adsabs/AstroCLIMB huggingface dataset:
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: The middle panel of this figure shows the detection of CN with Keck at 4.11 au in 2023 November. The top panel shows the lack of detection of CN at 4.2 au from McDonald ten days later. It is possible that this lack of detection is a matter of lack of sensitivity. The bottom panel is the de Vico spectrum as a comparison. Note that even with Keck we only see the lowest J-level lines for the P and R branches and do not see an obvious bandhead.
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: The region of the solar-removed CN band is shown for 2021 October 18 (scale on left side) and 2022 January 15 (scale on right side) along with the de Vico spectrum for comparison. Note the two K2 scales are offset with respect to one another for clarity. The dashed line denotes the bandhead of the CN band for de Vico. There is an apparent emission just to the red of the bandhead for January 15 (with an apparent absorption on October 18). There are no other features in either K2 spectrum.
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: The NH2 A 2A1 –X 2B1 (0, 4, 0)—(0, 0, 0) of NH2 is shown. In general, the NH2 lines do not form obvious band structures. The line at around 5731.5 Å is the most likely line to detect in this bandpass. It is clearly there at Rh = 2.51 au and may be detected as far out as 3.24 au.
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: The C2 d3Πg—a3ΠuΔv = 0 order of the spectra for each preperihelion night except 2022 January 15 are shown. There are clearly no C2 lines in the spectrum from 2021 October 18 at a heliocentric distance of 5.06 au. The spectrum from 2022 April 22 probably shows no features, while the (0, 0) bandhead is possibly visible on 2022 May 9. The (0, 0) bandhead is obviously present on 2022 June 10 while the (1, 1) bandhead begins to be believable on 2022 July 31. The two bandheads are marked with dashed lines.
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: The three forbidden oxygen lines are shown for 2022 June 25. Inspection of the three panels shows that the relative strengths of the comet lines and the telluric lines are very different for the 5577 Å lines versus the 6300 and 6363 Å lines.
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: Reflectance at 0.41 μm decreases with (a) accumulated fluence of radiation (expressed as the number of 24 hr days on Europa’s surface for an equivalent accumulation of electrons) and with (b) total energy deposited in the sample. Darkening at 0.41 μm occurs quickest and is strongest for Mg-chlorides but otherwise is similar for materials and somewhat linear, especially when irradiated at a given energy. Values for darkening measured after irradiating at a single energy are connected by a solid line. The gray rectangles are qualitative depictions of the clustering in the linear trends in the darkening of the materials other than Mg-chlorides. Not shown: the final 10 keV irradiation of 23% NaCl brine that lasted for ∼40 hr and the one irradiation at 20 keV that lasted another 25 hr (i.e., equivalent over 1 yr on Europa’s surface). Anhydrous NaCl is not shown because color center formation is the dominant spectral effect.
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: Visible spectra of a MgSO4 solution flash-frozen brine before irradiation (gray) and after irradiation at 1, 10, and 20 keV. The spectrum is dominated by water ice features at 1, 1.25, 1.5, 1.65, and 2 μm, with small nonice features at 1.3 and 1.7 μm. The feature at 2.2 μm is an artifact. Arrows marks feature in the infrared that is not present in water ice.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: H2SO4⋅8H2O is not affected by 1, 5, and 10 keV electrons but reddens when irradiated with 20 and especially 40 keV electrons with two inflection points, a weak one ∼0.425 μm and a strong one ∼0.55 μm. The infrared portion of this spectrum indicates grain size is very large (hundreds of microns). The data beyond 2 μm are noisy.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: Visible-infrared reflectance spectra of meridianiite, including pristine (gray) and after irradiation with 1 (magenta), 10 (cyan), and 20 keV (green). Arrows mark features in the infrared that are not present in water ice.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: Visible spectra of a MgSO4–NaCl solution pellet before irradiation (pristine in gray) and after irradiation at 1 (magenta), 10 (cyan), and 20 keV (green). Arrows mark features in the infrared that are not present in water ice.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: The electron irradiation did not fully alter any of the samples, i.e., in all cases, the penetration depth of the light at visible wavelengths exceeded the penetration depths of the electrons. (a) The penetration depth of electrons into water ice dramatically increases with increasing energy. Red “x”'s mark the penetration depths of various electron beam energies used in these experiments, and the blue curve is a model fit to those values. (b) High keV energies would be required for electrons to penetrate a largely transparent particulate material such as water ice (or most salts). Even 40 keV electrons do not fully sample the penetration depth of light at visible wavelengths for 10 μm grain sizes. The pellets created of unsieved but powered samples all have a fraction of grains >10 μm.
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: Linear modeling of the irradiation-induced reddening of sulfuric acid hydrate allows the extrapolation of the spectral effects to larger total fluences than was achieved in the laboratory to enable more accurate comparisons to the reflectance spectra of Europa. Reflectances were extrapolated independently at every wavelength. (a) The measured darkening at three example wavelengths for progressive irradiation of sulfuric acid hydrate (symbols) and linear fit (line). (b) The measured (black) and modeled or derived (red) spectra. The vertical lines in (b) denote the wavelengths that correspond to the same color lines in (a).
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: The dependence of the depth of the 0.46 μm F-center in NaCl on (a) equivalent exposure time on Europa’s surface in Earth days and (b) cumulative energy dosed onto the sample.
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: FeSO4⋅7H2O before (gray) and after irradiation with 40 keV electrons (red).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Orbital Decay Candidates Reconsidered: WASP-4 b Is Not Decaying and Kepler-1658 b Is Not a Planet
Authors: Joshua N. Winn, Guđmundur Stefánsson
Figure caption: Evidence for dilution in the light curve of Kepler-1658. Top: Kepler light curve, with its native 1 minute sampling as well as the phase-averaged version used for model fitting. Bottom: residuals between the data and the best-fit transiting-planet model. The pattern of residuals is well fitted by a model in which the “transits” are eclipses of a faint binary that contributes only 1.7% of the total light.
Paper: Orbital Decay Candidates Reconsidered: WASP-4 b Is Not Decaying and Kepler-1658 b Is Not a Planet
Authors: Joshua N. Winn, Guđmundur Stefánsson
Figure caption: Constraints on dilution from the Kepler-1658 light curve. Top: goodness of fit, χ2, as a function of ϵ, the fraction of the light contributed by the blended binary. Middle and bottom: corresponding values of the radius ratio between the two stars of the eclipsing binary, and the eclipse impact parameter. The data favor ϵ ≈ 0.017, r/R ≈ 0.27, and b ≈ 0.
Paper: Orbital Decay Candidates Reconsidered: WASP-4 b Is Not Decaying and Kepler-1658 b Is Not a Planet
Authors: Joshua N. Winn, Guđmundur Stefánsson
Figure caption: Kepler-1658 as a hierarchical triple star. The dependence of various observables is shown as a function of the mass of star B. Choosing MB ≈ 0.75 M⊙ (light gray band) is compatible with all the observables except the J-band apparent transit depth (see the text for details).
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: Postfit range-rate residuals (in mm s−1 units for a 60 s integration time), plotted against time from periapsis, in minutes. Different panels may have different vertical and horizontal (depending on the time of pericenter) scales. Different energy levels for the f-mode with ℓ = −m = 2 are represented by colors: green for low energy, teal for moderate energy, and purple for high energy. The simulations are carried out separately for T1 (left side) and T3 (right side). On each side, the repeated rows of the same color show the series of experiments including progressively more orbits in the fit.
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: Same as Figure 10 but for a single zonal f-mode with ℓ = 2 and m = 0. Different panels may have different vertical and horizontal (depending on the time of pericenter) scales. Please note that in the T1, low-energy case, five periapses (P1–P5) are required for the normal mode effects to become visible in the range-rate residuals. The black dots between P2 and P5 indicate this. For all other cases, either two or three periapses (P1–P3) are sufficient, and the notation follows that of Figure 10.
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: SNR of postfit range-rate residuals as a function of mode angular degree ℓ (x-axis) of the f-modes included in the simulations, and number of combined arcs (y-axis), shown for the three energy levels and for both the T1 and T3 cases. The SNR is plotted on a logarithmic scale, with detection defined as SNR > 3 (white dashed lines).
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: SNR from single passes. Same as Figure 6 but for single zonal f-modes (m = 0).
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: 3σ uncertainty for static zonal coefficients J2–J8 for T1 (left panel) and T3 (right panel). The simulations were repeated for low-energy modes (green line), moderate-energy modes (teal line), and high-energy modes (purple line). The gray shaded areas represent the solutions from M. Parisi et al. (2024). The black diamonds represent the value of the gravity moments from the uniformly rotating Uranus model.
Paper: A Multiarc Approach to Detecting Uranus’s Normal Modes via Doppler Tracking of a Planetary Orbiter
Authors: Marzia Parisi, Seho Kim, Chris Mankovich, James Fuller, A. James Friedson, Steven Markham
Figure caption: SNR from single passes. Same as Figures 6 and 8 but for multiple p- and f-modes with ﹩2\,\leqslant \,\ell \,\leqslant \,{\ell }_{{\rm{\max }}}﹩ and ∣m∣ ≤ ℓ.
Paper: Charged Ejecta Clouds from Granular Beds after Slow Impacts
Authors: Matthias Keulen, F. Oehme, G. Wurm, J. E. Kollmer
Figure caption: Different kinds of samples used. (a) Steel spheres, (b) basalt pebbles, (c) granular basalt bed, and (d) size distribution of the basalt bed determined using a Mastersizer 3000 with the peak at diameters of 586 μm.
Paper: Charged Ejecta Clouds from Granular Beds after Slow Impacts
Authors: Matthias Keulen, F. Oehme, G. Wurm, J. E. Kollmer
Figure caption: Experiment setup with launch mechanism pointing toward the regolith in its grounded cup and the resulting ejecta falling into the Faraday cup.
Paper: Charged Ejecta Clouds from Granular Beds after Slow Impacts
Authors: Matthias Keulen, F. Oehme, G. Wurm, J. E. Kollmer
Figure caption: Measured ejecta charge over mass for steel impactors. The green (triangle) data include the charge of the impactor. Symbols with error bars mark the averages of 0.1 g binned. For visibility, they are slightly shifted for different data sets.
Paper: Charged Ejecta Clouds from Granular Beds after Slow Impacts
Authors: Matthias Keulen, F. Oehme, G. Wurm, J. E. Kollmer
Figure caption: Measured ejecta charge over mass for basalt impactors. The green (triangle) data include the charge of the impactor. The x-axes are plotted logarithmically, as masses including and excluding impactors varied greatly.
Paper: Charged Ejecta Clouds from Granular Beds after Slow Impacts
Authors: Matthias Keulen, F. Oehme, G. Wurm, J. E. Kollmer
Figure caption: Histograms of measured ejecta charges for steel impactors. From top to bottom: fast impacts, slow impacts, and slow impacts where the impactor charge was also measured.
Paper: Charged Ejecta Clouds from Granular Beds after Slow Impacts
Authors: Matthias Keulen, F. Oehme, G. Wurm, J. E. Kollmer
Figure caption: Charge distribution on impactors. Top: steel impactor from 20 measurements. Bottom: basalt impactor from 20 measurements divided between the slightly different launch methods.
Paper: Charged Ejecta Clouds from Granular Beds after Slow Impacts
Authors: Matthias Keulen, F. Oehme, G. Wurm, J. E. Kollmer
Figure caption: Histograms of measured ejecta charges for basalt impactors.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: (a) Total tidal heating (in GW) vs. the effective viscosity of the ice shell and the core. The narrow regions bounded by the red lines indicate the range of heat loss that covers the estimates by C. Howett et al. (2011), D. J. Hemingway & T. Mittal (2019), and R. S. Park et al. (2024). (b) Tidal heating variation with ice shell effective viscosity for a fixed ηcore = 1020 Pa.s. (c) Tidal heating variation with core effective viscosity for a fixed ηshell = 1016 Pa.s. The gray areas highlight the region where tidal heating values are compatible with the estimated steady-state heating. The results are presented for Dshell = 14 km, Docean = 34 km, ρocean = 1000 kg m−3, ﹩{R}_{{\rm{core}}}=204﹩ km, ρshell = 930 kg m−3, μshell = 3 GPa, κshell = 10 GPa, ﹩{\rho }_{{\rm{core}}}=2175\,{\rm{kg}}\,{{\rm{m}}}^{-3}﹩, ﹩{\kappa }_{{\rm{core}}}=20﹩ GPa, and ﹩{\mu }_{{\rm{core}}}=15﹩ GPa. We assume an Andrade viscoelastic rheology.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: Exploration of the potentially observable quantities consistent with estimates of mass, heat flux, and libration amplitude for tidal dissipation scenarios in the shell and core. The heat flux is assumed as ﹩15\,{\rm{GW}}\lt \dot{E}\lt 40\,{\rm{GW}}﹩, covering the estimated ranges in D. Hemingway et al. (2018) and R. S. Park et al. (2024), and the direct measurements (C. Howett et al. 2011). Libration is assumed to be in the range 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩082 < γ < 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩169, covering the estimates in I. Nadezhdina et al. (2016), P. Thomas et al. (2016), and R. S. Park et al. (2024). Tidal heating produced in the shell in either scenario is also shown. In the 2D pdfs, the pink–gray and red–yellow themes refer to dissipation in the shell and core, respectively. All variables are shown in logarithmic axes. Unit conventions are the same as in Figure 4.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: Exploration of the potentially observable geodetic quantities that are consistent with estimates of mass, heat flux (C. Howett et al. 2011; D. J. Hemingway & T. Mittal 2019; R. S. Park et al. 2024), and libration amplitude spanned by estimates in I. Nadezhdina et al. (2016), P. Thomas et al. (2016), and R. S. Park et al. (2024). Other observables in this plot are free to vary. In the 2D pdfs, black (yellow) color indicates low (high) probability. The observed multiple peaks in the pdfs of ∣k2∣, ∣h2∣, ∣l2∣, and phase lags reflect the different regimes of dissipation consistent with the observations (see Figure 3). Phase lags of ﹩{\epsilon }_{{k}_{2}}﹩, ﹩{\epsilon }_{{h}_{2}}﹩, and ﹩{\epsilon }_{{l}_{2}}﹩ are in degrees, the amplitude of the libration is in meters, and J3 is multiplied by 106.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: Variations of the (a) period of natural (free) libration and (b) amplitude of forced libration of Enceladus as a function of shell thickness and density. The orbital period of Enceladus is shown by a gray line in (a). The end-member values of the amplitude of libration inferred by I. Nadezhdina et al. (2016), P. Thomas et al. (2016), and R. S. Park et al. (2024) (370 m < γ < 750 m) are shown by red lines in (b). The results are presented for ρocean = 1000 kg m−3, ﹩{R}_{{\rm{core}}}=197﹩ km, ρshell = 900 kg m−3, μshell = 3 GPa, κshell = 10 GPa, ηshell = 6 × 1013 Pa.s, ﹩{\rho }_{\mathrm{core}}=2320\,\mathrm{kg}\,{{\rm{m}}}^{-3}﹩, ﹩{\mu }_{{\rm{core}}}=40﹩ GPa, ﹩{\kappa }_{{\rm{core}}}=100﹩ GPa, and ηcore = 1019 Pa.s. The horizontal and vertical axes and the libration amplitude color scale are logarithmic.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: Tidal Love number amplitudes ((a), (b), and (c)) and phase lags ((d), (e), and (f)) for different shell and core viscosities. The same interior structure parameters as in Figure 2 are used.
Paper: Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
Authors: Amirhossein Bagheri, Mark Simons, Ryan S. Park, Alexander Berne, Douglas Hemingway, Mohit Melwani Daswani, Steven D. Vance
Figure caption: The pdfs of ice shell and core viscosities for each of the two cases of tidal dissipation occurring dominantly in the shell (panel (a)) and in the core (panel (b)), corresponding to two sets of observables in Figure 5.
Paper: The Caltech Mission to Apophis: Accelerating Planetary Science and Planetary Defense
Authors: Adriana Daca, Masatoshi Hirabayashi, Yaeji Kim, Joseph DeMartini, Carol Raymond, Alain Herique, Mark Haynes, Dirk Plettemeier, Bjorn Davidsson, José Andrade
Figure caption: Variations in the axis length change, i.e., the time variations in the relative separations along the longest axes of 10 particle segments (i.e., a pair of two particles attached to each other) to their initial separations. A positive change indicates the pair experiences tension, while a negative change means it experiences compression. The timing of ECA is marked with a black dashed line. Panel (a) shows the case of a hexagonal-close-packed rubble-pile Apophis with a bulk density of ∼2400 kg m−3 for a single encounter geometry. Particles are ∼7.18 m in radius, and Apophis is not tumbling. Panel (b) illustrates a random, polydisperse packed rubble-pile Apophis with a bulk density of ∼2400 kg m−3 and particles ranging between 2.4 and 7.18 m in diameter, which follows a size–frequency distribution with a power law with slope −3.
Paper: The Caltech Mission to Apophis: Accelerating Planetary Science and Planetary Defense
Authors: Adriana Daca, Masatoshi Hirabayashi, Yaeji Kim, Joseph DeMartini, Carol Raymond, Alain Herique, Mark Haynes, Dirk Plettemeier, Bjorn Davidsson, José Andrade
Figure caption: Probabilistic characterizations of stress variations during ECA, which is 140 minutes after the simulation starts. Panel (a) describes the probability of surface elements exceeding a ﹩{J}_{2}^{0.5}﹩ variation of 0.1 Pa due to rotational uncertainties, where J2 is the invariant of squared shear stress. A probability of unity would indicate that the provided surface element has a shear stress variation exceeding 0.1 Pa, regardless of the rotational state during ECA. Panel (b) shows the time evolution of maximum shear stress variations considering rotational variations. The closest encounter occurs between 2.5 and 3 hr in this plot. The panels were provided by M. Hirabayashi et al. (2021) but modified in this manuscript.