adsabs/AstroCLIMB huggingface dataset:
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Mass spectrum of the pure steel sample holder starting at m/z = 5. The inset shows a zoom from m/z = 50 to 390. Typical steel peaks in the relevant mass range are indicated in the spectra. The spectrum was measured at 3 μJ.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Mass spectra of the blank steel sample holder (a) and heptane deposited on the blank steel sample holder (b), measured at laser pulse energies in the range of 1–4 μJ. Contamination from pyrene and perylene is visible, as a mixture of these two was measured in the adjacent cavities; see Figure 17. No obvious heptane peaks or derivatives could be distinguished in the comparison of the two spectra.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Measurement of 100 μM anthracene at laser pulse energies in the range of 1–4 μJ. The parent peak is indicated in gray.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Mass spectra of 100 μM coronene measured at laser pulse energies in the range of 1–4 μJ. The parent peak is indicated at m/z = 300, as is the peak at m/z = 276.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Mass spectra of 100 μM perylene measured at laser pulse energies in the range of 1–4 μJ. The parent peak is indicated.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Overview of the four PAHs investigated in this campaign measured at a laser pulse energy of 1 μJ and a concentration of 100 μM. The spectra were normalized to the highest peak for the respective PAH.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Mass spectra of anthracene at concentrations in the range from 1 to 1000 μM. The sample was measured at a laser pulse energy of 3 μJ.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Two PAH mixtures measured with ORIGIN. (a) Perylene and pyrene mixed together with concentrations of 50 μM each. (b) Four-way mixture of all PAHs used in this study. The PAHs mixed together had a concentration of 25 μM each.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Ratio of the peak area of an m + 1 mass peak to the peak area with mass m for perylene (abbreviated as Per) and pyrene (Pyr) for the 40 individual positions. The concentration of the investigated sample is shown in the top right corner. The expected 13C ratio (red dotted line) was plotted against the mean of the 40 positions (solid black line) and the standard deviation from the mean (dashed gray lines).
Paper: Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment
Authors: Michelle R. Kirchoff, Luke Dones, Kelsi Singer, and Paul Schenk
Figure caption: New mosaics of Uranus’ large satellites in order of distance from Uranus constructed using improved processing techniques of Voyager 2 Imaging Science Subsystem images (see text). Best pixel scale for each satellite, typically occurring near ∼0° longitude and ∼25°–30°S latitude, is 0.26 km for Miranda, 1.3 km for Ariel, 5.1 km for Umbriel, 3.1 km for Titania, and 6.6 km for Oberon. Resolution degrades away from these areas due to the increased distance of Voyager 2 from the satellites during the flyby and image distortions. Areas in black could not be imaged due to the Uranus system being in summer solstice and flyby geometry.
Paper: Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment
Authors: Michelle R. Kirchoff, Luke Dones, Kelsi Singer, and Paul Schenk
Figure caption: Left column shows defined measurement areas indicated by black outlines, terrain boundaries indicated by light gray outlines (Miranda, Ariel, and Titania only), and crater measurements indicated by white circles. The completeness limit crater diameters measured and examined for each are 1.3–1.7 km for Miranda, 6.3 km for Ariel, 25.4 km for Umbriel, 15.5–17.5 km for Titania, and 33.0 km for Oberon (∼5 pixels across). Right column shows crater spatial density maps used in part to define terrain boundaries. Red indicates high crater density, while blue indicates low density. Approximate minimum and maximum densities per 106 km2 for each map (from top to bottom) are 900–8600, 180–1300, 120–350, 40–300, and 50–250. Satellites are vertically organized by distance from Uranus. Stars and diamonds indicate locations of lower crater density due to particular circumstances as described in the text.
Paper: Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment
Authors: Michelle R. Kirchoff, Luke Dones, Kelsi Singer, and Paul Schenk
Figure caption: Relative (R) crater SFD plots for all regions studied on the mid-sized Uranian satellites. Lines denote the kernel density estimator representation of the crater size–frequency distribution (SFD) and shaded regions their associated bootstrap uncertainties. R values are computed by normalizing the differential crater densities to an SFD with a −3 slope. Larger R values indicate higher spatial densities.
Paper: Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment
Authors: Michelle R. Kirchoff, Luke Dones, Kelsi Singer, and Paul Schenk
Figure caption: Comparison of crater size–frequency distributions (SFDs) from this work (lines and shaded areas) to previous work by the Strom group (blue circles) and Plescia group (brown squares) for relevant regions (see text for citations defining the groups). R values are computed by normalizing the differential crater densities to an SFD with a −3 slope. Larger R values indicate higher spatial densities.
Paper: Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment
Authors: Michelle R. Kirchoff, Luke Dones, Kelsi Singer, and Paul Schenk
Figure caption: Scaled crater SFDs for the Uranian satellites from this work and Triton from Schenk & Zahnle (2007) (top row), Saturnian satellites from Kirchoff et al. (2018) (bottom right), and Jovian satellites from Singer et al. (2019) (bottom left). These are scaled and compared to crater SFDs from cratered terrains on Charon (Singer et al. 2019). Upper-left plot shows Uranian satellites that match well to Charon, while the upper-right plot shows Uranian satellites and Triton that do not match well. R values are computed by normalizing the differential crater densities to an SFD with a –3 slope. Larger R values indicate higher spatial densities.
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Knowledge of Ceres’ astrobiological potential framed in the context of the ROW based on Dawn’s results. “Solid foundation” refers to direct observational constraints, while “key information” refers to indirect observational inferences and theoretical models. A future in situ mission or sample return would significantly progress along the roadmap. (Adapted from Hendrix et al. 2019 and based on an analysis by Castillo-Rogez 2020.)
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Geophysical context for the geological site investigated by this study. Medium-resolution imaging, compositional, and gravity data of the floor of Occator crater by the Dawn mission revealed the presence of a deep brine region that provides a long-lived source for evaporites found in Vinalia Faculae (Raymond et al. 2020; Scully et al. 2020; Nathues et al. 2020). A region of particular interest for a future sample return mission is Vinalia Faculae, located on the eastern part of the crater floor (see Section 3.4 for a detailed description of that region).
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: The characterization of Ceres’ deep brine environment is addressed via a combination of elemental and mineralogical measurements and mapping of phase relationships. Possible techniques (among many others) are presented here: Fourier transform infrared (FTIR) spectroscopy and X-ray diffraction (XRD) for bulk identification of mineralogy; instrumental neutron activation analysis (INAA) for bulk elemental chemistry, followed by inductively coupled plasma MS (ICP-MS) for a more complete set of elements; electron microbe wavelength dispersive spectroscopy analyses (EMPA WDS for chemistry) and fast ion beam–transmission electron microscopy (FIB-TEM for crystal structure/mineral identification) for detailed phase relationships; and secondary-ion MS (SIMS) for isotopic measurements on, e.g., carbonate oxygen. Numbers refer to testable hypotheses mentioned in the text. Left: Ceres cutaway produced by Raoul Ranoa. Top middle, NASA/JPL Caltech/UCLA/MPS/DLR/IDA; center middle, Altair et al. (2018); bottom middle: numerical modeling by Mohit Melwani Daswani (JPL).
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Characterization of organic matter that has been sitting in long-lived brines is addressed by a combination of elemental measurement; SOM and insoluble organic matter (IOM) characterization and relationships to minerals; and the isotopic composition of C, H, O, and N.; Raman spectroscopy to identify functional groups; nano-SIMS for spatial distribution of C, H, O, and N isotopes and relationship to mineral grains; transmission electron microscopy (TEM) for fine-scale (∼tens of nanometers) mineral-organic spatial relationships and mineral identification; C, N, and O X-ray absorption near edge structure (XANES)  for identification of organic functional groups and “bulk” O/C and N/C at fine scales; laser desorption laser ionization MS (L2MS) for identification of individual compounds; ultraperformance liquid chromatography fluorescence detection and quadrupole time-of-flight hybrid MS (UPLC-FD/QToF-MS) for amino acids; for IOM isotopes, demineralization followed by elemental analyzer (EA) GC-MS (C+N) and thermal conversion EA-GC-MS; for compound-specific isotopic composition of soluble organics, GC combustion isotope ratio MS (GC/C/IRMS) or picomolar-scale compound-specific isotope analyses (pico-CSIA). Figures: Chan et al. (2018).
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Hypotheses on the origin of Ceres can be tested by combining elemental ratios of light and heavy isotopes, such as bulk  ϵ50 Ti and ϵ54 Cr via multiple collection ICP-MS, bulk oxygen isotopic ratios (including calculation of Δ17O) with infrared laser-assisted fluorination coupled with dual-inlet MS, secondary-ion MS (SIMS) for O isotopic composition of specific silicate or carbonate grains, and nano-SIMS for in situ analysis of, e.g., H, N, and O isotopic distribution. Based on Meech & Raymond (2020).
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Five regions of high scientific value considered in this study. The PMCS science team concluded that Occator crater’s evaporites offer the greatest opportunity to progress along the ROW.
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Performance comparison between in situ measurement and Earth’s laboratory measurement techniques against measurement requirements (blue circles and lines). The requirement to measure 17O/16O and determine the nature of the organic compounds believed to be highly diluted drives the need for high-grade facilities. Initial isotopic ratios depend on the mineral in which the reference element is incorporated (e.g., Willacy & Woods 2009 for D/H). Although high-precision D/H can be measured in water with in situ payload, material ingestion techniques cannot separate minerals, resulting in a signal that is diluted and difficult or even impossible to interpret reliably. Based on Milam et al. (2021).
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Two landing regions identified as being of high value for the in situ concept: Homowo Regio (Occator crater northeastern ejecta) followed by Vinalia Faculae. The two regions are separated by about 40 km.
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Returned sample processing flowchart. Source: Curation and Analysis Planning Team for Extra-Terrestrial Material (CAPTEM), now the Extraterrestrial Materials Analysis Group (ExMAG). See NASEM (2019).
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Example trajectory for the outbound and return cruise phases for a 2030 launch. With SEP, sample return missions can be launched in any year from 2030 through 2037 with little change in performance. For example, a 2033 launch decreases the total flight time from 12.8 to 12.6 yr and increases the Earth arrival mass from 2264 to 2269 kg. A Mars gravity assist flyby and stay time of 500 days at Ceres are included in all cases.
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: The SEP lander spacecraft in the cruise configuration (top) and the landed configuration (bottom). In the cruise configuration, the solar arrays are articulated about the y-axis to track the Sun during thrusting with the electric propulsion system. A second axis of articulation about the x-axis reduces the risk of the arrays contacting objects on the surface of Ceres in the landed configuration.
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Example PlanetVac-type sampler. Compressed gas is used to lift loose surface material and transport it through a long tube leading to the sample container in the SRC. From Zacny et al. (2019).
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Sample chain elements shown in red.
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Conceptual SRC sample containment system architecture.
Paper: Concepts for the Future Exploration of Dwarf Planet Ceres’ Habitability
Authors: Julie Castillo-Rogez, John Brophy, Kelly Miller, Michael Sori, Jennifer Scully, Lynnae Quick, Robert Grimm, Michael Zolensky, Michael Bland, Debra Buczkowski, Carol Raymond, Amanda Hendrix, Thomas Prettyman, Yasuhito Sekne, Timothy Titus, David Williams, Paul Backes, Laura Barge, Anton Ermakov, Andrew Galassi, Scott Moreland, and Kris Zacny
Figure caption: Examples of 100 m diameter safe landing sites, based on Dawn XM2 imaging.
Paper: Evaluation of Recent Measurements of Mercury’s Moments of Inertia and Tides Using a Comprehensive Markov Chain Monte Carlo Method
Authors: Sander Goossens, Joe P. Renaud, Wade G. Henning, Erwan Mazarico, Stefano Bertone, and Antonio Genova
Figure caption: Results from the MCMC analysis, where we plot the entire polar moment vs. the crust–mantle polar moment (A–D) or the entire polar moment vs. k2 (E–H). We indicate the concentrations of the models with colors. We include ellipses for the measurements (the “target”) as well as for the ensemble average. We use the measurements from Genova et al. (2019), indicated as G19, or Mazarico et al. (2014), indicated as M14. We include k2 in the analysis as a measurement (indicated with “k2 measurement”), or do not include it as a measurement but instead predict it (“k2 predicted”).
Paper: Evaluation of Recent Measurements of Mercury’s Moments of Inertia and Tides Using a Comprehensive Markov Chain Monte Carlo Method
Authors: Sander Goossens, Joe P. Renaud, Wade G. Henning, Erwan Mazarico, Stefano Bertone, and Antonio Genova
Figure caption: Results from the MCMC analysis for the liquid outer core radius (CMB radius), when using different measurements. We include cases where k2 was used as a measurement (the solid lines), and cases where it was predicted (the dotted lines). We now also include measurements from Hauck et al. (2013; H13), and Bertone et al. (2021; B21), with k2 predicted.
Paper: Evaluation of Recent Measurements of Mercury’s Moments of Inertia and Tides Using a Comprehensive Markov Chain Monte Carlo Method
Authors: Sander Goossens, Joe P. Renaud, Wade G. Henning, Erwan Mazarico, Stefano Bertone, and Antonio Genova
Figure caption: The ratio of the radii of the inner core and outer core when using the measurements of Genova et al. (2019), now including k2 as a measurement.
Paper: Evaluation of Recent Measurements of Mercury’s Moments of Inertia and Tides Using a Comprehensive Markov Chain Monte Carlo Method
Authors: Sander Goossens, Joe P. Renaud, Wade G. Henning, Erwan Mazarico, Stefano Bertone, and Antonio Genova
Figure caption: The ratio of the radii of the inner core and outer core vs. the liquid or solid core density. These results are from the MCMC analysis using the measurements of Genova et al. (2019), including k2.