adsabs/AstroCLIMB huggingface dataset:
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Band I center vs. band II center for diogenite NWA 4664 and eucrites NWA 7266 and NWA 8563. The increase in shock darkening (SD) is represented as an increase in the opacity of the symbols. Measured band centers for orthopyroxenes (<11% Wo) and clinopyroxenes (>11% Wo) from J. B. Adams (1974) and E. A. Cloutis & M. J. Gaffey (1991) are also shown.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: PC2’ vs. PC1’ diagram from F. E. DeMeo et al. (2009). PC values calculated for diogenite NWA 4664 and eucrites NWA 7266 and NWA 8563 corresponding to different fractions of shock darkening (SD) are depicted with different symbols. The increase in SD is represented as an increase in the opacity of the symbols. The arrow indicates the direction in which shock darkening increases.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Top: reflectance measured at 0.55 μm and spectral slope vs. fraction of shock darkening for eucrite NWA 7266. Bottom: band I and II depths vs. fraction of shock darkening. Uncertainties are smaller than the symbols.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Left: spectra of eucrite NWA 8563 corresponding to the light-brown clast and clasts plus shock darkening (SD) from the dark matrix material. Right: the same spectra normalized to unity at 1.5 μm.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Spectrum of diogenite NWA 4664 compared to the spectrum of eucrite NWA 7266 corresponding to 50% shock darkening (SD).
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: Histograms of the NEB, EZ, and SEB comparing the variations in brightness temperature between the VLA and MWR measurements, where the brightness temperatures are plotted as percent difference from Equation (1). Normal distributions for each are shown, and the mean and standard deviation for each distribution are summarized in Table 5.
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: VLA maps showing the locations of the strongest positive and negative brightness temperature anomalies within the NEB, EZ, and SEB. The grayscale VLA maps are the same as Figure 4. Locations of warm brightness temperature anomaly are shown in red and represent the top 5% of anomalies. The negative brightness temperature anomalies are shown in blue and represent the bottom 5% of values. Darker colors for both indicate more extreme brightness temperatures. Unlike Figure 6, the anomalies were zonally detrended, as opposed to one Tb,mean per zone or belt as we did for Figure 6.
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: The leftmost panel shows the mean vertical ammonia profile for each latitude region, as indicated in the legend. The weighting functions in the rightmost four panels are based on the averaged ammonia abundance distributions for the given latitude regions from C. Moeckel et al. (2023). The central three panels show the weighting functions for MWR C4, C5, and C6. The rightmost panel shows the weighting function for the VLA frequency bands used, based on the average tropical distribution between −20° and 17° latitude. The shading indicates the impact of the wider VLA frequencies.
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: VLA maps of Jupiter with C, X, Ku, and K bands taken in 2013–2014 from I. de Pater et al. (2016, 2019b) and additional X band data from 2016 from C. Moeckel et al. (2023), as labeled. All maps are shown between ±45° planetographic latitude, and all had a limb-darkened disk added back in to show the absolute brightness temperature distribution. The color bar represents the brightness temperature of the maps in units of Kelvin. The resolution ellipse for each map is shown at the equator in black within a black box. We refer the reader to I. de Pater et al. (2016) to compare with semiconcurrent visible images.
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: VLA C band 2014 map showing artifact correction with an 80 pixel Gaussian filter (left) and K band 2014 map showing correction with a 40 pixel Gaussian filter (right).
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: VLA Ku band 2013 map showing artifact correction with a 65 pixel Gaussian filter.
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: VLA X band 2014 map showing artifact correction with an 80 pixel Gaussian filter (left) and X band 2016 map showing correction with a 120 pixel Gaussian filter (right).
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: Shallow-water CA calculations of the three identified regimes. Left: initial PV contours after stretching for 4 sols (red contours) and instantaneous PV for the same time (grayscale shading); the stereographic map shows latitudes from 50° to the pole. Right: stretching rates (solid; left y-axis scale) and PV (dashed; right y-axis scale), for a stable annulus (a), (b), unstable annulus (c), (d), and monopolar vortex (e), (f). The PV values are scaled by the quantity 2Ω/H (Ω is the rotation rate of the shallow-water model, and H is an imposed mean layer depth) to produce a unitless PV value that is comparable across different setups. Here a dip in stretching rates on the right is seen as a more circular contour on the left, denoting the location of the mixing barrier at the edge of the vortex.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: PlanetWRF scaled PV (1 PVU = 10−5 K m2 kg−1 s−1; fill) and zonal wind (in meters per second; black contours) averaged over 10 sols around the northern winter solstice (LS = 267° −272°) for simulations representing an annular vortex (a), (c) and a monopolar vortex (b), (d). Panels (a), (b): maps at the 300 K isentropic surface, extending from the pole to 40°N. Panels (c), (d): zonal averages; gray dashed contours are pressure surfaces in hectopascals.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: Modified annulus relaxation profiles used for Figure 3. Here qp is the initial latitudinal PV profile function, and the plot shows the unmodified PV structure of the stable annulus from Figures 1(a) and (b) (solid), the deepened annulus (dashed), the weakened annulus (dotted), and the shifted annulus (dashed–dotted), with φ1 and φ2 being the new latitudinal edges of the shifted annulus. As in Figure 1, the quantity 2Ω/H is a scaling factor to produce a unitless PV value that allows comparison of the PV across different setups.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: CA stretching rates (solid lines) and PV (dashed lines) averaged over the entire 90 sol calculation period for the 300, 400, and 500 K isentropic surfaces. Note that both vortices show a dip in stretching rates along the steepest latitudinal gradient of the PV. Also of note, the annular polar vortex becomes more monopolar with height, and the stretching rates become more similar between the two cases as well.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: Shallow-water tracer simulations for the three previously identified scenarios after 90 sols, with initial tracer distribution north of 80° to the pole. Maps show a latitudinal range from 20° to the pole (90°). Note that in all cases the tracer is unable to escape the confines of the region of high PV, indicating the isolation of the polar region from the midlatitudes on the interior of the polar vortex edge.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: Similar to Figure 1, except for three perturbed relaxation profiles: deepened annulus (a), (b), shallow annulus (c), (d), and shifted annulus (e), (f).
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: L’TES data binned into 10 spectra (crosses), ATPM heterogeneous surface model fits and corresponding uncertainty region (blue lines and shaded areas), and the single-temperature blackbody fit to the data (red lines).
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: The variation of Qd as a function of grain velocity and particle size is shown for particles ranging from 1 μm to 1 mm and dust ejection velocities between vd = 0 and 300 m s−1 for 327P/Van Ness.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: A(0°)fρ projected to 2 au against the perihelion distance for each JFC that has a measurable n in the 4 yr ATLAS sample. Orange points show the JFC’s projected A(0°)fρ at 2 au, and green points show the projected A(0°)fρ at 2 au post-perihelion. The red dashed line links the observations of the same JFC pre-perihelion to post-perihelion, where both measurements were made.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: Maximum A(0°)fρ vs. days from perihelion for each JFC. The green vertical line represents the perihelion for each individual comet, and the plot is color-coded according to orbital eccentricity.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: Maximum A(0°)fρ vs. time from perihelion as a function of orbital period for each JFC. The green vertical line represents the perihelion for each individual comet, and the plot is color-coded according to perihelion distance.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: JFC maximum activity as a function of heliocentric distance. The green dashed line indicates the corresponding A(0°)fρ for m(o) = 18.5 at opposition, necessary for clear detection of a coma. The absence of measured JFCs below this line is consistent with ATLAS sensitivity. The blue dashed line shows the H2O sublimation rate as a function of heliocentric distance.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: Comparison between our 67P o-band magnitudes transformed to r(PS1) and those obtained by D. Gardener et al. (2022). Good agreement is seen pre-perihelion until MJD ∼ 59500 and post-perihelion after MJD ∼ 59650.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: JFCs reaching perihelion in 2022 and 2023 that were visible to ATLAS. The blue stars represent the perihelion of each comet, pink represents the pre-perihelion Rh observed range by ATLAS, and black represents the post-perihelion Rh observed range by ATLAS.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: Panel (a) shows the activity index, n, for the JFC subset pre-perihelion. Panel (b) shows n for JFCs post-perihelion/post-max. Binned to Δn = 3.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: A(0°)fρ for comets 444P/WISE-PANSTARRS and 459P/Catalina during pre-perihelion dates when we obtained constant A(0°)fρ measurements within the measurement uncertainties. 444P/WISE-PANSTARRS is shown from Rh = 1.84 to 1.53 au, and 459P/Catalina is shown from Rh = 2.27 to 1.50 au. Orange and cyan points represent the ATLAS o band and c band, respectively.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: The transmission curves for the ATLAS c and o filters are shown in cyan and orange, respectively. A template comet spectrum with template gas abundances is plotted in black, with the molecular emissions labeled above each feature in the spectrum.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: Terminator orbits originating from L2 in the augmented CRTBP model for spherical ejecta with different radii. The combined mass of Didymos and Dimorphos is located at the origin of the secondary-centered synodic frame. From left to right, the subplots correspond to ejecta radii of 1 m, 10 cm, 1 cm, and 1 mm. Note that a smaller ejecta radius corresponds to a higher SRP acceleration of the ejecta.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: Planar Lyapunov orbits originating from L2 in the augmented Sun–Didymos and Dimorphos CRTBP model for spherical ejecta with different radii. The combined mass of Didymos and Dimorphos is located at the origin of the secondary-centered synodic frame. From left to right, the subplots correspond to ejecta radii of 1 m, 10 cm, 1 cm, and 1 mm. Note that a smaller ejecta radius corresponds to a higher SRP acceleration of the ejecta.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: The distribution of ejection velocity, angle, and location for ejecta following the stable manifold of the planar Lyapunov orbits and impacting the surface of (a) Didymos and (b) Dimorphos.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: The longitude distribution for ejecta following the stable manifold of the planar Lyapunov orbits and impacting the surface of (a) Didymos and (b) Dimorphos.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: An example of a backward-propagated ejecta trajectory along the stable manifold of a planar Lyapunov orbit eventually impacting Dimorphos. (a) Trajectory in the Didymos-centered synodic frame. (b) Trajectory in the Dimorphos-centered body-fixed frame.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: An example of a backward-propagated ejecta trajectory along the stable manifold of a planar Lyapunov orbit eventually impacting Didymos. (a) Trajectory in the Didymos-centered synodic frame. (b) Trajectory in the Didymos-centered body-fixed frame.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: The distribution of ejection velocity, angle, and latitude for ejecta following the stable manifold of the terminator orbits and impacting the surface of (a) Didymos and (b) Dimorphos.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: Stable (blue) and unstable (pink) manifolds emerging from an L2 planar Lyapunov orbit and directing to the secondary. Both manifolds emerge from the candidate orbit and intersect with a secondary-centered sphere of 4 km radius.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: The distribution of ejection location for ejecta following the stable manifold of the terminator orbits and impacting the surface of (a) Didymos and (b) Dimorphos.