adsabs/AstroCLIMB huggingface dataset:
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: Factoring of the efficiency into two terms η = ϵ η  0 . (a) The 2D-IceOnly model provides a fast-solve numerical prediction of the design efficiency η  0 , with uncertainty derived from experimental errors in v and T and literature errors in thermal conductivity. We compare the individual points to theoretical curves for 253 K (red) and 79 K (black). (b) The operational efficiency ϵ is then derived by dividing the total efficiency by η  0 . Because we have both measured the total efficiency and modeled it with the 2D-Water+Ice model (Figure 10), we compare ϵ  M  to ϵ  E . Multiplication of results (a) and (b) restores the total efficiency, with some of the errors canceling in the multiplication, especially the errors in ϵ  E , which are due to uncertainty in the inputs to ﹩{\dot{Q}}_{{\min }}﹩. For clarity, CryoA1 and CryoB1 have been omitted. The blue circles represent 2D model results for three scenarios where the 2D- and 3D-Water+Ice models diverge at low operational efficiency and one where they agree at high operational efficiency. In these cases, the 3D-Water+Ice model is used for comparison with experiment, while all other points utilize the 2D-Water+Ice model.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: Three regimes of operation (CryoB2, CryoB3, CryoC2), distinguished by their experimental and modeled operational efficiencies ϵ E  and ϵ  M , the locations of maximal probe wall temperature, and the size and shape of the water jacket surrounding the probe. CryoB3 (middle) illustrates efficient behavior, with well-distributed heat. The other examples present as inefficient either because insufficient heat is being distributed to the back of the system (left example, CryoB2) or because an excess of heat is distributed to the side and rear of the system (right two diagrams, CryoC2). The latter, if sufficiently promoted, evolves into a natural convection-dominated regime that results in a long melt plume and an undulated water melt jacket lacking axisymmetry, requiring a fully 3D model to properly resolve these effects. In this case, the prediction for the total heat differs significantly between the 2D- and 3D-Water+Ice models.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: The residual between models, defined as the 2D-IceOnly numerical model minus a given analytical model, normalized by the 2D-IceOnly numerical model. The residual is shown as a function of the parameter ﹩{\left({vR}/{\alpha }_{{0}}\right)}^{2}﹩, which suppresses end effects for the heat equation. These end effects are neglected in the derivation of the analytical models, so that numerical and analytical models converge for large values of ﹩{\left({vR}/{\alpha }_{{0}}\right)}^{2}﹩. Due to the limited scale of laboratory test beds, the models are validated in the gray shaded region, while large-scale flight concepts are expected to operate in the green shaded region.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: Hierarchy of steady-state cryobot models, starting with the highest fidelity model at the top. Computational cost is reduced by successive approximations, including (a) limiting the Rayleigh number (Ra) in the melt plume to establish axial symmetry; (b) designing to near-maximal operational efficiency (ϵ → 1) to eliminate the need for modeling the liquid layer around the probe, as explained in Section 6.3; (c) recognizing that flight systems will be fast moving with a narrow aspect ratio (L/R τ = vR/α  0  → ∞ ), as explained in Section 7; and (d) approximating the thermal diffusivity of ice (α) as a constant.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: (a) CryoB/CryoC and (b) WarmA probe model schematics in a moving reference frame. Inputs are the geometry, T ∞, v, and the local gravity  g , yielding the numerical solution for the heat fluxes q. Probe dimensions not to scale.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: The total efficiency is determined using both experimental results and the Water+Ice models, with agreement demonstrated between the two. For clarity, the small errors along the η  E  axis are not shown. The gap in data from η = 0.15 to 0.45 is due to the choice to test at two well-separated temperatures.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: Data points show the experimentally measured power ﹩{\dot{Q}}_{{E}}﹩ vs. descent speed v for (a) warm ice tests at 253 K and (b) cryogenic tests at 78 K. In the case of the cryogenic results, experimental error alone is insufficient to reconcile deviations from the Q–v trend predicted by the analytic models Aamot and Aamot+ or the 2D-IceOnly numerical model.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: The CryoB/CryoC probe and experiment setup. (a) Section view of the probe, indicating its internal components and main dimensions. (b) View of the interior of the Europa Tower showing the ice surface at the beginning of the second of the CryoC runs. Note the visual confirmation of hole closure on the bottom left of the picture, where CryoC1 descended through the ice.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: An example piezoelectric transducer pulse, echoing off the ice–water interface and returning to the probe. The two-way travel time of 3.6 μs is equivalent to a water gap size of 2.7 mm. For the preliminary test of this sensing system, no effort was made to optimize the noise of the transmission pulse, which can likely be made significantly cleaner.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: Hole closure confirmation for experiment CryoB3: the vertical line shows the moment of full hole closure according to the chamber pressure, vehicle velocity, and trailing temperature data. The hole closure is also visually confirmed, as can be seen in the pictures on the right, showing the probe before the start of the test and after hole closure.
Paper: Experimental Validation of Cryobot Thermal Models for the Exploration of Ocean Worlds
Authors: Paula do Vale Pereira, Michael J. Durka, Bartholomew P. Hogan, Kristof Richmond, Miles W. E. Smith, Dale P. Winebrenner, W. Timothy Elam, Benjamin J. Hockman, Alberto Lopez, Neal Tanner, Joshua Moor, James Ralston, Miriam Alexander, Wayne Zimmerman, Nolan Flannery, William Kuhl, Sarah Wielgosz, Kerri L. Cahoy, Thomas A. Cwik, William C. Stone
Figure caption: An attempt to measure the size of the melt cavity left behind the probes in experiments CryoC1, CryoC2, and CryoC3. (a) An example from the image set acquired in the process, with the 46 mm diameter scale shown. (b) A 60 cm section of the reconstructed solid model of the colored ice for each of the CryoC probes.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: (a) Frame of standard (ST) coordinates. The substellar point is located at latitude/longitude ﹩\left(\phi ,\lambda \right)=\left(0^\circ ,180^\circ \right)﹩. The three black arrows are the unit vectors of the local Cartesian coordinates ﹩(\hat{{{\boldsymbol{e}}}_{{\boldsymbol{i}}}},{\hat{{\boldsymbol{e}}}}_{{\boldsymbol{j}}},\hat{{{\boldsymbol{e}}}_{{\boldsymbol{k}}}})﹩. The red vector is the rotational angular velocity, and its projections onto the local axes are shown in the top right corner. (b) Frame of tidally locked (TL) coordinates. The substellar point is located at tidally locked latitude ϕ TL = 90°. The projections of the rotational angular velocity are shown in the top right corner, the solid line represents the terminator, and the dots represent the substellar points. The frames of the tidally locked latitude and longitude lines are shown in the bottom right corner. (c) Annual mean surface temperature (contours) and near-surface winds (vectors) on Earth. (d) Same as panel (c) but on a tidally locked terrestrial planet with an orbital period of 60 Earth days. (e) Same as panel (d) but shown in the tidally locked coordinates. Here SP and AP are the substellar and antistellar point, respectively.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: (a) Framework of the LEC on Earth. Boxes represent the energy reservoirs, and arrows represent generation (G), transformation (C), and dissipation (D) of energy. (b) Generation of P M. Uneven heating and cooling tilt the zonal mean isotherms (black curves) departed from the global mean isotherms (gray dashed lines), which generates P M. (c) Heat transport by baroclinic eddies, converting P M to P E. The zonal mean isotherm (gray dashed line) is warped to the isotherm (black curve) by baroclinic eddies, which decreases the zonal mean meridional difference, i.e., P M, but leads to zonal variance, i.e., P E. (d) Cross-isobaric motions, converting potential energy and kinetic energy to each other. (e) Wave–mean flow interactions, converting K E and K M to each other. Under a positive β-plane, arbitrary waves with group velocity directed away from the source region in the y-direction (c  gy ) can transport momentum back, along with conversion from K E to K M. Shear instabilities of zonal jets generate eddies, along with conversion from K M to K E.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Climatic elements on three planets. (a)–(c) Temporal and zonal mean temperature (colored shading) and zonal mean zonal winds (contour lines) on Earth; the rapidly rotating, tidally locked terrestrial planet; and the slowly rotating, tidally locked terrestrial planet. (d)–(f) Same as panels (a)–(c) but for deviations of temporal and zonal mean geopotential height from the global means (colored shading) and mass stream functions (contour lines, in units of 1010 kg s−1). Note that the ranges of the color bars in panels (d)–(f) are different. Panels (a), (b), (d), and (e) are shown in the standard coordinates, and (c) and (f) are shown in the tidally locked coordinates. Here SP and AP are the substellar and antistellar point, respectively.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Latitude–altitude cross sections of the LEC on Earth. (a)–(d) Mean potential energy (P M), eddy potential energy (P E), mean kinetic energy (K M), and eddy kinetic energy (K E), respectively; (e)–(h) conversion rates of mean potential energy to eddy potential energy, eddy potential energy to eddy kinetic energy, eddy kinetic energy to mean kinetic energy, and mean potential energy to mean kinetic energy, respectively. The global mean vertical integrals of each panel are the corresponding values in Figure 6. Panels are shown in the standard coordinates. The range of the color bar in panel (a) is different from those in panels (b)–(d).
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Deviations of temporal mean temperature from the global means at 500 hPa on (a) Earth; (b) one rapidly rotating, tidally locked terrestrial planet; and (c) one slowly rotating, tidally locked terrestrial planet. The temporal and global mean temperatures are shown in the top of each panel. The black dots represent substellar points.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Global mean vertical integrals of the energy components (in boxes) and conversion rates (close to arrows) on Earth. Units are 105 J m−2 for energy and W m−2 for conversion rates. Arrows without specific values represent generation and dissipation rates, same as those in Figure 1(a). The directions of the arrows represent the directions of energy conversion, and the main conversion paths are shown in blue. Values are calculated in the standard coordinates.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Same as Figure 7, but for the rapidly rotating, tidally locked terrestrial planet. Panels are shown in the standard coordinates. The maximum in panel (a) is about 600 × 105 J m−2 bar−1, the maximum in panel (h) is about 40 W m−2 bar−1, and the minimum is about −30 W m−2 bar−1.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Same as Figure 6, but for the rapidly rotating, tidally locked terrestrial planet. Values are calculated in the standard (a) and tidally locked (b) coordinates.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Longitude–altitude cross sections of eddy (a) meridional velocity, (b) temperature, and (c) geopotential height at 70°N on the rapidly rotating, tidally locked terrestrial planet. Panels are instantaneous quantities departed from their zonal means.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: A hypothetical uniform zonal mean zonal jet in the standard coordinates (a) is transformed into the winds in the tidally locked coordinates (b) using Equations (1) and (2). Blue dashed lines represent the equator (EQ) in the standard coordinates, red dashed lines represent the terminators (TM), the black dot in panel (a) represents the substellar point (SP), and the black triangle in panel (b) represents the north pole (NP) in the standard coordinates.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Same as Figure 6, but for the slowly rotating, tidally locked terrestrial planet. Values are calculated in the tidally locked (a) and standard (b) coordinates.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Same as Figure 7, but for the slowly rotating, tidally locked terrestrial planet. Panels are shown in the tidally locked coordinates. Here SP and AP are the substellar and antistellar point, respectively. The maximum in panel (a) is about 70 × 105 J m−2 bar−1, the maximum in panel (c) is about 70 × 105 J m−2 bar−1, and the maximum in panel (h) is about 150 W m−2 bar−1.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Climatic elements on the rapidly rotating, tidally locked planet in the standard (left column) and tidally locked (right column) coordinates. Top row: surface temperature (contours) and the near-surface winds (vectors). Middle row: air temperature (contours) and winds (vectors) at 500 hPa. Bottom row: deviations of geopotential height from the global means (contours) and winds (vectors) at 200 hPa. The black dot represents the substellar point, and the black triangle represents the north pole in the standard coordinates.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Same as Figure 7, but for the slowly rotating, tidally locked terrestrial planet. Panels are shown in the standard coordinates.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Same as Figure 7, but for the rapidly rotating, tidally locked terrestrial planet. Panels are shown in the tidally locked coordinates.
Paper: Lorenz Energy Cycle: Another Way to Understand the Atmospheric Circulation on Tidally Locked Terrestrial Planets
Authors: Shuang Wang, Jun Yang
Figure caption: Decomposition of temperatures and winds on the slowly rotating, tidally locked terrestrial planet in the standard coordinates. (a) Meridional contrast of zonal mean surface temperature, (b) eddy surface temperature, (c) zonal mean zonal and meridional winds at 300 hPa, (d) eddy winds at 300 hPa.
Paper: A Long-lived Lunar Magnetic Field Powered by Convection in the Core and a Basal Magma Ocean
Authors: Saira S. Hamid, Joseph G. O'Rourke, Krista M. Soderlund
Figure caption: (a) Surface field intensities of the nominal core model where core convection is driven by inner core growth relatively late in the Moon’s history. The BF, ML, CIA, and MAC scaling laws are used to estimate the surface field intensities of the dipole component. Surface field intensities are compared to the nominal BMO magnetic field intensity assuming the ML scaling law. (b) The dissipation budget of the nominal core model includes the entropy sink associated with thermal conductivity Φ K ; the dissipation associated with secular cooling Φ S , latent heat Φ L , gravitational energy Φ G , and radiogenic heating Φ R ; and the dissipation available for a dynamo ΦCMB. (c) If k  C  is lowered to 30 W m−1 K−1, purely thermal convection occurs intermittently between ∼0.7 and 2 Gyr. Those resultant surface fields are several times weaker than the BMO-hosted field. (d) Dissipation budget associated with a lower kC  of 30 W m−1 K−1.
Paper: A Long-lived Lunar Magnetic Field Powered by Convection in the Core and a Basal Magma Ocean
Authors: Saira S. Hamid, Joseph G. O'Rourke, Krista M. Soderlund
Figure caption: Results of the nominal core model with k  c  = 40 W m−1 K−1, Q  C  = 0 GW, [S] = 7.5 wt%, and [K] = 25 ppm coupled to the nominal BMO model (V19K50p54). All models began at 4.2 billion yr before the present day. (a) Temperature at the CMB, at the center of the core, or near the inner core boundary (ICB) and the average temperature of the core. (b) Inner core radius with respect to time. (c) Sulfur abundance in the outer core with respect to time. (d) Heat budget given by latent heat, Q  L ; radiogenic heating, Q  R ; gravitational energy, Q  G ; adiabatic heat flow in the core, Q AD; heat flow across the CMB, Q CMB; and secular cooling, Q  S .
Paper: A Long-lived Lunar Magnetic Field Powered by Convection in the Core and a Basal Magma Ocean
Authors: Saira S. Hamid, Joseph G. O'Rourke, Krista M. Soderlund
Figure caption: We study three stages in the coupled evolution of the lunar BMO and core. (Left) Convection in the BMO with the potential to produce an early, high-intensity dynamo ∼4.25–3.56 Gyr ago, while the core was fully liquid. Dashed arrows indicate that in limited scenarios, thermal convection in the core may have occurred in tandem with the BMO-hosted dynamo. (Middle) Compositional convection in the core produced a late, low-intensity dynamo until ∼1.9–0.8 Gyr ago once the inner core started growing and the BMO began to solidify. (Right) The internal field ceased ∼1 Gyr ago; once the BMO solidified sufficiently, the inner core grew too large, and convection ceased in the liquid outer core.
Paper: The State of CO and CO2 Ices in the Kuiper Belt as Seen by JWST
Authors: Michael E. Brown, Wesley C. Fraser
Figure caption: A small portion of the spectrum of 2005 RN43 showing both the 13CO2 line, which we use as a wavelength reference, and the CO line. The wavelength of the CO does not match that of CO clathrate hydrates or CO trapped in amorphous ice, but is a close match to pure CO (which is unstable at this temperature), and also to CO trapped in CO2 ice.