adsabs/AstroCLIMB huggingface dataset:
Paper: Comet 21P/Giacobini–Zinner: Narrowband Photometry of the Prototype of Carbon-chain Depleted Comets at Multiple Apparitions
Authors: David G. Schleicher
Figure caption: The logarithms of representative production rate ratios are presented as a function of time. Symbols are the same as in Figure 1. Note that the C2-to-CN ratio (top panel) shows little variation during an apparition, and the apparent offset between the 1985 and the later apparitions is entirely an artifact of using systematically smaller apertures in 1985 and aperture effects for C2 due to limitations of the Haser model. The CN-to-OH ratio (middle), in contrast, exhibits a large variation that we attribute to differences in this abundance ratio between source regions, coupled with seasonal solar illumination changes for each source. The NH-to-OH ratio (bottom) exhibits the opposite trends to the CN-to-OH ratio, again implying differences in composition between sources regions.
Paper: Comet 21P/Giacobini–Zinner: Narrowband Photometry of the Prototype of Carbon-chain Depleted Comets at Multiple Apparitions
Authors: David G. Schleicher
Figure caption: Logarithms of the gas production rates and A(θ)fρ of the dust as a function of time from perihelion. Different symbols and colors distinguish each apparition (see key above the plots); open symbols are pre-perihelion, and filled points are post-perihelion. The 1σ photometric uncertainties for individual data points are sometimes quite large owing to the faintness of G-Z at large distances and the overall strong depletion of the carbon-chain species and the moderate depletion of NH, as compared to OH and CN. Note that the production rates for all species reach a maximum 3–4 weeks before perihelion and drop rapidly in the 6–8 weeks surrounding perihelion. Following perihelion, all species continue to vary in a common manner for a given apparition, but differences between apparitions are readily evident.
Paper: Comet 21P/Giacobini–Zinner: Narrowband Photometry of the Prototype of Carbon-chain Depleted Comets at Multiple Apparitions
Authors: David G. Schleicher
Figure caption: Logarithm of the water production rates, based on our empirical conversion of the Haser model OH production rates, as a function of the time from perihelion (top panel). Symbols are the same as in Figure 1. The bottom panel shows the effective active area, also as a function of time, using the standard isothermal sphere vaporization model. As discussed in Section 4, the strong seasonal variation, coupled with maximum water production taking place several weeks prior to perihelion, implies a high-latitude source illuminated by a high subsolar latitude. If true, this combination could yield a vaporization rate as much as 4× larger than the standard model, thereby requiring an area only one-quarter the peak shown.
Paper: Comet 21P/Giacobini–Zinner: Narrowband Photometry of the Prototype of Carbon-chain Depleted Comets at Multiple Apparitions
Authors: David G. Schleicher
Figure caption: Logarithm of the phase-corrected dust production, A(0°)fρ, as a function of time from perihelion (top panel). Symbols are the same as in Figure 1. The generally lower values in 1985 are again due to the use of systematically smaller apertures at this apparition, coupled with the near-ubiquitous aperture effect we have detected in most comets. The effective dust-to-gas ratio, based on log A(0°)fρ–log Q(OH), is shown as a function of time (bottom panel). This ratio shows less variation than found in many other comets.
Paper: Near-infrared Spectroscopy of the Nucleus of Low-activity Comet P/2016 BA14 during Its 2016 Close Approach
Authors: Theodore Kareta, Vishnu Reddy, Juan A. Sanchez, Walter M. Harris
Figure caption: In the left panel, the maximum-likelihood thermal model with p  V  = 0.014 and η = 1.627, or p  V  = 0.023 and η = 1.622 after a correction for phase reddening, is shown as a dark red line, while the uncorrected data are shown as black open circles. The thermal model–corrected all-reflectance spectrum is shown as blue open circles. In the right panel, a corner plot shows the distribution of fit parameter values for p  V  and η for both models. The albedo constraint from radar observations (Naidu et al. 2016) is plotted as a vertical line. As expected, the albedo and beaming parameters show some degeneracy, as the model constrains the peak subsolar temperature, which is a function of both parameters. (See text for more details.)
Paper: Near-infrared Spectroscopy of the Nucleus of Low-activity Comet P/2016 BA14 during Its 2016 Close Approach
Authors: Theodore Kareta, Vishnu Reddy, Juan A. Sanchez, Walter M. Harris
Figure caption: Retrieved reflectance spectra of BA14 as obtained on 2016 March 7 and 10 from the NASA IRTF, normalized such that R(λ = 1.5 μm) = 1.0. The spectra on both nights are similarly red-sloped with a thermal excess visible at longer wavelengths (>2.25 μm), and the spectrum obtained on March 10 is slightly redder at all wavelengths with a slight slope break near 1.4–1.5 μm and a more linear spectrum at shorter wavelengths. See text for more details.
Paper: Near-infrared Spectroscopy of the Nucleus of Low-activity Comet P/2016 BA14 during Its 2016 Close Approach
Authors: Theodore Kareta, Vishnu Reddy, Juan A. Sanchez, Walter M. Harris
Figure caption: The along-slit spatial profiles are shown for BA14, as well as the telluric star observed immediately before and after as obtained on 2016 March 7. The profiles shown are medians over the wavelengths corresponding to the Jband (1.17–1.33 μm). The visible seeing was quite good (∼0.″51), and the resulting profiles are quite narrow, but the profile of BA14 is still significantly wider than the star was before or after. Worse seeing (such as that obtained on 2016 March 10) would not have shown this clear hint of activity, however weak it might be. See text for more details.
Paper: Ariel's Elastic Thicknesses and Heat Fluxes
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Erin Leonard, Tom Nordheim, Francesca Scipioni
Figure caption: (a) Annotated version of Voyager 2 ISS image c2684539 (pixel resolution: 995 m pixel−1) showing the Pixie Group chasmata analyzed in this study (Sylph is shown in Figure 5). (b) The locations of the profile lines used in our analyses. (c) The DEM we generated that covers these chasmata. (d) The locations of impact craters used to estimate the uncertainty associated with the DEM by analyzing crater depth-diameter ratios and comparing them with previously estimated values for Ariel (results shown in Figure A1).
Paper: Ariel's Elastic Thicknesses and Heat Fluxes
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Erin Leonard, Tom Nordheim, Francesca Scipioni
Figure caption: The large chasmata on Ariel. (a) The Pixie Group (cyan and orange arrows), which is the older set of canyons, relative to the Kachina Group (Voyager ISS image c2684535). The Pixie Group includes Brownie, Kewpie, Pixie, Slyph, Korrigan, and Kra Chasmata. Additionally, the Pixie Group includes separated canyons that may have originally aligned with Kra Chasma (orange arrows), which may have been offset due to rafting of large blocks (Croft & Soderblom 1991). (b) The Kachina Group (cyan arrows), which is likely younger than the chasmata within the Pixie Group. The Kachina Group is made up of faults comprising Kachina Chasmata and nearby subparallel faults (Voyager ISS image c2684533). (c) Double ridges (cyan arrows) present near the center of smooth floored chasmata in the Pixie Group (Voyager ISS image c2684539).
Paper: Ariel's Elastic Thicknesses and Heat Fluxes
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Erin Leonard, Tom Nordheim, Francesca Scipioni
Figure caption: Annotated version of the geologic map of Ariel’s imaged southern hemisphere (Croft & Soderblom 1991). The locations of the DEMs (cyan boxes) created for this study, covering the large chasmata, are shown.
Paper: Ariel's Elastic Thicknesses and Heat Fluxes
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Erin Leonard, Tom Nordheim, Francesca Scipioni
Figure caption: Diagram interpretation of chasma morphology, consisting of two bounding normal faults with evidence for flexure in the form of raised rims exterior to the faults and chasma. The flexural troughs bounding the chasma (gray shaded area) are shown. The orange arrows represent the directions of displacement.
Paper: A Collision Mechanism for the Removal of Earth's Trojan Asteroids
Authors: Kevin J. Napier, Larissa Markwardt, Fred C. Adams, David W. Gerdes, Hsing Wen Lin, 省文 林
Figure caption: Distributions of incoming speeds (left) and incoming direction (right) for asteroids with orbits leading to close encounters with Earth. In both plots, the asteroid orbits have semimajor axes in the range a = 1–5 au, and a uniform distribution of eccentricity. Only those asteroid orbits with sufficiently large values of eccentricity e cross the orbit of Earth and are included in the distribution. The two peaks in the distribution of incoming direction are a result of the impacting bodies being equally likely to hit Earth on the incoming or outgoing trajectories.
Paper: A Collision Mechanism for the Removal of Earth's Trojan Asteroids
Authors: Kevin J. Napier, Larissa Markwardt, Fred C. Adams, David W. Gerdes, Hsing Wen Lin, 省文 林
Figure caption: Scatter plot of the fraction of the initial population of 3021 ETs that ended the simulation in a Trojan (top) or a horseshoe (bottom) orbit, plotted as a function of the net linear momentum of the impactors. The panels on the right-hand side are histograms representing the probability with which a given fraction of coorbitals was retained. The fraction of objects remaining in coorbitals decreases as the net linear momentum of the impactors increases. Note that the vertical axis is linear in the range [0, 0.1] and logarithmic in the range [0.1, 1].
Paper: A Collision Mechanism for the Removal of Earth's Trojan Asteroids
Authors: Kevin J. Napier, Larissa Markwardt, Fred C. Adams, David W. Gerdes, Hsing Wen Lin, 省文 林
Figure caption: Box-and-whisker plots of the fraction of the initial population of 3021 ETs that ended the simulation in a Trojan (top) or a horseshoe (bottom) orbit, plotted as a function of the number of impactors. There are data points that exceed the vertical range we have chosen for these plots, but such events are relatively rare.
Paper: A Collision Mechanism for the Removal of Earth's Trojan Asteroids
Authors: Kevin J. Napier, Larissa Markwardt, Fred C. Adams, David W. Gerdes, Hsing Wen Lin, 省文 林
Figure caption: Our synthetic population projected into the ecliptic plane (left) and viewed from a higher inclination (right). The large cyan circle represents Earth, the large yellow circle represents the Sun, and the test particles are represented by smaller circles with colors corresponding to their inclinations (blue represents low inclination, and red represents high inclination, maxing out at approximately 40°).
Paper: New Polarimetric Data for the Galilean Satellites: Europa Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: The phase-angle dependence of polarization for Europa in the UBVR I filters obtained in 2018–2021 (black circles) and in 2000 (Rosenbush & Kiselev 2005; red circles). The fit to the BVRI data showed by the solid curve consists of two parts: an approximation of data within the range of phase angles from 0° to ∼3° and in the phase-angle range from approximately 3° to 12° using polynomials of the third and second degree, respectively.
Paper: New Polarimetric Data for the Galilean Satellites: Europa Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: The phase-angle dependence of polarization for leading (0° < L < 180°; filled circles) and trailing (180° < L < 360°; open circles) hemispheres of Europa in the V, R, and I bands (left, middle, and right, respectively). The black lines are the linear fit to the trailing hemisphere data.
Paper: New Polarimetric Data for the Galilean Satellites: Europa Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: Example of the phase-angle dependence of normalized Stokes parameters q  r  and u  r  for Europa in the V filter. The scatter of u  r  values around zero characterizes the real observation errors.
Paper: New Polarimetric Data for the Galilean Satellites: Europa Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: (a) Shifting the inversion point with increase of kl. (b) The best fit to the observational data in the R filter.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the average velocity distribution (in kilometers per second) of meteoroids into the Martian atmosphere determined by the MIF model for the JFCs (a, b, and c), the ASTs (d, e, and f), and the HTCs (g, h, and i) and three orbital positions: aphelion (L s = 71°, top panels), perihelion (L s = 251°, middle panels), and first crossing of the ecliptic plane (L s = 325°, bottom panels). These distributions are represented as a function of the Local True Solar Time and the latitude on Mars. Note that the color scales are different for each meteoroid population.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the average diameter distribution (in microns) of meteoroids into the Martian atmosphere determined by the MIF model for the JFCs (a, b, and c), the ASTs (d, e, and f), and the HTCs (g, h, and i) and three orbital positions: aphelion (L s = 71°, top panels), perihelion (L s = 251°, middle panels), and first crossing of the ecliptic plane (L s = 325°, bottom panels). These distributions are represented as a function of the Local True Solar Time and the latitude on Mars. Note that the color scales are different for each meteoroid population.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diagram illustrating the variability of the total mass influx and the total ablated mass with the orbital position (L s). The maximum global mass input occurs between L s = 270° (northern winter/southern summer) and L s = 325° (first crossing of the ecliptic plane), whereas the maximum deposition of metals in the Martian atmosphere matches with the maximum mass input of HTCs at perihelion (L s = 251°). Note that the mass fluxes are expressed in tons sol−1 (1 solar day at Mars is equivalent to 1.0275 Earth days). The values in parenthesis represent the fraction ablated with respect to the total mass input.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Normalized radiant distributions of meteoroid fluxes in Mars’ orbit predicted by the DMZC for three populations: the JFCs (a, b, and c), the ASTs (d, e, and f), and the HTCs (g, h, and i), and three orbital positions: aphelion (L s = 71°, top panels), perihelion (L s = 251°, middle panels), and first crossing of the ecliptic plane (L s = 325°, bottom panels). The abscissa axis represents the ecliptic longitude, λ, corrected by the subsolar terminator (a = λ − λ 0 = 0° at 12 hr), and the ordinate axis b is the latitude measured from the orbital plane of Mars.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Average velocity distributions (in kilometers per second) of meteoroids in Mars’ orbit predicted by the DMZC from the JFCs (a and b), the ASTs (c and d), and the HTCs (e and f), and two particle diameters: D = 50 μm (top panels) and D = 1000 μm (bottom panels). The abscissa axis represents the ecliptic longitude, λ, corrected by the subsolar terminator (a = λ − λ 0 = 0° at 12 hr), and the ordinate axis b is the latitude measured from the orbital plane of Mars. In the case of the JFCs and HTCs, the average velocity distribution for a given particle size does not change significantly with the orbital position and, therefore, these panels only show the corresponding results at perihelion (L s = 251°). Note that the color scales are different for each meteoroid population.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Altitude (in kilometers) of the ablation peak of Na predicted by the CABMOD model as a function of the initial diameter and entry velocity of the meteor, and a fixed zenith angle (ZA) of 45°. Figure 6(a) shows the altitude peaks for a latitude of −90° and a solar longitude L s = 90° (northern summer/southern winter), and Figure 6(b) represents a planetographic latitude of 60° and a solar longitude L s = 270° (northern winter/southern summer). The area shaded in dark blue represents all those particles that do not reach the melting temperature of 1800 K. The wavy structure of the contours is an artifact caused by the discretization of the particle size distribution.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Normalized velocity distributions in Mars’ orbit for the JFCs (a), the ASTs (b), and the HTCs (c) at perihelion (L s = 251°). The color profiles show the results for all of those diameters modeled by the DMZC. The solid-black line also represents the normalized overall flux for each meteoroid population as a function of the impact velocity. Note that both the profiles of the velocity distributions for the different particle sizes and the overall flux are normalized to an area equal to the unity.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Three-isotope plot of N2/36Ar vs. 132Xe/36Ar of the experimental cometary ices considering a solar-like starting composition and various temperatures of formation. Cosmochemical end-members are the same as in Figure 6. Squares represent the average of the repeated experiments (shown as diamonds) for a given temperature of deposition. Error bars represent the standard error of the repeated experiments at 1σ. The line between the symbols is for visual aid only. A similar detailed plot for 84Kr/36Ar vs. 132Xe/36Ar is given in Appendix Figure A6.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Experiments of H2O:N2:Ar:Kr:Xe mixtures deposited on the cold plate at 40, 50, 60, 70, and 80 K, respectively, and warmed up at 190 K. When the temperature of deposition increases, the amount of gas trapped and released around 140 K decreases. The background level of H2O and N2 is higher for experiments at 50 and 70 K before the filament of the QMS was replaced. This did not affect the enrichment ratio values given in Table 1.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Plot of 84Kr/36Ar vs. 132Xe/36Ar with several notable cosmochemical end-members: Solar (Lodders 2003; Meshik et al. 2014), CC gray box (range of the carbonaceous chondrite compositions; compilation from Bekaert et al. 2020), 67P/C-G (Rubin et al. 2018), and Early Atm (initial Earth atmospheric composition before Xe loss; Zahnle et al. 2018). Diamonds show the composition of experimental cometary ices if formed from a solar composition at various temperatures of formation. Squares are the average obtained for each temperature of deposition. Error bars represent the standard error of the repeated experiments for one temperature of formation at 1σ. Lines between symbols are for visual aid only.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: The circles show the evolution of the total gas pressure in the experimental volume as a function of temperature during the warm-up of the ice, measured by the ion gauge positioned before the QMS (Figure 1). The ice was formed at 28 K with an identical experimental procedure as the data shown in Figure 4. The slightly transparent colored curves are the intensities of H2O, N2, Ar, Kr, and Xe measured on the QMS (displayed as an ion current) during the experiment at 28 K presented in Figure 4.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: The N2 and noble gas release during the heating from 28 to 200 K at a rate of 1  K minute−1 in two experiments deposited (i) with water (similar to Figure 3; solid lines) and (ii) without water (dashed lines). In the experiment without water, the sublimation temperatures of N2, Ar, Kr, and Xe are shifted toward lower temperatures.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Wavelength distribution of the Hamamatsu H2D2 UV lamp (model L11798, MgF2 window) with a flux of around 1015 photons s–1 (Sebree et al. 2018).
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Drawing of the cryogenic trap designed for the EXCITING project, provided by Cryoscan©. This design is proprietary of Cryoscan©.