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Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: (Left) Retrieved vertical temperature profiles corresponding to the NEMESIS best-fit models in Figure 6. The retrieved temperature profile from L19 is shown in red for comparison. (Inset) Comparison of the retrieved 2012, 2015, and 2017 profiles near the location of Titan’s detached haze layer. (Right) Errors on the retrieved 2012, 2014, 2015, and 2017 models. The pressure scale on the right y-axis is approximate.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: Comparison of the retrieved 2014 (L  S  ∼ 56°;  cyan) and 2015 (L  S  ∼ 68°;  green) temperature profiles to (left) atmospheric model predictions from Lellouch et al. (1990), Yelle et al. (1997), and Bell et al. (2014; their model C) and (right) ground-based observations (Kim et al. 2000; L19) and measurements from the Cassini UVIS (Liang et al. 2007), INMS (Snowden et al. 2013), and CIRS (Mathé et al. 2020, shown as a range of equatorial temperatures measured from 2010 to 2017) instruments. The pressure scale on the right y-axis is approximate.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: ALMA spectra (black) extracted from nadir (left column) and limb (right column) pixels compared with the best-fit NEMESIS models (colored lines) for 2012 (first row), 2014 (second row), 2015 (third row), and 2017 (fourth row).
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: (Left) Vertical HCN VMR profiles corresponding to the NEMESIS best-fit models in Figure 6, retrieved simultaneously with the temperature profiles in Figure 7. The retrieved HCN profile from L19 is shown in red for comparison. (Right) Fractional errors on the retrieved 2012, 2014, 2015, and 2017 VMR profiles. The pressure scale on the right y-axis is approximate.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: (Top) HCN VMR at 1000 km as a function of time. (Bottom) Mesopause (black diamonds) and haze layer (blue lines) altitudes (left y-axis) and mesopause temperatures (red triangles; right y-axis) as a function of time. The secondary pressure axis is approximate.
Paper: Variability in Titan’s Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors: Alexander E. Thelen, Conor A. Nixon, Richard G. Cosentino, Martin A. Cordiner, Nicholas A. Teanby, Claire E. Newman, Patrick G. J. Irwin, Steven B. Charnley
Figure caption: Comparison of the retrieved 2014 (L  S  ∼ 56°;  cyan) and 2015 (L  S  ∼ 68°;  green) HCN vertical profiles to (left) photochemical model results (Willacy et al. 2016; Vuitton et al. 2019; Dobrijevic et al. 2021) and (right) ground-based observations (Yelle & Griffith 2003; Kim et al. 2005; L19) and Cassini UVIS (Shemansky et al. 2005; Koskinen et al. 2011), VIMS (Adriani et al. 2011), INMS (Magee et al. 2009; Cui et al. 2016), and CIRS (Mathé et al. 2020, as in Figure 10) measurements. The pressure scale on the right y-axis is approximate.
Paper: International Asteroid Warning Network Timing Campaign: 2019 XS
Authors: Davide Farnocchia, Vishnu Reddy, James M. Bauer, Elizabeth M. Warner, Marco Micheli, Matthew J. Payne, Tony Farnham, Michael S. Kelley, David D. Balam, Anatoly P. Barkov, Daniel Berteşteanu, Mirel Birlan, Bryce T. Bolin, Melissa J. Brucker, Luca Buzzi, Kenneth C. Chambers, Lukas Demetz, Anlaug A. Djupvik, Leonid Elenin, Paolo Fini, Randy Flynn, Gianni Galli, Xing Gao, Marcin Gȩdek, Mikael Granvik, Werner Hasubick, Alexander L. Ivanov, Viktor A. Ivanov, Natalya V. Ivanova, Cristóvão Jaques, Anni Kasikov, Myung-Jin Kim, David Lane, Hee-Jae Lee, Bin Li, Fan Li, Tim Lister, Vadim E. Lysenko, Eugene A. Magnier, Nawaz Mahomed, Jennie McCormick, Darrel Moon, Alessandro Nastasi, Dan A. Nedelcu, Guenther Neue, Elisabeta Petrescu, Marcel Popescu, Enrico Prosperi, Rafał Reszelewski, Dong-Goo Roh, Filipp D. Romanov, Toni Santana-Ros, Anastasia Schmalz, Sergei Schmalz, James V. Scotti, Robert Seaman, Nick Sioulas, Adrian B. Sonka, David J. Tholen, Madalina M. Trelia, Richard Wainscoat, Xin Wang, Guy Wells, Robert Weryk, Nikolai A. Yakovenko, Quanzhi Ye, Hong-Suh Yim, Chengxing Zhai, Chen Zhang, Haibin Zhao, Tinglei Zhu, Michał Żołnowski
Figure caption: Left: weighted rms of the cross-track residuals of each tracklet as a function of the astrometric position uncertainties. Right: estimated mean timing error (b  T ) for each tracklet of observations considered in our analysis. Crosses correspond to survey data, and circles correspond to follow-up data. The dashed line corresponds to the orbital uncertainty mapped into the along-track direction in the plane of sky and converted to time using the rate of motion.
Paper: International Asteroid Warning Network Timing Campaign: 2019 XS
Authors: Davide Farnocchia, Vishnu Reddy, James M. Bauer, Elizabeth M. Warner, Marco Micheli, Matthew J. Payne, Tony Farnham, Michael S. Kelley, David D. Balam, Anatoly P. Barkov, Daniel Berteşteanu, Mirel Birlan, Bryce T. Bolin, Melissa J. Brucker, Luca Buzzi, Kenneth C. Chambers, Lukas Demetz, Anlaug A. Djupvik, Leonid Elenin, Paolo Fini, Randy Flynn, Gianni Galli, Xing Gao, Marcin Gȩdek, Mikael Granvik, Werner Hasubick, Alexander L. Ivanov, Viktor A. Ivanov, Natalya V. Ivanova, Cristóvão Jaques, Anni Kasikov, Myung-Jin Kim, David Lane, Hee-Jae Lee, Bin Li, Fan Li, Tim Lister, Vadim E. Lysenko, Eugene A. Magnier, Nawaz Mahomed, Jennie McCormick, Darrel Moon, Alessandro Nastasi, Dan A. Nedelcu, Guenther Neue, Elisabeta Petrescu, Marcel Popescu, Enrico Prosperi, Rafał Reszelewski, Dong-Goo Roh, Filipp D. Romanov, Toni Santana-Ros, Anastasia Schmalz, Sergei Schmalz, James V. Scotti, Robert Seaman, Nick Sioulas, Adrian B. Sonka, David J. Tholen, Madalina M. Trelia, Richard Wainscoat, Xin Wang, Guy Wells, Robert Weryk, Nikolai A. Yakovenko, Quanzhi Ye, Hong-Suh Yim, Chengxing Zhai, Chen Zhang, Haibin Zhao, Tinglei Zhu, Michał Żołnowski
Figure caption: 2019 XS geocentric and heliocentric distance (top left), solar elongation and phase angle (top right), plane-of-sky rate of motion (bottom left), and V-band magnitude (bottom right) as a function of time. The vertical lines correspond to the time of perihelion and time of closest approach to Earth.
Paper: International Asteroid Warning Network Timing Campaign: 2019 XS
Authors: Davide Farnocchia, Vishnu Reddy, James M. Bauer, Elizabeth M. Warner, Marco Micheli, Matthew J. Payne, Tony Farnham, Michael S. Kelley, David D. Balam, Anatoly P. Barkov, Daniel Berteşteanu, Mirel Birlan, Bryce T. Bolin, Melissa J. Brucker, Luca Buzzi, Kenneth C. Chambers, Lukas Demetz, Anlaug A. Djupvik, Leonid Elenin, Paolo Fini, Randy Flynn, Gianni Galli, Xing Gao, Marcin Gȩdek, Mikael Granvik, Werner Hasubick, Alexander L. Ivanov, Viktor A. Ivanov, Natalya V. Ivanova, Cristóvão Jaques, Anni Kasikov, Myung-Jin Kim, David Lane, Hee-Jae Lee, Bin Li, Fan Li, Tim Lister, Vadim E. Lysenko, Eugene A. Magnier, Nawaz Mahomed, Jennie McCormick, Darrel Moon, Alessandro Nastasi, Dan A. Nedelcu, Guenther Neue, Elisabeta Petrescu, Marcel Popescu, Enrico Prosperi, Rafał Reszelewski, Dong-Goo Roh, Filipp D. Romanov, Toni Santana-Ros, Anastasia Schmalz, Sergei Schmalz, James V. Scotti, Robert Seaman, Nick Sioulas, Adrian B. Sonka, David J. Tholen, Madalina M. Trelia, Richard Wainscoat, Xin Wang, Guy Wells, Robert Weryk, Nikolai A. Yakovenko, Quanzhi Ye, Hong-Suh Yim, Chengxing Zhai, Chen Zhang, Haibin Zhao, Tinglei Zhu, Michał Żołnowski
Figure caption: Cross-track (left panel) and timing (right panel) errors (crosses) and 1σ error bars for a second example of tracklet of observations collected by Y00 during the campaign when the plane-of-sky rate of motion of 2019 XS was 1.″5 s−1. The dashed line corresponds to the orbit solution uncertainty in the along-track direction scaled by the rate of motion. The cross-track errors do not show any evident bias, but the estimated uncertainties underestimate the actual errors. The timing residuals suggest that there is a systematic timing error of −0.7 s.
Paper: International Asteroid Warning Network Timing Campaign: 2019 XS
Authors: Davide Farnocchia, Vishnu Reddy, James M. Bauer, Elizabeth M. Warner, Marco Micheli, Matthew J. Payne, Tony Farnham, Michael S. Kelley, David D. Balam, Anatoly P. Barkov, Daniel Berteşteanu, Mirel Birlan, Bryce T. Bolin, Melissa J. Brucker, Luca Buzzi, Kenneth C. Chambers, Lukas Demetz, Anlaug A. Djupvik, Leonid Elenin, Paolo Fini, Randy Flynn, Gianni Galli, Xing Gao, Marcin Gȩdek, Mikael Granvik, Werner Hasubick, Alexander L. Ivanov, Viktor A. Ivanov, Natalya V. Ivanova, Cristóvão Jaques, Anni Kasikov, Myung-Jin Kim, David Lane, Hee-Jae Lee, Bin Li, Fan Li, Tim Lister, Vadim E. Lysenko, Eugene A. Magnier, Nawaz Mahomed, Jennie McCormick, Darrel Moon, Alessandro Nastasi, Dan A. Nedelcu, Guenther Neue, Elisabeta Petrescu, Marcel Popescu, Enrico Prosperi, Rafał Reszelewski, Dong-Goo Roh, Filipp D. Romanov, Toni Santana-Ros, Anastasia Schmalz, Sergei Schmalz, James V. Scotti, Robert Seaman, Nick Sioulas, Adrian B. Sonka, David J. Tholen, Madalina M. Trelia, Richard Wainscoat, Xin Wang, Guy Wells, Robert Weryk, Nikolai A. Yakovenko, Quanzhi Ye, Hong-Suh Yim, Chengxing Zhai, Chen Zhang, Haibin Zhao, Tinglei Zhu, Michał Żołnowski
Figure caption: Cross-track (left panel) and timing (right panel) errors (crosses) and 1σ error bars for a selected tracklet of observations collected by N82 during the campaign when the plane-of-sky rate of motion of 2019 XS was 2″ s−1. The dashed line corresponds to the orbit solution uncertainty. The cross-track and timing errors do not show any significant bias, and the estimated uncertainties are consistent with the errors.
Paper: International Asteroid Warning Network Timing Campaign: 2019 XS
Authors: Davide Farnocchia, Vishnu Reddy, James M. Bauer, Elizabeth M. Warner, Marco Micheli, Matthew J. Payne, Tony Farnham, Michael S. Kelley, David D. Balam, Anatoly P. Barkov, Daniel Berteşteanu, Mirel Birlan, Bryce T. Bolin, Melissa J. Brucker, Luca Buzzi, Kenneth C. Chambers, Lukas Demetz, Anlaug A. Djupvik, Leonid Elenin, Paolo Fini, Randy Flynn, Gianni Galli, Xing Gao, Marcin Gȩdek, Mikael Granvik, Werner Hasubick, Alexander L. Ivanov, Viktor A. Ivanov, Natalya V. Ivanova, Cristóvão Jaques, Anni Kasikov, Myung-Jin Kim, David Lane, Hee-Jae Lee, Bin Li, Fan Li, Tim Lister, Vadim E. Lysenko, Eugene A. Magnier, Nawaz Mahomed, Jennie McCormick, Darrel Moon, Alessandro Nastasi, Dan A. Nedelcu, Guenther Neue, Elisabeta Petrescu, Marcel Popescu, Enrico Prosperi, Rafał Reszelewski, Dong-Goo Roh, Filipp D. Romanov, Toni Santana-Ros, Anastasia Schmalz, Sergei Schmalz, James V. Scotti, Robert Seaman, Nick Sioulas, Adrian B. Sonka, David J. Tholen, Madalina M. Trelia, Richard Wainscoat, Xin Wang, Guy Wells, Robert Weryk, Nikolai A. Yakovenko, Quanzhi Ye, Hong-Suh Yim, Chengxing Zhai, Chen Zhang, Haibin Zhao, Tinglei Zhu, Michał Żołnowski
Figure caption: Magnitude of cross-track (left panel) and along-track (right panel) residuals of the observations collected as part of the campaign as a function of the plane-of-sky rate of motion. Crosses correspond to survey observations, circles to targeted observations, and triangles to the calibration observations included in the fit. The two panels use the same scale to highlight the larger along-track residuals.
Paper: International Asteroid Warning Network Timing Campaign: 2019 XS
Authors: Davide Farnocchia, Vishnu Reddy, James M. Bauer, Elizabeth M. Warner, Marco Micheli, Matthew J. Payne, Tony Farnham, Michael S. Kelley, David D. Balam, Anatoly P. Barkov, Daniel Berteşteanu, Mirel Birlan, Bryce T. Bolin, Melissa J. Brucker, Luca Buzzi, Kenneth C. Chambers, Lukas Demetz, Anlaug A. Djupvik, Leonid Elenin, Paolo Fini, Randy Flynn, Gianni Galli, Xing Gao, Marcin Gȩdek, Mikael Granvik, Werner Hasubick, Alexander L. Ivanov, Viktor A. Ivanov, Natalya V. Ivanova, Cristóvão Jaques, Anni Kasikov, Myung-Jin Kim, David Lane, Hee-Jae Lee, Bin Li, Fan Li, Tim Lister, Vadim E. Lysenko, Eugene A. Magnier, Nawaz Mahomed, Jennie McCormick, Darrel Moon, Alessandro Nastasi, Dan A. Nedelcu, Guenther Neue, Elisabeta Petrescu, Marcel Popescu, Enrico Prosperi, Rafał Reszelewski, Dong-Goo Roh, Filipp D. Romanov, Toni Santana-Ros, Anastasia Schmalz, Sergei Schmalz, James V. Scotti, Robert Seaman, Nick Sioulas, Adrian B. Sonka, David J. Tholen, Madalina M. Trelia, Richard Wainscoat, Xin Wang, Guy Wells, Robert Weryk, Nikolai A. Yakovenko, Quanzhi Ye, Hong-Suh Yim, Chengxing Zhai, Chen Zhang, Haibin Zhao, Tinglei Zhu, Michał Żołnowski
Figure caption: Locations of the 70 ground-based observation sites that participated in the campaign.
Paper: International Asteroid Warning Network Timing Campaign: 2019 XS
Authors: Davide Farnocchia, Vishnu Reddy, James M. Bauer, Elizabeth M. Warner, Marco Micheli, Matthew J. Payne, Tony Farnham, Michael S. Kelley, David D. Balam, Anatoly P. Barkov, Daniel Berteşteanu, Mirel Birlan, Bryce T. Bolin, Melissa J. Brucker, Luca Buzzi, Kenneth C. Chambers, Lukas Demetz, Anlaug A. Djupvik, Leonid Elenin, Paolo Fini, Randy Flynn, Gianni Galli, Xing Gao, Marcin Gȩdek, Mikael Granvik, Werner Hasubick, Alexander L. Ivanov, Viktor A. Ivanov, Natalya V. Ivanova, Cristóvão Jaques, Anni Kasikov, Myung-Jin Kim, David Lane, Hee-Jae Lee, Bin Li, Fan Li, Tim Lister, Vadim E. Lysenko, Eugene A. Magnier, Nawaz Mahomed, Jennie McCormick, Darrel Moon, Alessandro Nastasi, Dan A. Nedelcu, Guenther Neue, Elisabeta Petrescu, Marcel Popescu, Enrico Prosperi, Rafał Reszelewski, Dong-Goo Roh, Filipp D. Romanov, Toni Santana-Ros, Anastasia Schmalz, Sergei Schmalz, James V. Scotti, Robert Seaman, Nick Sioulas, Adrian B. Sonka, David J. Tholen, Madalina M. Trelia, Richard Wainscoat, Xin Wang, Guy Wells, Robert Weryk, Nikolai A. Yakovenko, Quanzhi Ye, Hong-Suh Yim, Chengxing Zhai, Chen Zhang, Haibin Zhao, Tinglei Zhu, Michał Żołnowski
Figure caption: 2019 XS R.A. and decl. as a function of time.
Paper: The Effects of Methane Clathrates on the Thermal and Seismic Profile of Titan's Icy Lithosphere
Authors: Angela G. Marusiak, Steven Vance, Mark P. Panning, Andrea S. Bryant, Marc A. Hesse, Evan Carnahan, Baptiste Journaux
Figure caption: Vertical component of an M  w  3.1 event at epicentral distances of (a) 3°, (b) 50°, and at (c) 160°. Pure water (blue) is compared to a clathrate lid (red). To show both body and surface waves, the gray shaded areas have different y-axis limits. In the first plot, the clathrate-lid model has higher amplitudes than the pure water ice model. In the bottom two plots, the pure water ice model has greater amplitudes for surface waves but comparable amplitudes for body waves.
Paper: The Effects of Methane Clathrates on the Thermal and Seismic Profile of Titan's Icy Lithosphere
Authors: Angela G. Marusiak, Steven Vance, Mark P. Panning, Andrea S. Bryant, Marc A. Hesse, Evan Carnahan, Baptiste Journaux
Figure caption: (a) Seismic velocities of a purely water ice shell (blue) compared to a 10 km clathrate lid (red). (b) The pressure profile (purple) is nearly the same for both models, but the temperature (dashed) and density (dotted) lines vary between the models. (c) Attenuation profiles also vary with depth. The difference in thermal profile creates the changes seen in the seismic and attenuation profiles. The data used in this figure are available as the Data behind the Figure.(The data used to create this figure are available.)
Paper: The Effects of Methane Clathrates on the Thermal and Seismic Profile of Titan's Icy Lithosphere
Authors: Angela G. Marusiak, Steven Vance, Mark P. Panning, Andrea S. Bryant, Marc A. Hesse, Evan Carnahan, Baptiste Journaux
Figure caption: Rms comparison of pure water ice shell to clathrate-lid waveforms. The rms ratio for the radial (blue) and vertical (red) components are plotted vs. distance. Values greater than 1.0 (dashed gray) indicate the clathrate-lid model has greater amplitudes than the pure water ice model.
Paper: The Effects of Methane Clathrates on the Thermal and Seismic Profile of Titan's Icy Lithosphere
Authors: Angela G. Marusiak, Steven Vance, Mark P. Panning, Andrea S. Bryant, Marc A. Hesse, Evan Carnahan, Baptiste Journaux
Figure caption: (Top) Wedge diagram of internal structure for a purely water ice shell. (Bottom) Diagram of internal structure with a 10 km clathrate lid. The figures are to scale, such that the thin clathrate lid (red) represents only a small fraction of Titan’s cryo- and hydrosphere. The temperatures at the boundaries have been labeled, along with the layer thicknesses.
Paper: The Effects of Methane Clathrates on the Thermal and Seismic Profile of Titan's Icy Lithosphere
Authors: Angela G. Marusiak, Steven Vance, Mark P. Panning, Andrea S. Bryant, Marc A. Hesse, Evan Carnahan, Baptiste Journaux
Figure caption: Change in velocity for P waves (blue) and S wave (red) with depth. At the surface, both internal structure models have the same pressure and temperature but clathrates have smaller seismic velocities. The differences are exacerbated down to the depth of the conductive lid where the differences reach over 8%. Once the temperatures, pressures, and compositions are near identical again, the seismic velocities are near identical.
Paper: The Effects of Methane Clathrates on the Thermal and Seismic Profile of Titan's Icy Lithosphere
Authors: Angela G. Marusiak, Steven Vance, Mark P. Panning, Andrea S. Bryant, Marc A. Hesse, Evan Carnahan, Baptiste Journaux
Figure caption: We compare the dispersion curves for group (solid) and phase (dashed) velocity using the pure ice model (blue) and the clathrate-lid model (red). The differences are subtle and minor.
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: (Top) Effective slope (s  e ) and rms height (σ  h ) derived following our methodology applied to SHARAD surface reflectivity. (Bottom) Median differential slope at 600 m baseline (Kreslavsky & Head 2000) next to rms height at 75 m baseline, both derived from MOLA altimetry and MOLA pulse-width, respectively (Neumann 2003). Acronyms are shown to identify specific terrains discussed in the text: Elysium shield, Elysium plains, Medussa Fossae Formation and Noachian rise.
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Cross section of a 1 km crater under linear and nonlinear diffusive degradation with different rates. The average linear diffusivity inferred from degraded kilometer-scale craters on the lunar maria, κ FT (Fassett & Thomson 2014), reduces the crater to 55% of its original depth after 3 Gyr. Nonlinear diffusion from impacts occurring under the Neukum et al. (2001) production function reduces the crater’s depth by less than 1% of its original depth over the same timescale. A nonlinear diffusion rate that is roughly 250 times greater (κ LRO) would be required to match the degradation observed within the Fassett & Thomson (2014) crater population.
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Volume flux (left) and diffusivity (right) as a function of slope under the Neukum primary crater production function (Neukum et al. 2001) and subsequent secondary production function. The dashed line indicates the value predicted by the analytical linear diffusion model of Xie et al. (2017) (Equation (4)) for the same cratering rate.
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: (Left) Scatter plot SHARAD-derived vs. MOLA pulse-length rms heights. Dashed line is the identity line. Colors indicate sensitivity ranges pertaining to each data set (σ  h  < 2.25 m for SHARAD, σ  h  >1 m for MOLA). Red, blue, and yellow are where SHARAD only, MOLA only, or both are within their sensitivity ranges, respectively. (Right) Mapping showing where the SHARAD and MOLA sensitivity are achieved. Color coding is the same as for the left figure.
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Diagram of hillslope section with gradient, α, describing the geometry outlined in Section 2.4. We embed a crater profile in the digital terrain model at a range of positions (x  c , y  c ) and for each case compute the mass of the ejecta blanket that lies downslope of the plane at y = 0. The number of impacts of a given size occurring per unit time is found by applying the lunar crater production rate within the area element dxdy centered on (x  c , y  c ).
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Ejecta mass, dM, transported across the plane at y = 0 as a function of y  c , the position of the crater center in the along-slope direction. Left: mass transport by craters of different diameters on a 20° slope. Right: mass transported by a 100 m crater on slopes with varying gradients. Masses are shown for primary craters (transport by secondaries would be uniformly reduced by half).
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Positive crater topography is a combination of structural uplift and ejecta deposition. While the maximum ejecta thickness occurs at the crater rim, R, the maximum uplift height, h ul, occurs closer to the crater center, at the transient crater radius, R tr. The maximum uplift expressed in the final crater profile is taken to be half of the total rim height.
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Radial extent of the continuous ejecta blanket for a 100 m diameter crater on a range of surface slopes. Ejecta blankets become elongated in the downslope direction with increasing topographic gradient (downslope is toward the bottom of the figure).
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Centimeter-scale image requested by the Rover team showing upper exposed layers. Unit designations assigned by the Rover team are noted and correspond to those in Figure 4.