adsabs/AstroCLIMB huggingface dataset:
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Mixing ratio profiles with Earth data sources, demonstrating a new, comprehensive validation for our photochemical model. Our model has excellent agreement with global Earth data, using measured fluxes for key gases for the surface boundary condition. Here the photochemical model uses the average temperature from the data-derived 3D Spectral Earth model (Robinson et al. 2011). Calculated mixing ratio profiles of key species are shown with solid lines. For comparison, plotted are an average derived from the 3D Spectral Earth model (Robinson et al. 2011; dotted lines), measurements from Massie & Hunten (1981; dashed lines), the ICRCCM Earth midlatitude summer sounding case 62 (dashed–dotted lines), and data points for HCl (Ackerman et al. 1976), CH3Cl (Hu et al. 2010), and C2H6S (Seinfeld & Pandis 2006, Table 2.3).
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Theoretical transmission spectra (at 1 cm−1 resolution) of TRAPPIST-1 e with a modern-Earth-like atmosphere with increasing levels of CH3Cl enhancement. Error bars are shown for 50 transits with NIRSpec G395, which is sufficient for ﹩\left\langle {\rm{S}}/{\rm{N}}\right\rangle \approx 4.6﹩ on CH3Cl at 1000 × enhancement, and 100 transits with MIRI LRS, which is insufficient for the detection of CH3Cl despite the presence of a large absorption feature between 9 and 11 μm. Both simulated observations are binned to a resolving power of ﹩{ \mathcal R }=20﹩.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Theoretical transmission spectra (at 1 cm−1 resolution) of TRAPPIST-1 e with a cloudy modern-Earth-like atmosphere. In the top panel, error bars are shown for 100 transits with NIRSpec G140 (binned to a resolving power of ﹩{ \mathcal R }=40﹩), which is insufficient for O2 detection for TRAPPIST-1 e. In the bottom panel, error bars are shown for 100 transits with MIRI LRS (binned to a resolving power of ﹩{ \mathcal R }=20﹩), which is also insufficient for the detection of O3 at 9.6 μm. An S/N of 3 for O3 would require ~260 transits.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Left and middle: comparison of VPL Climate 1D temperature and H2O mixing ratio profiles with Earth retrieval data from 4/23/2008 in the VPL 3D Spectral Earth model (Robinson et al. 2011). Right: comparison of VPL Climate 1D eddy diffusion coefficient for mass with retrieved Earth values (Wofsy et al. 1972; Hunten 1975; Johnston et al. 1979; Allen et al. 1981; Massie & Hunten 1981; Patra & Lal 1997). The VPL Climate temperature and water vapor profiles are a good match to average Earth conditions, and the modeled eddy diffusion coefficient is within observed values.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The fraction of each NEA subpopulation (Atiras, Atens, Apollos, and Amors) from the MPC catalog as a function of absolute magnitude. The fractions for a value of absolute magnitude are cumulative, including all objects with values less than the value plotted. The effects of observational bias are clearly seen at H  V  > 24 mag.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The discovery epoch magnitude reported to the MPC for each NEA cataloged from 1970 to 2023. The yearly 80th percentile value of the discovery magnitude, m  V 80, is given as a red dashed line, with the blue dots representing the average value of the m  V 80 for each time period given in Table 2. The yellow lines represent the value of the magnitude used in the KOM from Table 2.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The comparison of the KOM using the NSS reference model with the known NEA population from the MPC at a range of absolute magnitude limits. The 10 random realizations of the NEA reference model were generated with a minimum effective diameter of 40 m.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The total discovery rate of NEAs per year is shown by a solid black line, with the yearly discovery rate of NEAs shown in different colored lines: PS (MPC sites F51 and 52) in solid blue and CSS (MPC sites 703 and G96) in solid red.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The discovery statistics over the last decade show that while the number of discoveries per year has risen regularly year over year, the fraction of objects with H  V  ≤ 23 mag has dropped by half from over half of the discoveries in 2011 to under a quarter of the discoveries in 2022.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The absolute magnitude distribution of 10 instances of the NEOS reference model for NEAs (solid gray lines) and the known population from the MPC catalog (solid red line) as of 2023 April.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The yearly NEA discovery rate from 2016 to 2022.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: A schematic showing the region in semimajor axis vs. eccentricity space of the four NEO subpopulations.
Paper: Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
Authors: David Polishook, Francesca E. DeMeo, Brian J. Burt, Cristina A. Thomas, Andrew S. Rivkin, Juan A. Sanchez, Vishnu Reddy
Figure caption: Top panel: seven near-IR reflectance spectra representing a daily measurement of the Didymos system. While all spectra have similar features, the immediate postimpact spectra (September 27 and 28) have spectra with lower spectral slopes (dark blue lines), compared to spectra from later dates (light purple lines) and the preimpact spectrum (September 26; red line). The colors representing the spectrum of each day remain fixed through the paper. Bottom panel: after removing the spectral slope using Equation (1), there is a good match between all seven reflectance spectra, suggesting that no change of material is present. The minimum value of a sixth-order fit to the 1 μm absorption band was used to normalized all spectra for display. We conclude that the slope variation is due to larger grains dominating the ejecta in the first ∼40 hr after the impact (see text for details).
Paper: Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
Authors: David Polishook, Francesca E. DeMeo, Brian J. Burt, Cristina A. Thomas, Andrew S. Rivkin, Juan A. Sanchez, Vishnu Reddy
Figure caption: Band analysis. Changes in four parameters with time (day 1 is September 26, and day 7 is 2022 October 2). Parameters are the 1 μm absorption band’s center and width (from 0.85 μm as described by DeMeo et al. 2014), the 1.5 μm height relative to the band I minima (also referred to as “potential depth” in DeMeo et al. 2014), and the 2 μm absorption band’s center. The left panels present the band analysis of the original spectra, where relatively larger changes can be measured on the nights immediately after the impact (September 27 and 28) compared to the preimpact spectrum and the later spectra. The right panels present the same parameters after the removal of the spectral slope (using the Brunetto et al. 2006 power-law “deweathering” equation; Equation (1)). The changes in the band parameters almost disappear, suggesting that the only parameter that changed during these nights is the spectral slope and not the other parameters that are affected by composition.
Paper: Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
Authors: David Polishook, Francesca E. DeMeo, Brian J. Burt, Cristina A. Thomas, Andrew S. Rivkin, Juan A. Sanchez, Vishnu Reddy
Figure caption: Pre- (September 26; red line) and post- (September 27; blue line) spectra of the Didymos system compared to the 1σ range (yellowish-orange bars) around averaged taxonomies (gray lines) of S- (top), Sq- (middle), and Q-types (bottom). The minimum value of a sixth-order fit to the 1 μm absorption band of the Didymos system spectra was normalized to the respective value of each of the taxonomies in order to ease the spectra comparison by using the 1 μm absorption band as an anchor. Both pre- and postimpact spectra match well to the S-type spectrum at the 1 μm absorption band and do not fit the Q-type reflectance spectrum, rejecting a hypothesis of an ejecta with fresh-looking material. The overall spectral slope of the preimpact spectrum fits well to the S-type spectrum; the same value of the postimpact spectrum better fits the S-type than the Sq- and Q-types.
Paper: Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
Authors: David Polishook, Francesca E. DeMeo, Brian J. Burt, Cristina A. Thomas, Andrew S. Rivkin, Juan A. Sanchez, Vishnu Reddy
Figure caption: Differences between the spectral slopes of the Chelyabinsk meteorite’s grains of different sizes relative to the spectral slope of grains of size 45–90 μm (left; black circles), compared to differences between the spectral slopes of the Didymos system after the DART impact relative to the spectral slope at preimpact (right, colored squares; same color scheme as in Figure 4). Both Y-axes are to scale, showing the similar range of spectral variation. The uncertainty is smaller than the markers' size.
Paper: Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
Authors: David Polishook, Francesca E. DeMeo, Brian J. Burt, Cristina A. Thomas, Andrew S. Rivkin, Juan A. Sanchez, Vishnu Reddy
Figure caption: PC2′–PC1′ plane with different taxonomy limits (DeMeo et al. 2009) and the values of the seven spectra (red circles, September 26; blue circles, September 27 and 28; purple circles, September 29 and 30, October 1 and 2). Colors are chosen as an indication of spectral slope: high (red), mid (purple), and low (blue). An inset panel presents a zoom-in plot with the dates of each spectra instead of the circles.
Paper: Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
Authors: David Polishook, Francesca E. DeMeo, Brian J. Burt, Cristina A. Thomas, Andrew S. Rivkin, Juan A. Sanchez, Vishnu Reddy
Figure caption: Reflectance spectra of each pair of images, or four images, taken on 2022 September 26 between 13:23 and 14:30 UT, that represent half of Didymos's rotation (thin colored lines). The combined reflectance spectrum of September 26 is also plotted (thick red dashed line; the same line appears in Figure 1). The postimpact reflectance spectrum (from September 27; thick blue dashed line) of the Didymos system is presented as a reference to a much smaller spectral slope. We found no variation within the scattering that is equivalent to the variation observed between the spectra  of September 27 and 28 and the rest of the spectra.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The inclination distribution of the objects cataloged by KOM up until the end of 2022 (red histogram), NEOS (blue histogram), and the two combined (black solid histogram). The distribution of objects identified as cataloged by KOM that are not observed by NEOS are shown as a yellow histogram. NEOS is found to be slightly more efficient at detecting and tracking the higher-inclination NEOS (i > ∼15°) than the current surveys.
Paper: Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
Authors: David Polishook, Francesca E. DeMeo, Brian J. Burt, Cristina A. Thomas, Andrew S. Rivkin, Juan A. Sanchez, Vishnu Reddy
Figure caption: Band analysis. Comparing the band I center, band II center, and BAR of meteorites of H-, L-, and LL-type ordinary chondrite to the Didymos system’s values measured by the IRTF. While the band I center and the BAR better fit the H- and L-types, the band II center better fits the L- and LL-types. Therefore, while the L-type is preferable, the result is inconclusive.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: A sequence of LUKE images where the ejecta cone can be seen in a face-on profile (ID 1), in a side-on profile (IDs 2 to 6), and transiting from a side-on profile to a view from behind (IDs 7 and 8). The images have been cropped to highlight the ejecta cone. The red lines in IDs 2 to 6 guide the eye through the edges of the projected cone. The edges serve for the measurement of the aperture angle of the projected cone 2δ. These angular measurements and some information about the images are given in Table 1. Except for ID 1, Dimorphos can be seen in other images with a shadow cast by the optically thick part of the ejecta cone. The very bright object in the corner of some of the images is Didymos, which is inside the crop.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Simulations of the ejecta cone using a cone with a circular base corresponding to LUKE observation IDs 1-6. The cone has an aperture angle of 122°, and its axis points to R.A., decl.: 136°,+5° in J2000. Several vectors are shown for reference: Red is the cone axis, gray is the incoming direction of the DART spacecraft, green is the north celestial pole, purple is the north pole of Didymos, and yellow is the direction of the Sun. Illumination effects and shadowing are not considered in this figure.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Context of the images from the LICIACube flyby of the Didymos system that are part of this analysis. The diagonal line is the trajectory of the LICIACube CubeSat as it flew by the Didymos system, and the exaggerated dots along this trajectory mark the instances of images 1 to 8, referred to in the Figure 2 and Table 1. Dimorphos is placed at the center of the J2000 coordinate system and is scaled up by a factor of 100 to improve its visibility. Panels (a), (b), and (c) show three orthogonal views of the flyby context in the XY, YZ, and XZ planes in J2000. The closest approach of LICIACube to Dimorphos took place at a distance of about 58 km, and this instance is given as a reference. The blue, red, and green axes correspond to the X,Y, and Z axes, respectively, in J2000.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: (a) Model of a cone with an elliptical base, described by two orthogonal half-angles η and γ, defined in the BAC plane and BAD plane, respectively. The cone axis points in the BA direction. (b) An example case of such a cone with η = 60° and γ = 30°, described by 33 vertices. The local Cartesian coordinate system is also defined, with the origin being at the apex. (c) The same cone with its cross section highlighted. Note that the cone axis points in the negative Z direction of the local cone coordinate system.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: A cone with a circular base and its projection onto a plane.
Paper: Unraveling the Geologic History of Miranda’s Inverness Corona
Authors: Erin J. Leonard, Chloe B. Beddingfield, Catherine M. Elder, Tom A. Nordheim
Figure caption: Previous maps of Inverness Corona from (A) Croft & Soderblom (1991), (B) Smith et al. (1986), and (C) Greenberg et al. (1991). (A) and (B) are portions of global geologic maps of Miranda, and thus do not map Miranda at the finest scale available. (C) is a portion of a global structural map of Miranda.
Paper: Unraveling the Geologic History of Miranda’s Inverness Corona
Authors: Erin J. Leonard, Chloe B. Beddingfield, Catherine M. Elder, Tom A. Nordheim
Figure caption: Basemap on Inverness Corona region in south polar stereographic projection. The south pole of Miranda is labeled “SP.” The box indicates the region of the geologic map (Figure 4).
Paper: Unraveling the Geologic History of Miranda’s Inverness Corona
Authors: Erin J. Leonard, Chloe B. Beddingfield, Catherine M. Elder, Tom A. Nordheim
Figure caption: Miranda as imaged by Voyager 2 with labels on each of the three corona and Verona Rupes, the prominent canyon system to the north (Modified from PIA18185). The approximate location of the south pole of Miranda is labeled “SP.”
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The maximum true anomaly as a function of the change in specific orbital angular momentum for an orbit perturbation. There is a discontinuity where the perturbation to the orbit changes the orbital angular momentum enough to push the system out of an equilibrium and the true anomaly switches from librating to circulating.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The maximum true anomaly as a function of the change in specific orbital angular momentum for an orbital perturbation. The discontinuities correspond to perturbations sufficient to push the orbit out of equilibrium and allow the true anomaly to track the secondary. The vertical dashed lines correspond to the analytical solutions from Equation (8) (left, indicating a decrease in the orbit period) and Equation (10) (right, indicating an increase in the orbit period). Numerical simulations are plotted as individual points, and show strong agreement with the analytical formulae.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Comparison between Keplerian, geometric, and observable elements for an equilibrated binary asteroid, showing the semimajor axis (top) and eccentricity (bottom). The physical parameters are shown as a black dashed line. While geometric elements are an improvement over Keplerian, the observable elements do the best job of describing the physical system.