adsabs/AstroCLIMB huggingface dataset:
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Comparisons of observations (points with error bars) and synthetic spectra at 67.°5N, 155°W in the 587 (top panel) and 1248 (middle panel) cm−1 spectral setting, which respectively capture H2 S(1) and CH4 emissions. The a priori (solid black line) and retrieved temperature profiles (solid colored lines) and uncertainty (dotted colored lines) are shown in the bottom panel. Green and red results denote March 17 and 19 results, respectively.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Vertical absolute contribution functions with respect to temperature for a subset of the (a) 587, (b) 730, (c) 819, (d) 950, and (e) 1248 cm−1 settings. The contribution functions have been convolved with the telluric transmission spectrum shown as a white solid line and according to the right-hand axis.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Comparison of observed (points with error bars) and modeled (solid lines) spectra for H2 S(1) (top panel) and CH4 (middle panel) emission at 72.°5S. Red and blue respectively denote results at 32.°5W (a longitude poleward of Jupiter’s southern main auroral oval) and 300°W (equatorward of the MAE). An offset has been added to the red spectra for clarity. The corresponding retrieved profiles of temperature (solid lines) and uncertainty (dotted lines) are shown in the bottom panel. The black solid line denotes the initial guess or a priori profile.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Retrieved temperature distributions on 2017 March 17 (left column) and 19 (right column) at 0.01 (first row), 0.1 (second row), 0.98 (third row), and 4.7 mbar (fourth row). Solid black lines denote the statistical-mean position of the ultraviolet oval (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Distribution of coadded TEXES observations of the H2 S(1) quadrupole (first row), C2H2 (second row), C2H6 (third row), C2H4 (fourth row), and CH4 (fifth row) emission on 2017 March 17 (left column) and 19 (right column). Points are colored by the brightness temperature of an emission line at the indicated wavenumber according to the color bar. The statistical-mean auroral oval position is shown as a solid black line (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Distribution of coadded TEXES observations of the H2 S(1) quadrupole (first panel), C2H2 (second panel), C2H6 (third panel), C2H4 (fourth panel), and CH4 (fifth panel) emission on 2017 March 18. Points are colored by the brightness temperature of an emission line at the indicated wavenumber according to the color bar. The statistical-mean auroral oval position is shown as a solid black line (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Vertical profile of temperature (black) according to the lower axis and vertical profiles of CH4 (pink), 13CH4 (red), CH3D (orange), C2H2 (green), C2H4 (blue), and C2H6 (cyan) according to the upper axis. This is Model 7 from Sinclair et al. (2020), which is based on the photochemical model presented in Moses & Poppe (2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Longitude–pressure cross section of retrieved temperatures at 67.°5N. Results for 2017 March 17 are shown in the top panel and for March 19 in the middle panel. The temperature difference (March 19–March 17) is shown according to the color bar, and line contours mark the 2σ, 3σ, 4σ, 5σ, and 6σ levels to demonstrate where temperature changes are significant with respect to uncertainty. Vertical dashed lines correspond to the longitudinal boundaries of the auroral oval at 67.°5N.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Retrieved temperature distributions on 2017 March 18 at 0.01 (first panel), 0.1 (second panel), 0.98 (third panel), and 4.7 mbar (fourth panel). Solid black lines denote the statistical-mean position of the ultraviolet MAE (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Comparisons of observations (points with error bars) and synthetic spectra at 72.°5N, 162.°5W in the 730 (top panel), 950 (middle panel), and 819 (bottom panel) cm−1 spectral settings, which respectively capture C2H2, C2H4, and C2H6 emissions. Only a subset of the spectral ranges inverted is shown for clarity. The a priori (solid black line) and retrieved profiles (solid colored lines) and uncertainties (dotted colored lines) are shown in the bottom panel. Green and red results denote spectra/results for March 17 and 19, respectively.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Individual TEXES scans of high northern latitudes. Each point represents a spectrum and is colored according to the radiance from 587.0275 to 587.0375 cm−1, which captures the H2 S(1) quadrupole emission feature. Scans are shown in chronological order from left to right and top to bottom. Solid black lines represent the statistical-mean position of the ultraviolet auroral ovals (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Test retrievals of C2H6 at 72.°5S, 17.°5W (top panel) and C2H2 at 72.°5N, 162.°5W (bottom panel). Black denotes the a priori, retrieved profiles are solid colored lines, and uncertainties on the retrieved profiles are dotted colored lines. Purple denotes the profile retrieved when an 18% fractional uncertainty is adopted at all altitudes. The remaining profiles are those retrieved when the a priori uncertainty was decreased to 1% at pressures higher than 3 (blue), 1 (cyan), 0.3 (green), 0.1 (orange), 0.03 (red), and 0.01 mbar (pink). The corresponding reduced χ 2 values are also shown in each plot.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Retrieved abundances of C2H2 (left column), C2H4 (middle column), and C2H6 (right column) at high southern latitudes on 2017 March 17. Results are shown at 0.001 (first row), 0.01 (second row), 0.1 (third row), 0.98 (fourth row), and 4.7 mbar (fifth row). The solid black line denotes the statistical-mean position of the ultraviolet auroral oval (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Longitudinal variations of retrieved C2H2 at 0.01 mbar (top panel), C2H4 at 0.01 mbar (middle panel), and C2H6 at 0.98 mbar (bottom panel) at 72.°5N. Results are shown at altitudes where the observations are more sensitive and thus the longitudinal/temporal variations are strongest. Results for March 17 and 19 are shown in green and red, respectively. Observations at 819 cm−1 on March 17 did not capture 72.°5N, so no C2H6 results are shown for this date. The vertical dotted lines denote the statistical-mean position of the ultraviolet main auroral oval (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Comparisons of observations (points with error bars) and synthetic spectra on 2017 March 18 in the 730 (first panel), 950 (second panel), and 819 (third panel) cm−1 spectral settings, which respectively capture C2H2, C2H4, and C2H6 emissions. The a priori (solid black line) and retrieved profiles (solid colored lines) and uncertainties (dotted colored lines) are shown in the fourth panel. Blue results denote spectra/results for 65°S, 340°W, and red results denote 72.°5S, 17.°5W.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Same as Figure 13 but instead using observations on 2017 March 19.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Same as Figure B1 but for observations of high southern latitudes.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Retrieved abundances of C2H2 (left column), C2H4 (middle column), and C2H6 (right column) at high southern latitudes on 2017 March 18. Results are shown at 0.001 (first row), 0.01 (second row), 0.1 (third row), 0.98 (fourth row), and 4.7 mbar (fifth row). The solid black line denotes the statistical-mean position of the ultraviolet auroral oval (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Example retrievals of temperature and C2H4 at 72.°5N, 165°W (left column) and 162.°5W (right column), where the retrieval places the enhancement of C2H4 with respect to a priori at different altitudes. The first and second rows compare observed and modeled spectra at 587 and 1248 cm−1, respectively, from which the temperature profile is retrieved. The third row compares observed and modeled spectra at 950 cm−1 from which the C2H4 profile is retrieved. The bottom panel shows retrieved profiles (solid red, with dotted red lines showing the 1σ uncertainty) of the temperature, according to the lower axis, and C2H4, according to the upper axis. Solid black lines mark the a priori profiles.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Individual TEXES scans of high northern latitudes. Each point represents a spectrum and is colored according to the mean radiance in all sampled C2H2 emission lines from 729.0 to 730.0 cm−1. Scans are shown in chronological order from left to right and top to bottom. Solid black lines represent the statistical-mean position of the ultraviolet auroral ovals (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Individual TEXES scans of high northern latitudes. Each point represents a spectrum and is colored according to the mean radiance in all sampled C2H4 emission lines from 949.0 to 950.0 cm−1 Scans are shown in chronological order from left to right and top to bottom. Solid black lines represent the statistical-mean position of the ultraviolet auroral ovals (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Individual TEXES scans of high northern latitudes. Each point represents a spectrum and is colored according to the mean radiance in all sampled CH4 emission lines from 1245.20 to 1250.03 cm−1. Scans are shown in chronological order from left to right and top to bottom. Solid black lines represent the statistical-mean position of the ultraviolet auroral ovals (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Same as Figure B9 but for observations of high southern latitudes.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Individual TEXES scans of high northern latitudes. Each point represents a spectrum and is colored according to the mean radiance in all sampled C2H6 emission lines from 819.0 to 820.0 cm−1. Scans are shown in chronological order from left to right and top to bottom. Solid black lines represent the statistical-mean position of the ultraviolet auroral ovals (Bonfond et al. 2017).
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Same as Figure B5 but for observations of high southern latitudes.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Same as Figure B7 but for observations of high southern latitudes.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Same as Figure B3 but for observations of high southern latitudes.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Retrievals of the vertical profile of C2H4 at 72.°5N, 165°W using observations on 2017 March 19. The solid black line represents the initial guess or a priori profile. Solid and dotted lines represent retrieved profiles and uncertainties, respectively. Retrieved profiles are shown where the fractional uncertainty is constant at all altitudes (purple) and where it is reduced to 1% abundances at pressures higher than 3 (blue), 1 (cyan), 0.3 (green), 0.1 (orange), 0.03 (red), and 0.01 mbar (pink). The corresponding reduced χ 2/n values are shown in the legend.
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: Model validation chain. The experimental results of this work (Section 4) provide validation of high-fidelity numerical models (Section 5). The validated numerical models then enable definition of the range of validity for established fast-compute analytic models; this range fortuitously coincides with anticipated operational conditions on Europa and so that these analytic models can be used to support agile mission concept development (Section 7).
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) Experimental setup inside the APL-UW LECS cold room showing the WarmA probe entering a transparent ice column with embedded thermistors and associated measurement electronics, as well as probe guidance and depth measurement hardware; (b) WarmA laboratory-scale melt probe; (c) WarmA during descent in transparent ice, with red dye added into the melt hole to aid visual observation of the melt jacket.
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 Europa Tower, located at Stone Aerospace. (a) External view. (b) Schematic of the tower with primary dimensions. The points represent the location of the thermocouples embedded in the ice. Each cryogenic ice block was used for three experiments, spaced evenly around the central thermocouple string at 120° intervals.
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: Current understanding of Europa’s ice structure, highlighting the difference between brittle, conductive ice close to the surface and warm, convective ice near the ocean. Figure from Howell & Pappalardo (2020).