glass transition temperatures (Tg) for four oxychlorine solutions at the MFCS, eutectic, and critical concentrations, respectively, for (a) Ca(ClO4)2, (b) Mg(ClO4)2, (c) Ca(ClO3)2, and (d) Mg(ClO3)2 as a function of cooling rate (ΔT). In each panel, the black dashed curve indicates the maximum freeze concentration solution (MFCS) at the specified molality with the shaded region around the curve showing variance. The solid black curve denotes the equilibrium eutectic composition for the corresponding solution, and the light gray region highlights the difference between the eutectic and MFCS curves, indicating the most likely region for the Tg in a freeze concentrated solution to occur. The critical concentration is given by the dotted line. Displayed solely for reference, the Tg of pure water (136 ± 2 K) is shown as a constant benchmark that does not vary with oxychlorine cooling rate and is included to provide context.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Calculated water activity (aw) as a function of initial solution molality and temperature using Pitzer parameters from J. D. Toner et al. (2015). The top row shows a heat map with isolines for activity, while the bottom row is in the style of A. H. Stevens & C. S. Cockell (2023) and contextualizes aw in terms of currently known limits for life. The rectangular areas show where freeze concentration as a result of ice precipitation is most likely to occur, proceeding until the MFCS is reached. The eutectic temperature is shown as a white dotted line, while a value of 0.6 aw is given by the black dotted line, and the solid white line shows the critical concentration, above which bulk vitrification may occur. Red shaded regions are uninhabitable for known terrestrial life, whereas green shaded regions are habitable. Yellow shaded regions indicate the transition zone. Thus, if the MFCS is reached, then the residual brine falls outside estimates of habitable aw.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Phase diagrams with metastable features for (a) Ca(ClO4)2 and (b) Mg(ClO4)2 with Tg curves, supercooling, and freeze concentration regions depicted. Solubility data are from J. D. Toner et al. (2014) and references therein. Freeze concentration regions are shaded in gray and the dotted line shows the eutectic temperature. Below the eutectic, the glass phases (calculated as Tg onset) formed via supercooling are shown for both fast (200 K minute−1) and slow rates (0.5 K minute−1). At concentrations more dilute than the eutectic, primary ice precipitates first, resulting in a residual freeze-concentrated liquid that vitrifies at an approximately constant temperature (T′g). This behavior suggests that, at lower concentrations, a slushy, metastable layer may persist.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Phase diagrams with metastable features for (a) Ca(ClO3)2 and (b) Mg(ClO3)2 according to solubility data from J. Hanley et al. (2012). Solid lines indicate ice and salt solubilities with the dotted line showing the eutectic temperature. Below the eutectic, the glass phase (calculated as Tg onset) is shown for both fast and slow rates. Freeze concentration regions are shaded in gray. At concentrations more dilute than the eutectic, primary ice precipitates first, resulting in a residual freeze-concentrated liquid that vitrifies at an approximately constant temperature (T′g). This behavior suggests that, at lower concentrations, a slushy, metastable layer may persist.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Modeled effect of initial concentration and ΔT (rate of cooling or warming) on aqueous calcium and magnesium (per)chlorate solutions. Panels (a) and (b) display the glass transition temperature (Tg) for Ca(ClO3)2 and Ca(ClO4)2, respectively, while panels (c) and (d) show the corresponding values for Mg(ClO3)2 and Mg(ClO4)2. The solid lines represent the eutectic temperature (TE), while the dashed line indicates the maximum freeze-concentrated solution (MFCS), which may be supersaturated. The critical temperature for vitrification (Tcrit) is also marked, below which bulk vitrification does not readily proceed. The light-toned region represents where freeze concentration occurs, and the black arrows point to increasing concentration of the residual liquid until the MFCS threshold. The color bars indicate the onset temperature of the glass transition.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Illustration of the brine vein network between ice grains with brine pockets at the crystal junctions. Such brine channels have been observed in terrestrial sea ice on the order of 10–100 μm (e.g., C. Krembs et al. 2011), which is comparable to the sample volume used in this study. In oxychlorine-rich brines, these brine pockets could exist in a supercooled state or even transition into glass.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: First column shows cold crystallization after devitrification of 3.0 m Mg(ClO4)2 at ΔT = 5, 10, and 20 K minute−1, respectively, while second column shows cold crystallization after devitrification for 6.0 m Ca(ClO3)2 at ΔT = 5, 10, 20, and 50 K minute−1, respectively For Mg(ClO4)2, cold crystallization was eliminated in a 50 K minute−1 sample. The cold crystallization event is characterized by an exothermic peak, indicating the transformation of amorphous material into a crystalline structure upon warming. Conversely, the melting process is observed as an endothermic trough, signifying the transition of crystalline regions into the liquid phase. The exothermic peak area closely matches the endothermic melting trough across all measured rates, further confirming that the entirety of the cold crystals undergoes melting.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: (a) Example of a DSC thermogram for 9.4 molality Ca(ClO3)2 showing bulk vitrification of a brine and the glass transition temperature using 5 K minute−1 cooling and warming rates. (b) Example of the variation of the glass transition with concentration for Ca(ClO3)2 at 5 K minute−1 for warming. “Exo” refers to the exothermic direction of the thermogram. The only phase transition present in the bulk vitrified samples is the glass transition, which is identifiable by the step change in heat capacity at a given temperature shown here within the blue boxes.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Examples of DSC thermograms of hypoeutectic solutions of Ca(ClO4)2 and Mg(ClO4)2 exhibiting freeze concentration. The glass transition was evident upon both cooling and warming in all experiments and could be confirmed in the derivative. A hysteresis effect, as clearly seen in the derivative, is noted in the glass transition region for all experiments upon warming. “Exo” refers to the exothermic direction of the thermogram. The glass transition region, highlighted in the inset plot, shows the comparatively subtle glass phase transition. While freezing and melting are demarked by large exothermic and endothermic peaks, respectively, the glass transition is identified by a step change in heat capacity.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: (a), (d) Variation of the glass transition temperature (Tg) vs. the warming rate of the glass (log |ΔT| (K minute−1)) for calcium and magnesium chlorate. (b), (e) Variation of Tg with concentration (molality (mol kg−1)). The glass transition temperature depends both on the concentration of the perchlorate solution and the warming or cooling rates. Subfigures (c) and (f) show the excellent agreement and linearity between the parameterized and measured values, where predicted values fall on or within a confidence interval of 95%.
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Comparison of the mass fraction of ice (white circles) or glass (black circles) with the initial molality of the solution for chlorates and perchlorates. For the conditions of this study, pure water is expected to form crystalline ice. Error bars are near or within the symbols and represent the variation resulting from differing |ΔT| (K minute−1).
Paper: Freeze Concentration, Supercooling, and Glass Formation in Perchlorate and Chlorate Brines: Habitability in Salty Martian Ice
Authors: Ardith Bravenec, David C. Catling
Figure caption: Examples of DSC thermogram of cold crystallization (the exothermic peak during the warming ramp, between Tg and melting) for NaClO4. The glass transition was evident upon both cooling and warming in all experiments and could be confirmed in the derivative.
Paper: Investigating Local- and Global-scale Dust Redistribution on Comet 67P/Churyumov–Gerasimenko
Authors: Jacob L. Kloos, Tony L. Farnham, Jessica M. Sunshine, Juan Luis Rizos
Figure caption: Modeled thickness of dust material removed between 3 au pre-perihelion and 3 au post-perihelion. The stark asymmetry between the northern and southern hemisphere is due to the coincidence of southern summer with perihelion. Local topography is also observed to influence the local gas and dust activity.
Paper: Investigating Local- and Global-scale Dust Redistribution on Comet 67P/Churyumov–Gerasimenko
Authors: Jacob L. Kloos, Tony L. Farnham, Jessica M. Sunshine, Juan Luis Rizos
Figure caption: Modeled thickness of dust material accumulated between 3 au pre-perihelion and 3 au post-perihelion owing to airfall. Strong rotational effects are observed as the comet sweeps up coma material throughout its counterclockwise rotation.
Paper: Investigating Local- and Global-scale Dust Redistribution on Comet 67P/Churyumov–Gerasimenko
Authors: Jacob L. Kloos, Tony L. Farnham, Jessica M. Sunshine, Juan Luis Rizos
Figure caption: Simulated trajectories of dust particles emitted from the surface at nonescaping velocities (v = 0.1–0.7 m s–1) with respect to a body-fixed reference frame. The warped trajectories are the result of the weak gravitational attraction combined with the rotation of the nucleus. As will be shown, the effects of rotation have a strong effect on the distribution of dust fallback.
Paper: Investigating Local- and Global-scale Dust Redistribution on Comet 67P/Churyumov–Gerasimenko
Authors: Jacob L. Kloos, Tony L. Farnham, Jessica M. Sunshine, Juan Luis Rizos
Figure caption: Sample output of thermal sublimation model at 2.5 au. Instantaneous irradiance (left), surface temperature (middle), and water sublimation rate (right) on C-G are computed using a DSM with 50,000 facets. This figure illustrates that the temperature and sublimation are governed by the instantaneous illumination conditions.
Paper: Investigating Local- and Global-scale Dust Redistribution on Comet 67P/Churyumov–Gerasimenko
Authors: Jacob L. Kloos, Tony L. Farnham, Jessica M. Sunshine, Juan Luis Rizos
Figure caption: Comparison of modeled dust fallback distribution and OSIRIS imagery highlighting the topographic influence of airfall. Model results show how the leading edges accumulate more material than the trailing edges. This is supported by OSIRIS images, which show smoother, accumulated terrain on the leading edge and craggy rough terrain in more eroded areas.
Paper: Investigating Local- and Global-scale Dust Redistribution on Comet 67P/Churyumov–Gerasimenko
Authors: Jacob L. Kloos, Tony L. Farnham, Jessica M. Sunshine, Juan Luis Rizos
Figure caption: Net accumulation of dust material across one orbital cycle, calculated as “(Gain – Loss).”
Paper: Investigating Local- and Global-scale Dust Redistribution on Comet 67P/Churyumov–Gerasimenko
Authors: Jacob L. Kloos, Tony L. Farnham, Jessica M. Sunshine, Juan Luis Rizos
Figure caption: Subsolar latitude vs. heliocentric distance of C-G. The Sun is concentrated in the south at and after perihelion, whereas the north is never strongly illuminated. The points represent the diurnal epochs that were simulated in this work.