adsabs/AstroCLIMB huggingface dataset:
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: (a) Zonal mean temperature (T); (b) salinity anomaly (S); and (c) potential density anomaly (ρ  σ , with reference pressure near the ocean surface) in the quasi-equilibrium state of all simulations. The first to fourth columns show the results of the high-salinity simulation with high horizontal diffusivity (HS h ), the high-salinity simulation with low horizontal diffusivity (HS l ), the low-salinity simulation with high horizontal diffusivity (LS h ), and the low-salinity simulation with low horizontal diffusivity (LS l ), respectively. In (a1) and (a2), the contour interval is 0.01 °C below −2.14 °C and 0.001 °C above −2.14 °C. In (a3) and (a4), the contour interval is 0.01 °C below −0.6 °C and 0.2 °C above −0.6 °C. In (b1) and (b2), a reference salinity of 34.97 g kg−1 is subtracted, and the contour interval is 10−3 g kg−1. In (b3) and (b4), a reference salinity of 8.45 g kg−1 is subtracted, and the contour interval is 5 × 10−4 g kg−1. In (c1) and (c2), a reference density of 1029.13 kg m−3 is subtracted, and the contour interval is 10−3 kg m−3 below 5 × 10−3 kg m−3 and 3 × 10−4 kg m−3 above 5 × 10−3 kg m−3. In (c3) and (c4), a reference density of 1007.7 kg m−3 is subtracted, and the contour interval is 10−3 kg m−3 below −10−2 kg m−3 and 5 × 10−3 kg m−3 above −10−2 kg m−3.
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: (a) Zonal mean zonal velocity (u); (b) stream function (Ψ, with clockwise circulation defined as positive); and (c) zonal mean vertical kinetic energy (w 2, in logarithmic scale) in the quasi-equilibrium state of all simulations. The first to fourth columns show the results of the high-salinity simulation with high horizontal diffusivity (HS h ), the high-salinity simulation with low horizontal diffusivity (HS l ), the low-salinity simulation with high horizontal diffusivity (LS h ), and the low-salinity simulation with low horizontal diffusivity (LS l ), respectively. The stream function is calculated as ﹩{\rm{\Psi }}=-{\int }_{0}^{{\lambda }_{x}}{\int }_{{r}_{b}}^{r}{vr}\cos \phi d\lambda {dr}﹩, where λ  x  = 15π/180 is the longitudinal extent of the domain, v is the meridional velocity, λ is longitude, and r is radius. The black dashed lines denote the boundary of the tangent cylinder (a cylinder that is parallel to the rotational axis and is tangent to the bottom core).
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: (a) Prescribed ice topography and (b) corresponding conductive heat loss (blue line) and bottom heating (red line) per unit area, as a function of latitude. The global integral of the bottom heating balances the conductive heat loss. The apparent offset between the blue and red lines in panel (b) is due to the different surface areas at the bottom and ice–ocean interface.
Paper: The Effect of Salinity on Ocean Circulation and Ice–Ocean Interaction on Enceladus
Authors: Yaoxuan Zeng, Malte F. Jansen
Figure caption: Thermal wind balance in the quasi-equilibrium state of all simulations. (a) shows ﹩2\vec{{\rm{\Omega }}}\cdot {\rm{\nabla }}[u]﹩ and (b) shows −∂[b]/r∂ϕ, respectively, where [·] denotes a zonal average. The first to fourth columns show the results of the high-salinity simulation with high horizontal diffusivity (HS h ), the high-salinity simulation with low horizontal diffusivity (HS l ), the low-salinity simulation with high horizontal diffusivity (LS h ), and the low-salinity simulation with low horizontal diffusivity (LS l ), respectively.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: W1 phase slope vs. diameter (km) for Themis-family objects, Flora-family objects, and AKARI objects after removing all NEOWISE observations with S/N ≤ 7.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: W1 phase slopes of Themis-family asteroids vs. their log W1 albedo. The black line represents a five-point running mean.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: Average S/N vs. W1 phase slope for the Themis family (left) and the Flora family (right), colored by diameter. The S/Ns shown here are the average of the W1 observations used to determine the phase curve point for the lowest available phase angle for a given object.
Paper: 3 μm Phase Curves of Main-belt Asteroids from NEOWISE Photometry
Authors: Matthew Varakian, Nancy Chanover, Joseph Masiero, Dagmara Oszkiewicz
Figure caption: Left: W1 phase slope vs. phase angle coverage for Flora-family objects. Right: diameter vs. phase angle coverage for Flora-family objects. The orange line is a linear fit to the data.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: (a) South pole map of the lunar south pole (poleward of 85° S), where high slopes (greater than 10°) are shown in white and low slopes (less than 10°) are shown in gray. Surface roughness maps at (b) 50 m baseline (1 km resolution) and (c) 30–120 m baseline (240 m resolution). Cold traps (T max < 110 K) are outlined in black, and selected ROIs are labeled. Latitude is given by concentric circles at 1° increments. Maps are in polar stereographic projection.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: Frequency distribution of topographic roughness at the lunar south pole (poleward of 85° S) at 50 m baselines (left) and 30–120 m baselines (right) at 1 cm roughness bins for cold traps (top) and surrounding non-cold-trap regions (bottom). High slopes (greater than 10°) are shown in purple, low slopes (less than 10°) are shown in green, and all slopes (no restrictions) are shown in blue.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: QuickMap LROC images of equatorial craters of interest shown in Lambert conformal projection: (a) Morozov F, (b) Rosenberger C, (c) Van Maanen, (d) Fraunhofer E, (e) Brisbane, and (f) Asclepi. Orange circles denote crater rims, and white contours encircle light plains deposits identified in Meyer et al. (2020).
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: QuickMap LROC images of Amundsen shown in stereographic projection. The orange circle denotes the crater rim, and the white contour encircles light plains deposits identified in Meyer et al. (2020). The thin pink contour indicates the PSR.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: Surface roughness map at 50 m baseline (1 km resolution) in equidistant cylindrical projection for six equatorial craters that serve as comparisons with polar ROIs: (a) Morozov F, (b) Rosenberger C, (c) Van Maanen, (d) Fraunhofer E, (e) Brisbane, and (f) Asclepi. ROIs are outlined in black contours.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: 30–120 m baseline (240 m resolution) surface roughness maps of the lunar cold traps of interest and the directly surrounding non-cold-trap regions for (a) Faustini, (b) Shoemaker, (c) Haworth, (d) Nobile, (e) Cabeus, and (f) an unnamed region. Cold-trap areas (T max < 110 K) are outlined in black contours.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: 50 m baseline (1 km resolution) surface roughness maps of the lunar cold traps of interest and the directly surrounding non-cold-trap regions for (a) Faustini, (b) Shoemaker, (c) Haworth, (d) Nobile, (e) Cabeus, and (f) an unnamed region. Cold-trap areas (T max < 110 K) are outlined in black contours.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: Surface roughness ratios for six ROIs and for the average of all south pole cold traps. Roughness ratios below unity (horizontal dashed line) indicate that a cold trap is less rough than its directly surrounding regions.
Paper: Surface Roughness at the Moon’s South Pole: The Influence of Condensed Volatiles on Surface Roughness at the Moon’s South Pole
Authors: Lizeth O. Magaña, Parvathy Prem, Ariel N. Deutsch, Anna C. Martin, Heather M. Meyer, Caleb I. Fassett, Michael K. Barker, Angela Stickle, Benjamin D. Byron, Kathleen E. Mandt, Kurt D. Retherford
Figure caption: LROC mosaic of the lunar south pole provided by the LROC QuickMap tool. Cold-trap areas (T max <110 K) are masked in white.
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Degree-2 admittances Z 20 (blue) and Z 22 (red) as a function of the MoI. A two-layer model is assumed in this computation by accounting for the fourth-order expression for equilibrium figures (Tricarico 2014). Ice density is considered fixed (ρ Shell = 925  kg m−3), and we only vary the core density ﹩{\rho }_{\mathrm{Core}}﹩ between 2000 and 3000 kg m−3. The intersection of the admittances (Z 20 = Z 22) identifies the expected value of MoI = 0.335 that provides self-consistent results (e.g., Hemingway et al. 2018). The admittance uncertainties (blue and red shaded areas) are retrieved by assuming 3σ uncertainties for the shape (Tajeddine et al. 2017) and gravity models (this paper). Gray and yellow shaded areas show the level of accuracy for the MoI based on the gravity estimates obtained with Cassini (σ MoI = 0.002) and this study (σ MoI = 0.00016), respectively.
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Histograms for the Love number k 2 predicted through the MCMC interior model inversion based on the current knowledge of Enceladus’s mass and MoI. The probability distribution resembles a χ 2 distribution with a mode of 0.02, which is consistent with previous studies (e.g., Baland et al. 2016; Ermakov et al. 2021). The shaded area shows the level of uncertainty that is expected with the gravity investigation (this study, see Table 1).
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Power spectra of the gravity field computed from isostatically compensated and uncompensated topography (gray shaded area) and seafloor topography by varying its mean radius ﹩\left({R}_{{sf}}\right)﹩, amplitude (Δh), and density contrast with the ocean (Δρ). Each panel shows with colors the power spectrum of the gravity field from the seafloor topography by assuming constant values for Δρ = 1500 kg m−3 and Δh = 5 km (left), R sf = 190 km and Δh = 5 km (middle), and Δρ = 1500 kg m−3 and R sf = 190 km (right).
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Power spectra of the predicted gravity field based on isostatically compensated (gray dashed line) and uncompensated (gray solid line) topography (Tajeddine et al. 2017) and of the formal uncertainties of the gravity field determined with radio and optical data (blue dashed line) and radio only (red solid line). The black line shows the Kaula rule 40 × 10−5/l 2 that resembles the power spectrum of a partially compensated topography.
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Power dissipated in Enceladus’s interior as a function of ice shell and rocky core viscosity by assuming high rigidity (left) and low rigidity (right) for the rocky core.
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Degree-strength map of Enceladus’s gravity field obtained by using the covariance matrix from the numerical simulations and the expected acceleration profile based on the gravity from uncompensated topography.
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Histograms for core (a) radius and (c) density and ocean (b) depth and (d) density resulting from the MCMC carried out by using as observations 3-standard-deviation formal uncertainties of Enceladus’s mass, MoI, J 3, ﹩{Re}({k}_{2})﹩, and ﹩\mathrm{Im}({k}_{2})﹩ resulting from the numerical simulations of this study (see Table 1).
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Observation (black) and mapped (red) distributions and histograms of the ensemble for Enceladus’s mass, MoI, J 3, and Love number Re(k 2) and Im(k 2).
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Histograms for core (a) radius and (c) density and ocean (b) depth and (d) density resulting from the MCMC carried out by using as observations Enceladus’s mass and MoI measured by Cassini.
Paper: Gravity Investigation to Characterize Enceladus's Ocean and Interior
Authors: Antonio Genova, Marzia Parisi, Anna Maria Gargiulo, Flavio Petricca, Simone Andolfo, Tommaso Torrini, Edoardo Del Vecchio, Christopher R. Glein, Morgan L. Cable, Cynthia B. Phillips, Nicholas E. Bradley, Ricardo L. Restrepo, Declan M. Mages, Alessandra Babuscia, Jonathan I. Lunine
Figure caption: Histograms for core and ice shell (a, b) rigidities and (c, d) viscosities resulting from the MCMC interior model inversion.
Paper: Hunting for Hydrated Minerals on Trans-Neptunian Objects
Authors: Tom Seccull, Wesley C. Fraser, Dominik A. Kiersz, Thomas H. Puzia
Figure caption: Optical reflectance spectra of 2004 GV9. (A) Here we compare our new GMOS reflectance spectra of 2004 GV9 both to each other and to coarse spectra derived from published single-epoch photometry (Rabinowitz et al. 2008; DeMeo et al. 2009; Fraser et al. 2015; Tegler et al. 2016). Hollow points in the GMOS spectra are affected by incomplete background subtraction, telluric band residuals, proximity to the GMOS chip gaps, or a combination of these effects. All data sets are scaled to unit reflectance at 0.625 μm. We present all spectra calibrated with HD 124523 overlaid for direct comparison, and also offset for clarity. All offset spectra are offset vertically in increments of +0.2. (B) Here we show our 2004 GV9 spectra following division by a line fitted to them across their full wavelength coverage. Spectra from each epoch are offset vertically for clarity in increments of +0.1. Only spectra calibrated with HD 124523 are shown. Points affected by residuals of telluric absorption or imperfect background subtraction have been omitted. The data behind this figure are available in FITS format in a .tar.gz package.(The data used to create this figure are available.)
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Level curves of the resonant Hamiltonian (Equation (3)) for a zero-inclination 9:1 resonator (e = 0.65). The evolution of two synthetic resonators over a short 3 Myr N-body integration is also plotted. One of these objects (blue dots) was placed in the leading asymmetric island, while the other (orange dots) was placed in the symmetric island. Both objects initially had e = 0.65 and i = 0. The curves are plotted in a rather than Σ, as Σ is approximately linear in a over the small range of resonant behavior.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Final semimajor axis classification of objects for perturbers with different perihelion distances. All perturbers had a mass of 8.4 M ⊕. For each each perihelion distance, we group the nine perturber eccentricities and inclinations together into a single sample in order to obtain better statistics. Error bars (1σ) are derived by treating the number of objects in each classification category as a Poisson variable.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Survival rate as a function of initial perihelion distance (left) and inclination (right) in the control simulations, which contained only the four known giant planets with no distant perturber. Inclination bins are centered on multiples of 10°, and span 5° in either direction of the center. Perihelion distance bins are centered on multiples of 2 au, and span 1 au in both directions of the center. Error bars (1σ) are derived by treating the number of surviving objects in each bin as a Poisson variable.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Evolution of proper orbital elements for 100 randomly selected objects from the control simulations, which included only the four known giant planets and the generated resonators. While proper a is defined as the maximum of a over a sliding 10 Myr window, in this figure we follow Morbidelli (1997) and plot each object’s sliding maximum and minimum a, in order to preserve visual symmetry about the center of the 9:1 resonance. The dashed vertical line indicates the exact center of the resonance at 130.1 au, while the solid black lines are curves of constant perihelion distance.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Evolution of proper orbital elements for 100 randomly selected objects from the integration involving the perturber with M = 8.4 M ⊕, q = 240 au, e = 0.3, and i = 11°. As with Figure 3, both the maximum and minimum of a over the sliding 10 Myr window are plotted for each object to preserve visual symmetry. The dashed vertical line indicates the center of the 9:1 resonance, while the solid black lines are curves of constant perihelion distance.
Paper: Can Neptune’s Distant Mean Motion Resonances Constrain Undiscovered Planets in the Solar System? Lessons from a Case Study of the 9:1 Resonance
Authors: Matthew W. Porter, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams
Figure caption: Normalized distribution of libration amplitude in the 2 Myr extension of the control integration. Of the 10,000 total objects in the control simulation, 4138 exhibited libration in the extension integration.