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Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: Predictions from models I and A for the mass fractions of heavy elements, Z, and helium, Y/(X + Y), are shown as a function of equatorial radius. Instead of a compact core of Z ≈ 1, our models include a dilute core that reaches to 63% of the planet's radius (R = 0.63). In its inner part, the composition is uniform, with Z values ranging from 0.16 to 0.19. This inner region is surrounded by a stably stratified layer where Z gradually decreases until it reaches a constant, approximately solar value for R ≥ 0.63. The lower panel shows the helium distribution of our models that are constrained to match measurements of the Galileo entry probe near R = 1 and, on average, to agree with the protosolar helium abundance.
Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: Temperature and density profiles of model A. The vertical dotted lines mark the boundaries of the helium rain region. The dashed lines show the boundaries of the transition layer. The bottom panel shows the density deviation from a protosolar adiabat (Y = 0.2735 and Z = 0.0153; Lodders 2010) for T 1bar = 166.1  K. Because of the helium sequestration, the density of model A is lower in the molecular and helium rain layers. Conversely, in the dilute core and the core transition layer, the density of model A is much higher because of the enrichment in heavy elements. In the metallic hydrogen layer, the density of model A is slightly higher than that of the protosolar adiabat because of the enrichment in helium.
Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: Model predictions for the amount of heavy elements in the molecular envelope, Z 1, if we introduce a density correction, Δρ/ρ, for all pressures P ≥ P  c  to the EOS in our A-type models and then reoptimize them to the match the Juno measurements. The blue curves represent the results from simple reoptimizations that only match the planet's mass and J 2. The red curves were obtained by matching the mass and all gravity coefficients, which led us conclude that a density correction only in the metallic region for P ≥ 200 GPa does not significantly affect Z 1. Instead, Z 1 was found to be sensitive to a density reduction in the pressure interval from 10 to 200 GPa.
Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: If one assumes a superadiabatic temperature gradient (circles) in the stably stratified transition layer (0.41–0.63 R J), one can construct interior models that accommodate a larger amount of heavy elements (Y-axis) than in model A (diamond) because the temperature in the core region is higher. We represent this temperature change by plotting against the temperature in the planet's center (X-axis).
Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: Wind speeds as a function of latitude observed in Jupiter's atmosphere (Tollefson et al. 2017). We assume they decay with depth and incorporate them into our thermal wind calculations. In our thermal wind approach (i), this wind profile is adopted without modification, but the wind depth depends on latitude. The gray profiles in the lower panel show an ensemble of wind depth profiles for I-type interior models. The red curve shows the wind depth profiles for our preferred interior model A. In our thermal wind approach (ii), the reconstructed cloud-level wind profiles (yellow region in upper panel) are permitted to deviate from the observations, while the wind decay function is latitude-independent. The dashed orange curve shows the wind solution for the preferred interior model A.
Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: (a) Observed cloud-level wind (black) and the range of model solutions (red shaded area) developed with thermal wind approach (ii). (b)–(e) Corresponding model solutions for the even gravity harmonics. Shown are the measurements (black crosses, with the size of the cross representing the measurement uncertainty), the interior model solutions (blue dots), and the model solutions when the wind-induced gravity harmonics are added to the interior model solutions (red dots). The insets show the zoom-in on the measured values.
Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: The density modification and corresponding correction to J 4 is shown as a function of equatorial spheroid radius λ  i .
Paper: Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core
Authors: Burkhard Militzer, William B. Hubbard, Sean Wahl, Jonathan I. Lunine, Eli Galanti, Yohai Kaspi, Yamila Miguel, Tristan Guillot, Kimberly M. Moore, Marzia Parisi, John E. P. Connerney, Ravid Helled, Hao Cao, Christopher Mankovich, David J. Stevenson, Ryan S. Park, Mike Wong, Sushil K. Atreya, John Anderson, Scott J. Bolton
Figure caption: Inner and outer radii of the core transition layer derived from ensembles of type A models (left panel). The probability densities in the two other panels are normalized so that the integrals under the curves equal 1. For the outer and inner radii, we derived values of 0.63 ± 0.01 and 0.41 ± 0.03, respectively. The uncertainty intervals were chosen so that approximately 80% of all models are represented.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: Distribution of gri-slope vs. perihelion distance of low-q asteroids. The dashed line and shaded region show the trend for S- and Q-type NEAs using data in Binzel et al. (2004) and Lazzarin et al. (2004, 2005) and the uncertainty at a 95% confidence level according to Graves et al. (2019). Our data are consistent with Graves et al. (2019) at the 1σ level.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: Distribution of rotational periods vs. diameter of low-q asteroids (red) compared to the general asteroid population from the JPL Small-Body Database (black). The critical spin limit of 2.2 hr can be seen for asteroids with diameters greater than 200 m.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: Rotational light curve of 2000 BD19 using data from 2020 January using Lowell Observatory’s 31-inch telescope. The light curve is phased to the best-fit period of 10.57 hr determined by Warner (2015a). We were unable to constrain the rotational period further.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: Rotational light curve of 2002 AJ129 using data from 2018 February using Lowell Observatory’s 31-inch telescope. The light curve is phased to the best-fit period of 3.918 hr.
Paper: Surface Properties of Near-Sun Asteroids
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Quanzhi Ye, 泉 志 叶, Henry H. Hsieh, Colin Snodgrass, Alan Fitzsimmons, Derek C. Richardson, Jessica M. Sunshine, Nora L. Eisner, Annika Gustaffson
Figure caption: Rotational light curve of 2006 HY51 using data from 2019 March using Lowell Observatory’s 42 inch telescope. The light curve is phased to the best-fit period of 3.350 ± 0.008 hr.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: A color map that shows the constrained core size within the possible porosity ranges. The black dotted lines define the minimum core size possible to be exposed at Panthia (left) and Eros (right) via an impact cratering process. In the determined porosity range, there are some cases in the lower right corner where the porosity of the core is set to be higher than that of the overlying silicate layer. We address that this condition may not be realistic, although the composition discontinuity between the core and silicate layer may allow that porosities in the core and silicate layer are not mutually related.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: An inverse problem algorithm to constrain the structure layout using the three-layer model and FEM technique. Currently, the bulk density and mass of Psyche have large uncertainties, although there is some supporting evidence inferring those parameters. Given this issue, we decided to fix the bulk density as 4.0 g cm−3, which is the best-matched parameter from the earlier studies, in the three-layer model. This value is estimated by Shepard et al. (2021), given that the nominal mass is 22.87 × 1018 kg, which is driven by Baer & Chesley (2017) and Elkins-Tanton et al. (2020). The matched case is defined before the final stage when the discrepancy between the boundary line and the compressed layer from the initial structure layout is less than 0.01 km.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: Correlation between a radius of the core (R  c ) and the compressed layer (R  m1). The blue line represents a core radius depending on the compressed layer radius. The left dotted line (C1) is a boundary where the core radius is identical to the compressed layer. The upper horizontal line (C2) shows the minimum dimension (∼88.5 km) along the shortest principal axis, while the right dotted line (C3) means the maximum dimension (∼140 km) along the longest principal axis. The white area includes possible sets of (R  c , R  m1).
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: A color map that shows the silicate-rich layer thickness: (a) the minimum thickness placed at the polar region, and (b) the maximum thickness located at the equatorial region.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: Comparison of color maps that shows the silicate-rich layer thickness between the crushing limit of 5 and 15 MPa: (a) the minimum thickness at 5 MPa, (b) the maximum thickness at 5 MPa, (c) the minimum thickness at 15 MPa, and (d) the maximum thickness at 15 MPa. As mentioned in Figure 8(b), the 15 MPa provides a noncolored area that represents that the simulation is not converged. Thus, the white area here also represents the case having no solution for the interior layout.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: Comparison of color maps between the crushing limit of (a) 5 MPa and (b) 15 MPa. In most cases where the core exceeds a certain size (∼80 km), the 15 MPa provides a noncolored area that represents that the simulation is not converged. We interpret this area as when the pressure in the silicate layer does not approach the defined crushing limit, and thus no solution for the interior layout exists.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: Three-layer model layout. Definitions of all symbols in the figure are described in Table 1.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: Structure layout (a) at the initial stage and (b) at the final stage. Figure (b) show a unique case when the boundary line matches the crushing limit. Here, the crushing limit is set as 10 MPa. This case represents when the porosity of the iron core and the top surface is 0% and 50%, respectively, given e = 30%.
Paper: A Numerical Approach Using a Finite Element Model to Constrain the Possible Interior Layout of (16) Psyche
Authors: Yaeji Kim, Masatoshi Hirabayashi
Figure caption: Elastic stress fields of Eros derived by a semianalytical model (Nakano & Hirabayashi 2020).
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Observed C/O ratio of an interstellar comet as a function of the measured production rates of CO and CO2 relative to H2O. The solid line indicates the region where the observed C/O ratio is 0.5. Since processing preferentially removes CO and CO2 relative to H2O, comets to the right of this line formed exterior to the CO snow line. The dashed line indicates where the primordial C/O ratio is 0.5, using the transformation presented in Figure 13. Objects to the left of this line formed interior to the CO snow line. Objects in between both of these lines could have formed exterior to the CO snow line with primordial C/O ratios greater than 0.5, with their observed C/O ratios altered due to processing. The location of Borisov is indicated with a dotted line, implying that it formed exterior to the CO snow line.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Cumulative distribution functions for impact parameter and hyperbolic excess velocity for interstellar objects that will be detected by the LSST from Figures 12 and 15 in Hoover et al. (2022). These are calculated using a detailed population synthesis assuming that the interstellar objects were as bright as ’Oumuamua.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Relative erosion of an interstellar comet in the solar system and ISM. We show the change in radius of the comet in the solar system divided by the change in radius in the ISM, calculated for a range of impact parameters and hyperbolic velocities using Equation (13). The ratio for objects the age of 1I/‘Oumuamua and 2I/Borisov are shown in red and blue contours. The locations of these two detected interstellar objects are indicated.
Paper: The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets
Authors: Darryl Z. Seligman, Leslie A. Rogers, Samuel H. C. Cabot, John W. Noonan, Theodore Kareta, Kathleen E. Mandt, Fred Ciesla, Adam McKay, Adina D. Feinstein, W. Garrett Levine, Jacob L. Bean, Thomas Nordlander, Mark R. Krumholz, Megan Mansfield, Devin J. Hoover, Eric Van Clepper
Figure caption: Transformation from the observed to primordial C/O ratio of an interstellar comet. The ratio is calculated by evaluating Equations (14) and (17) for a range of production rate ratios. Processing decreases the observed C/O ratio due to preferential desorption of CO and CO2 relative to H2O.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Variations of the degree 2 zonal and sectorial gravity field harmonics due to the atmospheric mass redistribution during a Martian year. The spherical harmonics coefficients are 4π normalized.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Temporal variations of the Venus geoid induced by the atmosphere over shaded topographic relief at four different times. The maps are centered at 180° longitude. The subsolar point (red dot) is located at longitude (a) 0°, (b) 90°, (c) 180°, and (d) 270°. The visible sectorial pattern is produced by the thermal tides and rotates in phase with the subsolar point.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Load Love numbers of Venus up to degree 20 for different interior models. The core is assumed to be entirely fluid in panels (a) and (b) and entirely solid in panels (c) and (d). Models in panels (a) and (c) are characterized by low mantle viscosity (1019 Pa s), and a higher value (1022 Pa s) is selected for panels (b) and (d).
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Degree 2 load Love number of Venus’s dependence on the frequency of the loading by assuming different rheology models. The dotted line represents the period of the thermal tides responsible for the loading deformations on Venus.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Degree 2 load Love number of Venus for models with a fluid inviscid core and varying core size and mantle viscosity. Crosses represent models for which the computed k 2 is not in agreement with the observations. Gray dots represent models with an elastic mantle.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Time variations of the degree 2 zonal and sectorial gravity field harmonics due to the atmospheric mass redistribution during a Venus solar day. The spherical harmonics coefficients are 4π normalized.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Degree 2 load Love number of Venus for models with a solid core and varying core size and viscosity.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Degree 2 tidal and load Love numbers of Venus for all of the accepted models. The models are color-coded according to the viscosity of the mantle.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Degree 2 tidal and load Love numbers of Mars for all of the accepted models. The models are color-coded according to the viscosity of the mantle.
Paper: Constraining the Internal Structures of Venus and Mars from the Gravity Response to Atmospheric Loading
Authors: Flavio Petricca, Antonio Genova, Sander Goossens, Luciano Iess, Giorgio Spada
Figure caption: Load Love numbers of Mars up to degree 20 for different values of (a) mantle viscosity and (b) core radius.
Paper: Did Earth Eat Its Leftovers? Impact Ejecta as a Component of the Late Veneer
Authors: Philip J. Carter, Sarah T. Stewart
Figure caption: Number of embryos (M ≥ 0.01 M ⊕; top), number of planetesimals (M < 0.01 M ⊕; middle), and fraction of nearby planetesimals (bottom) with correlation coefficients of 0.5 or above for each embryo in several simulations. The number of similar bodies is shown as a function of semimajor axis (left) and mass of the relevant embryo (right). Purple points are for Grand Tack simulations, and orange points are for calm accretion simulations. The fraction of planetesimals that are similar to each embryo is calculated only for planetesimals with semimajor axes within 0.2 au of the embryo, as indicated by the black horizontal bar in the bottom left panel. The sizes of the points are scaled to the mass of the embryos. Embryos from low-resolution simulations are excluded from the planetesimal (bottom) panels.