adsabs/AstroCLIMB huggingface dataset:
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Compositions of solar system rocks compared to CI chondrite, for BE, BSE, MORB, CC, BSM, and EH. Error bars for each element correspond to the mean uncertainty in the WD abundances for that element. The reduced χ 2 value for each correlation with CI chondrite is indicated in the plots in the upper left corner. Where ﹩{\chi }_{\nu }^{2}\lesssim 3﹩–4, the data are taken as evidence for chondritic rocky parent bodies or planets.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Top: distribution of iron mass fractions (f Fe) for the WDs and Hypatia catalog stars. We show both raw and steady-state values for the WDs and split the Hypatia catalog stars into low ([Fe/H] < − 0.5) and high ([Fe/H] > − 0.5) metallicity categories. Bottom: median and 1σ spread in f Fe for the sample of WDs based on 100 random draws from their median and uncertainty in the raw Si, Mg, and Fe abundances. Most WD iron fractions have a range of at least 10% when accounting for uncertainty in their abundances.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Distribution of ﹩{\chi }_{\nu }^{2}﹩ for the WDs (raw and steady-state adjusted), compared to the Hypatia catalog stars. The vertical line shows the approximate critical ﹩{\chi }_{\nu }^{2}﹩ value (﹩{\chi }_{\nu }^{2}\sim 3﹩–4, based on the number of observed elements), so that samples within the shaded regions are considered to be consistent with a chondritic composition.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: The HST images obtained on 2022 September 28 (code (l); upper panel) and 2022 October 8 (code (o)) in Table 3, indicating the most obvious features encountered in the images. Axes are labeled in pixels, where 1 pixel represents ≈2 km projected on the sky. Celestial north is up, and celestial east is left in both panels.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Subset of SPACEOBS images used for modeling. Axes are labeled in kilometers of projected distance at the asteroid in all panels. Labels (a)–(i) indicate observation time as given in Table 2. Celestial north is up, and celestial east is left in all panels.
Paper: A Long-lived Lunar Magnetic Field Powered by Convection in the Core and a Basal Magma Ocean
Authors: Saira S. Hamid, Joseph G. O'Rourke, Krista M. Soderlund
Figure caption: Predictions of the local Rossby number for the nominal core model estimated from CIA, ML, and MAC scaling laws.
Paper: A Long-lived Lunar Magnetic Field Powered by Convection in the Core and a Basal Magma Ocean
Authors: Saira S. Hamid, Joseph G. O'Rourke, Krista M. Soderlund
Figure caption: Sensitivities of the nominal core model to core parameters k  C , [K], [S], and Q  C  for the nominal V19K50p54 BMO model. (a) The surface magnetic field intensity is most sensitive to k  C  and [S] and less sensitive to [K] and Q  C . (b) Our choice of [S] controls the predicted timing of inner core growth and thus a compositionally driven core dynamo. The shaded region represents inner core radii that are probably inconsistent with lunar gravity data (e.g., Williams et al. 2014). (c) The duration of the dynamo is predicted to increase with increasing Q  C  and decreasing k  C . High [S] tends to delay the onset of inner core crystallization and result in a shorter field duration. The shaded region represents durations that are likely inconsistent with constraints on the end of the lunar dynamo (e.g., Mighani et al. 2020). The magnetic field intensity and the duration of the core dynamo are given by the MAC scaling law.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 1064 nm, linear polarization, DAO = (0″, 0″, 0.″9). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 1064 nm, linear polarization, and DAO = (0″, 0″, 0″). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 532 nm, linear polarization, and DAO = (0″, 0″, 0.″9). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 532 nm, circular polarization, and DAO = (0″, 0″, 0.″9). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 532 nm, circular polarization, and DAO = (0″, 0″, 0″). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 1064 nm, circular polarization, and DAO = (0″, 0″, 0″). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 532 nm, circular polarization, and DAO = (0″, 0″, 0.″5). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 1064 nm, linear polarization, and DAO = (0″, 0″, 0.″5). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Ocean pH and density as functions of CH4 and CO2 ice input. Panels (a) and (c) display the ocean pH for a W:R of 1.5 and 10.0, respectively. The density is a function of the abundances of solutes within the ocean. For example, more dissolved carbon dioxide and/or carbonate ions means a higher-density ocean. The density values are output from the FREZCHEM software, which accounts for pressure and temperature and includes standard aqueous solute species relevant to the input elements in Table 1. Panels (b) and (d) display the pH of the ocean, which, among other things, determines whether CO2 is preferentially dissolved in the ocean as a gas or as carbonates. The red dashed line indicates the upper bound for CO2 saturation, 2.5 m. Cometary CO2 added to the system past this line would exist as liquid CO2. All panels are at 283 K and 50 MPa.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: CO, H2S, H2, and N2 are potential clathrate-forming gases; the panels display their fugacities (bars) as a function of the W:R ratio and accreted abundance of CO2. Increasing the abundance of CO2 lowers the pH of the ocean, which affects the equilibrium fugacities of the other dissolved gas species. These plots assume that the other cometary ices, e.g., CO, H2S, and NH3, accreted in the abundance listed in Table 1. Only N2 could potentially have a high enough abundance in the ocean to form kilometers of clathrates; however, as noted in Section 3.3, nitrogen clathrate has a higher dissociation pressure, and its production may be inhibited by the slow kinetics of NH3 to N2 at low temperature. The red dashed line indicates the upper bound for CO2 saturation, 2.5 m. Cometary CO2 added to the system past this line would exist as liquid CO2. All panels are at 283 K and 50 MPa.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: The abundance and timing of clathrate formation influence the history of Pluto’s ocean and ice shell evolution. We find three possible paths for the evolution of Pluto’s ocean based on the timing, quantity, and location of clathrate formation. Other icy outer solar system bodies may have experienced similar evolutionary histories. Diagrams are not to scale.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Cumulative H2O, CO2, and CH4 release from core metamorphism. Core metamorphism releases enough CH4 and CO2 for ∼25 km of clathrate production. The curves plot the cumulative potential thickness of clathrate layers from thermal metamorphism, assuming that the total amount of released CO2 and CH4 is fully enclathrated. CH4 release occurs late in the metamorphic history, whereas CO2 release occurs earlier.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: CO2 clathrate production as a function of accreted ammonia (at 50 MPa). Increasing the concentration of accreted ammonia ice reduces the possible thickness of CO2 clathrates. This is because adding NH3 increases the ocean’s pH, which shifts the equilibrium toward carbonates instead of aqueous CO2. Additionally, ammonia also depresses the dissociation temperature of clathrates.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Whereas Figure 3 shows the thickness of clathrate layers assuming that CO2 and CH4 exist simultaneously, this plot displays the thickness of CO2 and CH4 clathrates allowing for complete equilibrium. In this case, only one clathrate or the other forms. The abundance of CO2 largely controls which clathrate forms. Like Figure 3, a higher W:R favors CO2 clathrate formation. The gray regions of the density contrast plots indicate regions of neither CO2 nor CH4 clathrate formation, in which case the volatile carbon becomes graphite or carbonates.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Mole fractions of CO2 and CH4, and density of CH4–CO2 clathrates as a function of CH4 and CO2 fugacities at 283 K and 50 MPa. The relative abundances of dissolved CO2 and CH4 determine the properties of the resulting clathrates.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Predominance diagram of methane, CO2, and carbonate ions as a function of pH and log mH2 at 283 K and 50 MPa. Low mH2 is oxidizing, and high mH2 is reducing.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Predicted aqueous solutes for Pluto’s ocean (a) as a function of accreted CO2 and at W:R = 1.5, (b) as a function of W:R and at CO2 wt% = 1.5, and (c) as a function of W:R and at CO2 wt% = 15. Predicted precipitated minerals (d) as a function of accreted CO2 and at W:R = 1.5 and (e) as a function of W:R and at CO2 wt% = 1.5. All panels are at 283 K and 50 MPa.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Left panel: map of effective resolution (in meters, binned at 80 m pixel−1) defined as the largest crater diameter that would not be sampled by LOLA. For this and all map-projected figures, the map projection is stereographic centered at the pole. Scale is true at the pole, with a projection radius of 1737.4 km. Right panel: due to LRO’s evolving polar orbit, the effective resolution increases toward the pole while some areas have received greater coverage than others even at the same latitude, as evident from the larger range in the percentile curves.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: (a) Subregion of a 20 m pixel−1 map-projected NAC image M139729686, (b) 20 m pixel−1 rendered LDEM, (c) LDEM effective resolution in meters, (d) LDEM counts pixel–1. The 1 km long arrows indicate the direction to the south pole (orange) and stereographic +X/+Y (purple/brown).
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Hillshade of old (left) and new (right) 20 m pixel−1 LDEM.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 1064 nm, circular polarization, and DAO = (0″, 0″, 0.″9). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 1064 nm, circular polarization, and DAO = (0″, 0″, 0.″5). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 532 nm, linear polarization, and DAO = (0″, 0″, 0.″5). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Histogram of V-band absolute magnitudes from JPL Horizons of the sample of objects with semimajor axes less than Neptune’s a < a  N  (solid red) and greater than Neptune’s a > a  N  (dashed blue) used in this study. Bin size = 2 mag.
Paper: Mineralogical Characterization and Phase Angle Study of Two Binary Near-Earth Asteroids, Potential Targets for NASA’s Janus Mission
Authors: Lucille Le Corre, Juan A. Sanchez, Vishnu Reddy, Adam Battle, David C. Cantillo, Benjamin Sharkey, Robert Jedicke, Daniel J. Scheeres
Figure caption: NIR spectrum of (175706) 1996 FG3 for each night of observation. The best sets of spectra (based on S/N, weather conditions, and telluric band residuals) were used to compute the average spectrum for each night.
Paper: Mineralogical Characterization and Phase Angle Study of Two Binary Near-Earth Asteroids, Potential Targets for NASA’s Janus Mission
Authors: Lucille Le Corre, Juan A. Sanchez, Vishnu Reddy, Adam Battle, David C. Cantillo, Benjamin Sharkey, Robert Jedicke, Daniel J. Scheeres
Figure caption: Molar content of Fa vs. ol/(ol+px) ratio for (35107) 1991 VH. Black dashed boxes represent the range of measured values for each ordinary chondrite subgroup. Gray solid boxes correspond to the uncertainties associated with the spectrally derived values from Sanchez et al. (2020). Figure adapted from Dunn et al. (2010).
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Bar plot of Galactic latitude of observations for each object in ATLAS c (upper plot) and o (lower plot). The red bar denotes the sky region spanning ±10° from the Galactic equator.
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Orbital distribution diagram showing semimajor axes (a), orbital eccentricities (e), and orbital inclinations (i) of the objects used in this study. Data taken from JPL Horizons.
Paper: Mineralogical Characterization and Phase Angle Study of Two Binary Near-Earth Asteroids, Potential Targets for NASA’s Janus Mission
Authors: Lucille Le Corre, Juan A. Sanchez, Vishnu Reddy, Adam Battle, David C. Cantillo, Benjamin Sharkey, Robert Jedicke, Daniel J. Scheeres
Figure caption: NIR spectra of (175706) 1996 FG3 normalized to unity at 1.5 μm. Each plot corresponds to the average spectrum for one night of observation. Modeled albedo curves that encompass the observed thermal fluxes and thermally corrected spectra are also shown.
Paper: A Shallow-water Model Exploration of Atmospheric Circulation on Sub-Neptunes: Effects of Radiative Forcing and Rotation Period
Authors: Ekaterina Landgren, Alice Nadeau, Nikole Lewis, Tiffany Kataria, Peter Hitchcock
Figure caption: Supercritical pitchfork bifurcation diagram illustrating a potential mechanism for the emergence of asymmetric gyres. Prior to the bifurcation, the symmetric equilibrium is stable. At the bifurcation point, the previously stable symmetrical equilibrium becomes unstable, and two new equilibrium branches appear, with one cyclonic gyre in either the north or south hemisphere.
Paper: A Shallow-water Model Exploration of Atmospheric Circulation on Sub-Neptunes: Effects of Radiative Forcing and Rotation Period
Authors: Ekaterina Landgren, Alice Nadeau, Nikole Lewis, Tiffany Kataria, Peter Hitchcock
Figure caption: Snapshots of oscillatory behavior for a regime corresponding to a weakly forced planet with a scale height corresponding to ﹩\overline{{\rm{\Phi }}}=4\times {10}^{6}﹩ at rotation period P rot = 1 day and radiative timescale τ rad = 10 days. Over the course of the oscillation, a hot equatorial band (top panel) alternates with two hot tropical bands (bottom panel) with a period of ≈55 hr.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption:  λ = 532 nm, linear polarization, and DAO = (0″, 0″, 0″). Top: FFDP; middle: OCS vs. VA; bottom: OCS at VA 1.″05 vs. azimuth angle.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption: VA for three Earth station latitudes as seen from the lunar center of mass vs. lunar longitude and latitude.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption: The Apollo 14 retroreflector has a 10 × 10 array of corner cube prisms. Picture from NASA.
Paper: Lunar Laser Ranging Retroreflectors: Velocity Aberration and Diffraction Pattern
Authors: James G. Williams, Luca Porcelli, Simone Dell'Agnello, Lorenza Mauro, Marco Muccino, Douglas G. Currie, Dennis Wellnitz, Chensheng Wu, Dale H. Boggs, Nathan H. Johnson
Figure caption: The two views on the left show a next-generation CCR in an MPAc mount; the two views on the right show the dust cover closed and open (credit ESA).