adsabs/AstroCLIMB huggingface dataset:
Paper: Pre-encounter Predictions of DART Impact Ejecta Behavior and Observability
Authors: Eugene G. Fahnestock, Andrew F. Cheng, Stavro Ivanovski, Patrick Michel, Sabina D. Raducan, Alessandro Rossi, Paul A. Abell, Steven Chesley, Elisabetta Dotto, Fabio Ferrari, Ludmilla Kolokolova, Emily Kramer, Jian-Yang Li, Stephen R. Schwartz, Stefania Soldini, Gonzalo Tancredi, Adriano Campo Bagatin, Yun Zhang
Figure caption: Radial profiles of mean magnitude per pixel averaged within the annuli defined for Figure 7 over all angular positions going around each annulus. The horizontal axes are actually giving the pixel distance r from the target (Dimorphos) of the inner edge of the 10 pixel wide annuli. For panel (a), the lines are for 1 hr increments from t = 1 (darkest blue) to 24 (darkest red) hr, while for panel (b), the lines are for 1 day increments from t = 24 hr = 1 day (darkest blue) to 20 days (darkest red).
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Yield surfaces: Drucker–Prager & Lundborg with limiting strengths of 1 GPa and 10 GPa, 1.4 kPa cohesion, and a coefficient of friction of 0.77. The Lundborg curves asymptote to the limiting strength.
Paper: Pre-encounter Predictions of DART Impact Ejecta Behavior and Observability
Authors: Eugene G. Fahnestock, Andrew F. Cheng, Stavro Ivanovski, Patrick Michel, Sabina D. Raducan, Alessandro Rossi, Paul A. Abell, Steven Chesley, Elisabetta Dotto, Fabio Ferrari, Ludmilla Kolokolova, Emily Kramer, Jian-Yang Li, Stephen R. Schwartz, Stefania Soldini, Gonzalo Tancredi, Adriano Campo Bagatin, Yun Zhang
Figure caption: Angular profiles of mean magnitude per pixel going from north toward east (i.e., counterclockwise from up) in the no-PSF-applied images of (a) Figure 6(a) and (b) Figure 6(c). Each line is for a different annulus formed by pixels within the range of pixel distance r from the target (Dimorphos) indicated by the legend. The horizontal axes are in degrees, and the angular bins averaged over are 5° wide.
Paper: Pre-encounter Predictions of DART Impact Ejecta Behavior and Observability
Authors: Eugene G. Fahnestock, Andrew F. Cheng, Stavro Ivanovski, Patrick Michel, Sabina D. Raducan, Alessandro Rossi, Paul A. Abell, Steven Chesley, Elisabetta Dotto, Fabio Ferrari, Ludmilla Kolokolova, Emily Kramer, Jian-Yang Li, Stephen R. Schwartz, Stefania Soldini, Gonzalo Tancredi, Adriano Campo Bagatin, Yun Zhang
Figure caption: Radial profiles of mean magnitude per pixel, created the same way as for Figure 8 but for two specific times plotted within Figure 8(a) and now comparing the nominal versus off-nominal cases having different total masses of ejecta and cSFD power-law slopes as specified in Table 2.
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Crush Curves. We compare the crushing behavior for the same regolith material using two different compaction models: ε–α compaction model (iSALE) and P–α compaction model (both SPH codes). For comparison, we add the crush curves for lunar microbreccia and lunar dust (Stephens & Lilley 1970). The left panel shows the pressure–distension relation, and the right panel shows the same for a normalized distension.
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Experimental setup (a) and example high-speed images for regolith simulant (b) as illustrated by Chourey et al. (2020) in their Figures 2 & 10.
Paper: Practical Stereophotoclinometry for Modeling Shape and Topography on Planetary Missions
Authors: Eric E. Palmer, Robert Gaskell, Michael G. Daly, Olivier S. Barnouin, Coralie D. Adam, Dante S. Lauretta
Figure caption: Ingestion of new images into SPC. (a) Images are converted into a simple binary 2D array of unsigned short integers, and the geometric reference system of the images is converted into a body-fixed frame. (b) The images are aligned with the existing DTM. (c) Previously existing maplets are associated with the images.
Paper: Practical Stereophotoclinometry for Modeling Shape and Topography on Planetary Missions
Authors: Eric E. Palmer, Robert Gaskell, Michael G. Daly, Olivier S. Barnouin, Coralie D. Adam, Dante S. Lauretta
Figure caption: High-level view of the stages of building a DTM using SPC. A starting DTM and an estimate for the object’s rotation rate and pole (i.e., planetary constants) are required. The starting DTM is improved using limb vectors during the spacecraft’s approach to the target. Once the target fills the field of view, maplet-base modeling is better. First, SPC covers (or tiles) the surface with small 2D maplets and extracts topography from the position and shading of the images. Second, new images are added to the system, allowing higher-resolution data to improve the DTM. These two processes are repeated until the model reaches the desired GSD.
Paper: Practical Stereophotoclinometry for Modeling Shape and Topography on Planetary Missions
Authors: Eric E. Palmer, Robert Gaskell, Michael G. Daly, Olivier S. Barnouin, Coralie D. Adam, Dante S. Lauretta
Figure caption: During maplet-based modeling, the surface is covered with small maplets. The image on the left shows the starting state of a global set of maplets with only the most basic generation of topography (see Section 3.4.2). As the data are processed and the DN information is converted into a consistent topographic solution, the maplets’ topography changes to reflect the surface of the target. Eventually, the maplets will curve and make a closed and consistent object from which the data are resampled to make a global DTM.
Paper: Practical Stereophotoclinometry for Modeling Shape and Topography on Planetary Missions
Authors: Eric E. Palmer, Robert Gaskell, Michael G. Daly, Olivier S. Barnouin, Coralie D. Adam, Dante S. Lauretta
Figure caption: Actual navigation alignment offset for asteroid Lutetia, image N332048572, using reconstructed SPICE kernels. The real image is colored red. The rendered DTM image is colored cyan. When the actual image and the DTM agree, the alignment image is gray to gray-pink. We can easily identify a camera position/pointing shift that is required. Also, it allows interpretation of variations in overall size and large surface features. If there are deviations between the models, they can be seen as distinct shifts of features between the two channels.
Paper: Practical Stereophotoclinometry for Modeling Shape and Topography on Planetary Missions
Authors: Eric E. Palmer, Robert Gaskell, Michael G. Daly, Olivier S. Barnouin, Coralie D. Adam, Dante S. Lauretta
Figure caption: Generation of a DTM via limb-based modeling using data obtained during approach to the target. Once the images are incorporated (converted into an SPC-compatible format) and aligned to the existing DTM, the limbs are extracted. The limbs are combined as a point cloud to construct an updated model. Translation tools convert or combine the point cloud of vertices to a DTM [VECS2SHAPE/VECS2CUBE].
Paper: Practical Stereophotoclinometry for Modeling Shape and Topography on Planetary Missions
Authors: Eric E. Palmer, Robert Gaskell, Michael G. Daly, Olivier S. Barnouin, Coralie D. Adam, Dante S. Lauretta
Figure caption: AES is the multistep process of extracting the DN values from the images to correct the DTM by comparing them with the rendered model’s DN values. Each step improves the topography and albedo, which results in a more accurate representation of each model subimage. An example subimage pair is shown in Figure 7. These steps are all accomplished in the module called LITHOS.
Paper: Heliocentric Effects of the DART Mission on the (65803) Didymos Binary Asteroid System
Authors: Rahil Makadia, Sabina D. Raducan, Eugene G. Fahnestock, Siegfried Eggl
Figure caption: The B-plane deflections for varying values of β ⊙ showing a linear increase in deflection magnitude with increasing heliocentric momentum enhancement parameters for the (a) 2062 October 20 and (b) 2123 November 4 close approaches.
Paper: Heliocentric Effects of the DART Mission on the (65803) Didymos Binary Asteroid System
Authors: Rahil Makadia, Sabina D. Raducan, Eugene G. Fahnestock, Siegfried Eggl
Figure caption: The B-plane deflections and associated uncertainty ellipses for a dynamical model that includes the Yarkovsky effect (colored) and one that does not (gray scale) for the (a) 2062 October 20 and (b) 2123 November 4 close approaches.
Paper: Arecibo Planetary Radar Observations of Near-Earth Asteroids: 2017 December–2019 December
Authors: Anne K. Virkki, Sean E. Marshall, Flaviane C. F. Venditti, Luisa F. Zambrano-Marín, Dylan C. Hickson, Anna McGilvray, Patrick A. Taylor, Edgard G. Rivera-Valentín, Maxime Devogèle, Eframir Franco Díaz, Sriram S. Bhiravarasu, Betzaida Aponte Hernández, Carolina Rodriguez Sánchez-Vahamonde, Michael C. Nolan, Phil Perillat, Israel Cabrera, Elliot González, Daniel Padilla, Victor Negrón, Juan Marrero, Johbany Lebrón, Adrian Bagué, Francisco Jiménez, Andy López-Oquendo, Daniel Repp, Riley A. McGlasson, Brynn Presler-Marshall, Ellen S. Howell, Jean-Luc Margot, Sanjana Prabhu Desai
Figure caption: As Figure 3.
Paper: Arecibo Planetary Radar Observations of Near-Earth Asteroids: 2017 December–2019 December
Authors: Anne K. Virkki, Sean E. Marshall, Flaviane C. F. Venditti, Luisa F. Zambrano-Marín, Dylan C. Hickson, Anna McGilvray, Patrick A. Taylor, Edgard G. Rivera-Valentín, Maxime Devogèle, Eframir Franco Díaz, Sriram S. Bhiravarasu, Betzaida Aponte Hernández, Carolina Rodriguez Sánchez-Vahamonde, Michael C. Nolan, Phil Perillat, Israel Cabrera, Elliot González, Daniel Padilla, Victor Negrón, Juan Marrero, Johbany Lebrón, Adrian Bagué, Francisco Jiménez, Andy López-Oquendo, Daniel Repp, Riley A. McGlasson, Brynn Presler-Marshall, Ellen S. Howell, Jean-Luc Margot, Sanjana Prabhu Desai
Figure caption: The delay-Doppler images with the vertical × horizontal resolution. The range (delay) increases from top to bottom, and the Doppler frequency increases from left to right, i.e., the right-hand side is approaching, while the left-hand side is receding. Pixel values are in units of standard deviations above the noise baseline (i.e., linear z-scores). The color map is clipped such that z-scores <0 map to black while white represents values higher than the 95th percentile. The images are available in FITS format through Figshare (Virkki et al. 2022).
Paper: Arecibo Planetary Radar Observations of Near-Earth Asteroids: 2017 December–2019 December
Authors: Anne K. Virkki, Sean E. Marshall, Flaviane C. F. Venditti, Luisa F. Zambrano-Marín, Dylan C. Hickson, Anna McGilvray, Patrick A. Taylor, Edgard G. Rivera-Valentín, Maxime Devogèle, Eframir Franco Díaz, Sriram S. Bhiravarasu, Betzaida Aponte Hernández, Carolina Rodriguez Sánchez-Vahamonde, Michael C. Nolan, Phil Perillat, Israel Cabrera, Elliot González, Daniel Padilla, Victor Negrón, Juan Marrero, Johbany Lebrón, Adrian Bagué, Francisco Jiménez, Andy López-Oquendo, Daniel Repp, Riley A. McGlasson, Brynn Presler-Marshall, Ellen S. Howell, Jean-Luc Margot, Sanjana Prabhu Desai
Figure caption: The distribution of OC radar albedos and optical geometric albedos of 41 NEAs: 37 as presented in Section 4 in addition to the radar and geometric albedos as published for (433) Eros (Magri et al. 2001), (1981) Midas (McGlasson et al. 2022), (2100) Ra-Shalom (Shepard et al. 2008b), and (3200) Phaethon (Taylor et al. 2019a). The taxonomic type is indicated when known or using a question mark when unknown or questionable. The mean OC radar albedos for S + Q- and C-type NEAs with 1σ standard deviations is 0.19 ± 0.06 (11 NEAs) and 0.06 ± 0.05 (4 NEAs), respectively, while the global average for 41 NEAs was 0.21 ± 0.11. The number of NEAs that are V types, X complex, or L/Ld types is too low to provide statistical significance. The relative uncertainty for the radar albedo of Midas is estimated at ∼40% using a shape model (McGlasson et al. 2022); therefore, the radar albedos of the other less-constrained cases are estimated to be at least 50%.
Paper: Arecibo Planetary Radar Observations of Near-Earth Asteroids: 2017 December–2019 December
Authors: Anne K. Virkki, Sean E. Marshall, Flaviane C. F. Venditti, Luisa F. Zambrano-Marín, Dylan C. Hickson, Anna McGilvray, Patrick A. Taylor, Edgard G. Rivera-Valentín, Maxime Devogèle, Eframir Franco Díaz, Sriram S. Bhiravarasu, Betzaida Aponte Hernández, Carolina Rodriguez Sánchez-Vahamonde, Michael C. Nolan, Phil Perillat, Israel Cabrera, Elliot González, Daniel Padilla, Victor Negrón, Juan Marrero, Johbany Lebrón, Adrian Bagué, Francisco Jiménez, Andy López-Oquendo, Daniel Repp, Riley A. McGlasson, Brynn Presler-Marshall, Ellen S. Howell, Jean-Luc Margot, Sanjana Prabhu Desai
Figure caption: Example of Doppler-bandwidth determination from the Doppler-echo-power spectra for (3753) Camillo and 2013 CW32. The panels on the top show the echo-power standard deviations per frequency bin with “smoothing” (see the text for definition), and the panels on the bottom show the cumulative echo power (standard deviations, as a “function” of frequency) for the same asteroids without smoothing. All Doppler bandwidths were determined by eye using plots such as the panels on the bottom. The outlying “tails” in the Doppler spectrum in the top-right panel are likely due to smoothing. This illustrates why the bandwidths are determined using unsmoothed spectra.
Paper: Arecibo Planetary Radar Observations of Near-Earth Asteroids: 2017 December–2019 December
Authors: Anne K. Virkki, Sean E. Marshall, Flaviane C. F. Venditti, Luisa F. Zambrano-Marín, Dylan C. Hickson, Anna McGilvray, Patrick A. Taylor, Edgard G. Rivera-Valentín, Maxime Devogèle, Eframir Franco Díaz, Sriram S. Bhiravarasu, Betzaida Aponte Hernández, Carolina Rodriguez Sánchez-Vahamonde, Michael C. Nolan, Phil Perillat, Israel Cabrera, Elliot González, Daniel Padilla, Victor Negrón, Juan Marrero, Johbany Lebrón, Adrian Bagué, Francisco Jiménez, Andy López-Oquendo, Daniel Repp, Riley A. McGlasson, Brynn Presler-Marshall, Ellen S. Howell, Jean-Luc Margot, Sanjana Prabhu Desai
Figure caption: The echo-power spectra of 35 of the 37 NEAs selected for further analysis with the Doppler-frequency offset from the expected Doppler frequency on the horizontal axis and the z-scores of the echo power on the vertical axis. The solid line depicts the echo-power spectra in the OC polarization and the dashed line in the SC polarization. The time stamp depicts the midreceive time in UT to a precision of a minute.
Paper: Arecibo Planetary Radar Observations of Near-Earth Asteroids: 2017 December–2019 December
Authors: Anne K. Virkki, Sean E. Marshall, Flaviane C. F. Venditti, Luisa F. Zambrano-Marín, Dylan C. Hickson, Anna McGilvray, Patrick A. Taylor, Edgard G. Rivera-Valentín, Maxime Devogèle, Eframir Franco Díaz, Sriram S. Bhiravarasu, Betzaida Aponte Hernández, Carolina Rodriguez Sánchez-Vahamonde, Michael C. Nolan, Phil Perillat, Israel Cabrera, Elliot González, Daniel Padilla, Victor Negrón, Juan Marrero, Johbany Lebrón, Adrian Bagué, Francisco Jiménez, Andy López-Oquendo, Daniel Repp, Riley A. McGlasson, Brynn Presler-Marshall, Ellen S. Howell, Jean-Luc Margot, Sanjana Prabhu Desai
Figure caption: Average SC/OC ratios and absolute magnitudes of 112 NEAs with the taxonomic type indicated when known or a question mark when unknown or questionable. NEAs with unreliable SC polarization measurements (S/NSC ≤ 3.0) were omitted. The colored vertical bars on the left-hand side designate the means and 1σ standard deviations of the SC/OC ratios reported in this paper (Table 2), and the vertical bars on the right-hand side designate those reported in Benner et al. (2008) for the taxonomic types with at least five objects.
Paper: Heliocentric Effects of the DART Mission on the (65803) Didymos Binary Asteroid System
Authors: Rahil Makadia, Sabina D. Raducan, Eugene G. Fahnestock, Siegfried Eggl
Figure caption: (a) Total ejecta mass from DART-like impacts into asteroid surfaces with varying cohesion, Y 0, and coefficient of internal friction, f, and fixed porosity (ϕ 0 = 40%) from Bern SPH (Raducan & Jutzi 2022) and iSALE-2D (Raducan et al. 2019) simulations. The continuous lines show the total amount of ejecta mass that is ejected with velocities higher than the escape velocity of the Didymos system, whereas the dotted lines show the total amount of ejecta mass with velocities lower than the escape velocity of the Didymos system. (b) Momentum enhancement from DART-like impacts into asteroid surfaces with varying cohesion, Y 0, and coefficient of internal friction, f, and fixed porosity (ϕ 0 = 40%) from Bern SPH (Raducan & Jutzi 2022) and iSALE-2D (Raducan et al. 2019) simulations. The solid lines show the total momentum enhancement generated by the impact. The dotted lines show the heliocentric momentum enhancement (i.e., the total momentum of the ejecta that leaves the Didymos system).
Paper: Heliocentric Effects of the DART Mission on the (65803) Didymos Binary Asteroid System
Authors: Rahil Makadia, Sabina D. Raducan, Eugene G. Fahnestock, Siegfried Eggl
Figure caption: Summary of ejecta particles that escape the Didymos system. (a) Magnitude of the ejecta particles’ momenta at the time of crossing the Hill sphere, colored by the particle mass. (b) Cumulative ejecta contribution to the momentum enhancement parameter (β ⊙ − 1) as a function of time. The components are shown in the International Celestial Reference Frame Earth mean equator frame.
Paper: Heliocentric Effects of the DART Mission on the (65803) Didymos Binary Asteroid System
Authors: Rahil Makadia, Sabina D. Raducan, Eugene G. Fahnestock, Siegfried Eggl
Figure caption: Updated B-plane map for the 2123 November 4 Didymos–Earth close approach. (a) Didymos coordinates on the close approach B-plane shown to scale. (b) Didymos position uncertainty shown to scale on the B-plane for the nominal (no deflection) case, the DART spacecraft contribution only (β ⊙ = 1) case, a single impulse at the time of impact in case 1, and multiple impulses for each escaping ejecta particle in case 2. (c) Didymos position uncertainty zoomed in to show details on the B-plane for the nominal (no deflection) case, DART spacecraft contribution only (β ⊙ = 1) case, single impulse at the time of impact in case 1 (β ⊙ = 1.789), and multiple impulses for each escaping ejecta particle in case 2.
Paper: Heliocentric Effects of the DART Mission on the (65803) Didymos Binary Asteroid System
Authors: Rahil Makadia, Sabina D. Raducan, Eugene G. Fahnestock, Siegfried Eggl
Figure caption: Updated B-plane map for the 2062 October 20 Didymos–Earth close approach. (a) Didymos coordinates on the close approach B-plane shown to scale. (b) Didymos position uncertainty shown to scale on the B-plane for the nominal (no deflection) case, the DART spacecraft contribution only (β ⊙ = 1) case, a single impulse at the time of impact in case 1, and multiple impulses for each escaping ejecta particle in case 2. (c) Didymos position uncertainty zoomed in to show details on the B-plane for the nominal (no deflection) case, DART spacecraft contribution only (β ⊙ = 1) case, single impulse at the time of impact in case 1 (β ⊙ = 1.789), and multiple impulses for each escaping ejecta particle in case 2.
Paper: Heliocentric Effects of the DART Mission on the (65803) Didymos Binary Asteroid System
Authors: Rahil Makadia, Sabina D. Raducan, Eugene G. Fahnestock, Siegfried Eggl
Figure caption: Didymos–Earth close approach uncertainty ellipses for validating the new Gauss–Radau integrator accuracy against results from Chesley & Eggl (2018) during the (a) 2062 October 20 close approach and (b) 2123 November 4 close approach.
Paper: Effects of Impact and Target Parameters on the Results of a Kinetic Impactor: Predictions for the Double Asteroid Redirection Test (DART) Mission
Authors: Angela M. Stickle, Mallory E. DeCoster, Christoph Burger, Wendy K. Caldwell, Dawn Graninger, Kathryn M. Kumamoto, Robert Luther, Jens Ormö, Sabina Raducan, Emma Rainey, Christoph M. Schäfer, James D. Walker, Yun Zhang, Patrick Michel, J. Michael Owen, Olivier Barnouin, Andy F. Cheng, Sidney Chocron, Gareth S. Collins, Thomas M. Davison, Elisabetta Dotto, Fabio Ferrari, M. Isabel Herreros, Stavro L. Ivanovski, Martin Jutzi, Alice Lucchetti, Elena Martellato, Maurizio Pajola, Cathy S. Plesko, Megan Bruck Syal, Stephen R. Schwartz, Jessica M. Sunshine, Kai Wünnemann
Figure caption: Studies of the effects of projectile geometry suggested that using three offset spheres was a better representation of the DART impact than a single spherical projectile of equivalent mass. (Left) results for Spheral simulations showing deflection velocity (for the case of a relatively strong Dimorphos) as a function of the orientation angle of the impactor (shown on the right). The orientation angle is measured from the plane that is tangent to the target surface, where 90° details impactors in series and 0° details impactors aligned parallel to the target surface. A three-sphere representation was a much closer match to the predicted deflection velocity from the full spacecraft model than a single sphere impactor.
Paper: Effects of Impact and Target Parameters on the Results of a Kinetic Impactor: Predictions for the Double Asteroid Redirection Test (DART) Mission
Authors: Angela M. Stickle, Mallory E. DeCoster, Christoph Burger, Wendy K. Caldwell, Dawn Graninger, Kathryn M. Kumamoto, Robert Luther, Jens Ormö, Sabina Raducan, Emma Rainey, Christoph M. Schäfer, James D. Walker, Yun Zhang, Patrick Michel, J. Michael Owen, Olivier Barnouin, Andy F. Cheng, Sidney Chocron, Gareth S. Collins, Thomas M. Davison, Elisabetta Dotto, Fabio Ferrari, M. Isabel Herreros, Stavro L. Ivanovski, Martin Jutzi, Alice Lucchetti, Elena Martellato, Maurizio Pajola, Cathy S. Plesko, Megan Bruck Syal, Stephen R. Schwartz, Jessica M. Sunshine, Kai Wünnemann
Figure caption: Parallel-line plot showing the interaction of material strength parameters (fi, Yi0) and porosity (ϕ) on the momentum enhancement factor (β). Each line represents a single simulation and is colored by the calculated β. The thickness of the line is used as a visualization tool to allow multiple overlapping lines to be shown. The vertical axes show the material property inputs for each simulation: porosity (φ), coefficient of friction (fi), and material strength/cohesion (Yi0 (also called Y0 in some codes)). These three material parameters significantly affect momentum enhancement, but their relationship is complex, though general trends can be seen.