adsabs/AstroCLIMB huggingface dataset:
Paper: Surface Binding Energies for Amorphous Plagioclase Feldspar Calculated Using Molecular Dynamics
Authors: Amanda Ricketts, Benjamin A. Clouter-Gergen, Anastasis Georgiou, Deborah Berhanu, Liam S. Morrissey
Figure caption: Visualization of local bonding environments for atoms with near-minimum and near-maximum SBE values for each element in amorphous albite.
Paper: Surface Binding Energies for Amorphous Plagioclase Feldspar Calculated Using Molecular Dynamics
Authors: Amanda Ricketts, Benjamin A. Clouter-Gergen, Anastasis Georgiou, Deborah Berhanu, Liam S. Morrissey
Figure caption: Frequency distributions for the elemental SBEs of albite (A) and anorthite (B). SBEs are plotted in 1 eV bins.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: Logarithmic production rates for comet 21P/Giacobini-Zinner as a function of the log of the heliocentric distance. Open symbols represent data obtained before perihelion, while filled symbols are used for post-perihelion data. Downward-pointing arrows near the bottom of a panel indicate measurements that were attempted but went to zero after sky and continuum subtraction and are listed as “und,” or undefined, in Table 4. The vertical dashed line represents the perihelion distance and is color-coded to match the comet.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: Logarithmic production rates for comets 114P/Wiseman-Skiff (blue downward-pointing triangles), 123P/West-Hartley (orange squares), 126P/IRAS (violet diamonds), and 168P/Hergenrother (red circles). Further information is the same as in Figure 1.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: Key logarithmic abundance ratio plots from the restricted subset of our database, with the five additional strongly carbon-chain depleted comets from our full database included and represented by skeletal symbols. Logarithmic mean production rate ratios of minor species with respect to OH and CN are presented and coded for our six compositional classes, listed in the key at the top of the figure.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: Logarithmic production rates for comets 31P/Schwassmann-Wachmann 2 (blue circles), 155P/Shoemaker 3 (orange triangles), 260P/McNaught (green squares), and 298P/Boattini (violet downward-pointing triangles). Further information is the same as in Figure 1.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: Logarithmic production rates for comets 57P/duToit-Neujmin-Delporte (orange downward-pointing triangles), 101P/Chernyk (red squares), 217P/LINEAR (blue diamonds), and 290P/Jager (green circles). Further information is the same as in Figure 1.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: C2-to-CN logarithmic production rate ratios vs. heliocentric distance (rH) for comets 21P/G-Z (left) and 73P/S-W 3 (1995 measurements of the fragmenting main nucleus + Component C from 2006; right). Open symbols represent data obtained before perihelion, while filled symbols are used for post-perihelion data. Downward-pointing arrows near the bottom of a panel indicate measurements that were attempted but went to zero after sky and continuum subtraction. There is a trend of increasing C2-to-CN production rates with decreasing heliocentric distance throughout our database, independent of compositional class. Nearly all abundance ratio sets for G-Z, and all for S-W 3—even at smaller heliocentric distances—are clearly well below the nominal boundary of approximately −0.13, above which we consider an abundance ratio to be typical.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: Logarithmic production rates for comets 43P/Wolf-Harrington (violet squares), 87P/Bus (green downward-pointing triangles), and C/Shoemaker (1984s) (orange circles). Further information is the same as in Figure 1.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: Logarithmic mean production rate ratios of C2-to-CN and C3-to-CN vs. mean heliocentric distance (rH). Colors and symbols are the same as in Figure 6. For C2-to-CN, between 1 and 3 au there is a 0.3 change in the slope of the fit (log space) for comets with typical carbon-chain values, which is equal to almost a factor of 2. For the strongly depleted class, the progression is also present and is just slightly steeper with a 0.4 change in the fit, or a factor of 2.5. This progression is the result of Haser model parameters as discussed in the text and is not seen for C3-to-CN. For both ratios, the offset between typical and strongly carbon-chain depleted compositional classes is clear at all heliocentric distances.
Paper: Comprehensive Analyses of the Strongly Carbon-chain Depleted Comets in Lowell Observatory’s Narrowband Photometry Database
Authors: Allison N. Bair, David G. Schleicher
Figure caption: Logarithmic mean production rate ratios of C2-to-CN and C3-to-CN as a function of the Tisserand invariant (TJ) with respect to Jupiter. Colors and symbols are the same as in Figure 6. The association of carbon-chain depleted comets with the JF (TJ > 2) dynamical class is very strong. Nearly 90% of comets believed to originate from the Oort Cloud have typical composition (green), and most carbon-chain depleted comets (light and dark blue) are JF, presumed to have originated in the Kuiper Belt.
Paper: A High-precision, Differentiable Code for Solar System Ephemerides
Authors: Ben Cassese, Malena Rice, Tiger Lu
Figure caption: The difference in positions predicted by JPL’s solution 220, assist, and jorbit. All simulations began from the same initial position/velocity on 2029 January 1, and their differences are the result of different implementations of the acceleration model and/or underlying integrator. Dashed lines show the results when leaving out individual components of the acceleration model. ✎
Paper: A High-precision, Differentiable Code for Solar System Ephemerides
Authors: Ben Cassese, Malena Rice, Tiger Lu
Figure caption: Comparison between jorbit’s derivative calculations computed via automatic differentiation (autodiff. on axis labels) and those computed by a simple finite differencing method (num. on axis labels). The upturn at small step sizes is due to numerical errors in the finite differencing scheme at small step sizes. ✎
Paper: Resolved Convection in Hydrogen-rich Atmospheres
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: The saturation density ρ* = pμ*/(RT) for a mixture of water vapor and a background gas with molar mass μa varying from 44 g mol−1 to 2 g mol−1. The total pressure is held fixed at 105 Pa, and the temperature ranges from 200 K to the boiling point of water at this pressure. For cases in which the background gas is lighter than water vapor, the portions of the curves for which ρ* increases with temperature are plotted with dashed lines, and the point where the saturation specific humidity ﹩{q}_{v}^{* }﹩ equals the critical humidity threshold qcrit (Equation (13)) is marked with a solid circle.
Paper: Resolved Convection in Hydrogen-rich Atmospheres
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: High-frequency (hourly) output from 20 days of the DeepBL simulations with μa = 4 and 6 g mol−1. Top row: surface sensible heat flux (SHF) in W m−2. Bottom row: column-integrated cloud water in kg m−2.
Paper: Resolved Convection in Hydrogen-rich Atmospheres
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: Cloud emission temperatures and qcrit values for a wide range of condensing species. We define cloud emission temperature as the temperature for which ﹩{q}_{v}^{* }(p,T)={q}_{{\rm{crit}}}﹩, for a representative emission pressure of p = 0.1 bar. The latent heat and saturation vapor pressure curves required to calculate qcrit and ﹩{q}_{v}^{* }﹩ were obtained from P. Gao et al. (2020) and R. T. Pierrehumbert (2011).
Paper: Resolved Convection in Hydrogen-rich Atmospheres
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: Results from the VaryBeta experiment. (Left) Temperature profiles. (Right) Specific humidity profiles.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: The GIRO probe prototype printed in resin and coated with conductive paint to emulate the performance of the flight version that will be printed in aluminum. The two patch antennas are shown, one of which—for this test—has replaced one of three LED housings. The yellow instrument is a level being used to calibrate the geometry of the antenna test.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: A conceptual representation of two GIRO probes being deployed at Enceladus, showing the deployer, the two-way radio link with the High Gain Antenna (HGA), and the watching cameras that will use the lights on each probe to enhance the gravity signature extraction.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: A schematic of the simple, but very high-precision, analog, carrier-only X-band transponder, showing the two phase-locked loops of the design.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: Electropneumatic deployment system of the first prototype GIRO deployer under test.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: Probe transmitter antenna radiation pattern, closely following the a priori simulation, with a net performance (grounded to the conductive shell) of better than 6 dB. Panels (a) and (c) show the variation of the angle away from the spin axis plots for simulation and measurement, respectively. Panels (b) and (d) are zoomed-in views of (a) and (c), respectively.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: The rms of expected uncertainty of the recovered Enceladus gravity field.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: Modeling of the thermal balance/equilibrium of the GIRO probe, showing equilibrium in flight at about 16°C.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: The transponder brassboard (utilizing component evaluation boards) undergoing lab testing (the annotations refer to components and quantities shown in Figure 2).
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: The battery cassette/carrier.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: Performance of GIRO’s analog transponder, showing an AD coherence of several times better than the technology goal at a 100 s integration time.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: A resin preprint of the second-generation GIRO structural design, showing the three LED fixtures on the right.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: The GIRO probe antennas undergoing tests in the radio test chamber.
Paper: Gravity Imaging Radio Observer (GIRO) for Planetary Science and Mission Opportunities
Authors: R. S. Park, J. E. Riedel, E. J. Brandon, N. E. Harvey, S. Manafi, M. C. Smart, Z. J. Towfic, A. Berne, W. I. Bertiger, J. T. Keane, A. S. Konopliv, N. Mastrodemos, M. Simons, S. D. Vance, A. T. Vaughan
Figure caption: Expected accuracy of the recovered lunar gravity field.
Paper: A Change of the Rotation Period of Asteroid (65803) Didymos Caused by the DART Impact
Authors: Josef Ďurech, Petr Pravec, Masatoshi Hirabayashi, Derek C. Richardson, Harrison Agrusa, Ryota Nakano
Figure caption: The dependence between ΔP and Δφ. The red circle represents the best-fit values for the original dataset, with the spin pole of Didymos fixed in the direction of the orbital pole of Dimorphos. Blue points are based on bootstrap samples. When the spin axis direction is optimized, the best-fit solution for ΔP and Δφ moves to values represented by the red triangle. Bootstrap samples with free pole direction are shown as green triangles.
Paper: A Change of the Rotation Period of Asteroid (65803) Didymos Caused by the DART Impact
Authors: Josef Ďurech, Petr Pravec, Masatoshi Hirabayashi, Derek C. Richardson, Harrison Agrusa, Ryota Nakano
Figure caption: The correlation between ΔP and tchange. The red points represent the results based on the original dataset. The blue points are results based on bootstrap data.
Paper: A Change of the Rotation Period of Asteroid (65803) Didymos Caused by the DART Impact
Authors: Josef Ďurech, Petr Pravec, Masatoshi Hirabayashi, Derek C. Richardson, Harrison Agrusa, Ryota Nakano
Figure caption: Convex shape model of Didymos reconstructed from its light curves.
Paper: A Change of the Rotation Period of Asteroid (65803) Didymos Caused by the DART Impact
Authors: Josef Ďurech, Petr Pravec, Masatoshi Hirabayashi, Derek C. Richardson, Harrison Agrusa, Ryota Nakano
Figure caption: Example light curves at which the difference between the constant-period model (dashed black curve) and the model with the two different periods (solid red curve) is most prominent. The blue points are measured photometric data normalized to the unit mean brightness.
Paper: A Change of the Rotation Period of Asteroid (65803) Didymos Caused by the DART Impact
Authors: Josef Ďurech, Petr Pravec, Masatoshi Hirabayashi, Derek C. Richardson, Harrison Agrusa, Ryota Nakano
Figure caption: Histograms of periods determined from bootstrap samples for four subsets of light-curve data. The postimpact periods are separated from the preimpact periods.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Top panel: retrieved temperature profiles (solid colored lines) and uncertainty (dotted colored lines) using the non-auroral-mean spectra at 65∘S for IRTF-TEXES results. Results are colored according to the pressure level, as indicated by the legend on the left. The bottom left panel shows similar results for temperatures retrieved from the southern auroral-mean spectra (poleward of the MAE). The bottom right panel shows retrieved profiles of CH3, which was allowed to vary in fitting the auroral-mean spectra. Only the 1 μbar results are shown where there is sensitivity to CH3 (see Figure 7).
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: CH4 homopause altitudes as a function of latitude, as derived from IRTF-TEXES observations on 2019 August 20. Results in the southern and northern hemispheres are shown on the left and right, respectively. The top row shows results previously presented in J. A. Sinclair et al. (2020) using an earlier model grid; the bottom row shows results derived in this work using the updated model grid (see Section 4.2 for further details). Black results denote a longitudinal mean where all sampled longitudes were coadded into a single spectrum. Blue results at high northern latitudes denote the nonauroral mean, where spectra recorded at longitudes outside/equatorward of the MAE were coadded into a single spectrum. Red results denote an auroral mean using observations inside or poleward of the MAE. Results that only shown an upper error bar are where a lower 1σ uncertainty could not be derived and so we show only an upper (1σ) limit. Vertical dashed lines mark the lowest-latitude extent of the southern and northern MAEs (B. Bonfond et al. 2017).
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Variations in the χ2 (Equation (1)) as a function of the model tested in fitting the non-auroral-mean observation (left column) and auroral-mean (right column) observation at 60∘N on 2019 August 20. Results in the top row use the model grid presented in this work (Figure 6); results in the bottom row use the model grid presented in J. A. Sinclair et al. (2020). The conversion from homopause pressure of each model to altitude with respect to 1 bar is shown in the upper x-axis of each panel. Vertical solid and dotted red lines denote the best-fitting result and the 1σ confidence levels, respectively.
Paper: Improved Constraints on the Vertical Profile of CH4 at Jupiter’s Mid- to High Latitudes, Using IRTF-TEXES and SOFIA-EXES Spectroscopy
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, Matthew Richter, Maisie Rashman, Curtis de Witt, Julianne Moses, Vincent Hue, Pablo Rodríguez-Ovalle, Thierry Fouchet, Ananyo Bhattacharya, Bilal Benmahi, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Retrieved temperature profiles using the non-auroral-mean (top panel) and auroral-mean (bottom panel) observations at 60∘N. The black solid line indicates the a priori temperature profile; solid colored lines show retrieved profiles, with the uncertainty shown as a dotted line. Green results correspond to the inversion where the 587, 606, and 1248 cm−1 spectral settings were used; red results correspond to the inversion where the 587 cm−1 spectral setting was omitted. The reduced χ2 values for each retrieval are indicated in each plot.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: Top: distributions of the probability (y-axis) for a simulated atmosphere to yield the given network metric value, global species variance, or CH4 abundance in log ppm (x-axis) over each of the sampled Archean Earth data sets, probed at 0.2 mbar. Dark brown represents the abiotic flux model set; light brown represents the distributions after perturbing this model by removing C2H2. Dark green represents the biotic flux model set; light green represents the distributions after perturbing this biotic model. Bottom: Anderson scores of the biotic flux scenario as compared to the perturbed biotic model and the abiotic flux scenario compared to the perturbed abiotic model, demonstrating how the network metrics are much more sensitive to the perturbation than methane gas abundance or global species variance.
Paper: A Complex Systems Approach to Exoplanet Atmospheric Chemistry: New Prospects for Ruling Out the Possibility of Alien Life As We Know It
Authors: Theresa Fisher, Estelle Janin, Sara Imari Walker
Figure caption: A simplified example of a set of chemical reactions represented graphically as a network. The reactions included in this network are CH4 + O2 → H2O + CO2, H2 + O2 → H2O, and H2O2 → H2 + O2. Each species present in the reaction list is represented by a node; reactant nodes are connected via edges to the nodes representing the products of the reactions they participate in. Edge weights correspond to the rates of the reactions represented by the edges, calculated as the reaction rate constant multiplied by the abundance of the reactants (edge weight values shown in this figure are for illustrative purposes only).