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Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Location of flight 1, with an inset at the upper left showing the larger context. For flight 1, Ingenuity hovered at a lateral distance due west of Perseverance of about 63 m. North is up in both the detail and inset panels. All geography figures come from the Mars 2020 Mission Tracker website (https://experience.arcgis.com/experience/84a507c94b3a4b32b654e7f544ad1d52).
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Geography of flight 3. Ingenuity flew about 50 m due north at an altitude of 5.28 m and then flew due south, returning to its takeoff point very near the takeoff point for flights 1 and 2. The lateral distance indicated by the ruler in the figure is the distance along the ground.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Telemetry streams (panels (a) and (b)) and MEDA wind data (panel (c)) for flight 2. The legends provide the curve labels, and line colors and styles and shaded gray regions have the same meanings as in Figure 3. (Note that an azimuth of −180° is equivalent to +180°.)
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Zoomed-in view of Ingenuity’s fuselage and interior, as adapted from the Mars 2020 Software Interface Specification. The helicopter camera locations and viewing frustrums are shown. The yaw (z), pitch (y), and roll (x) axes are also shown. For example, a given pitch angle corresponds to a right-handed rotation about the y-axis.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Wind speeds and directions inferred during flights 59 (a) and 61 (b) over the time window when Ingenuity was hovering. The colored wedges show the range of uncertainties on the wind direction for points inferred from Ingenuity telemetry (see Table 1). The blue upward-pointing triangles show inferred values during the ascent, while the orange downward-pointing triangles are from the descent. The solid gray lines show the corresponding wind speed profile from the Mars MCD model, and the dashed gray lines show the wind profile extrapolated from MarsWRF. The arrows attached to points and to the profiles indicate the direction in which the winds are blowing, with north at the top of the plot.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Based on C. Dull et al. (2022), our model for relating the drone’s tilt angle (given in terms of pitch and roll by Equation (1)) to airspeed.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Time series of wind speeds during flight 1. The orange dots represent the wind speeds inferred from Ingenuity’s tilt, downsampled by a factor of 100. The gray lines show the Gaussian process model, and the resulting average and uncertainty are shown in orange at the top right (also illustrated by the horizontal orange lines). The MEDA wind speed is shown in blue.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Telemetry streams for flight 59. The legend provides the curve labels, and line colors and styles and shaded gray regions have the same meanings as in Figure 3. There are no MEDA wind data against which to compare.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Location of flight 59 with an inset at the upper right showing the larger context, with north pointing forward into the distance along the surface in the oblique panel and up in the inset. For flight 59, Ingenuity took off from a point northwest of Perseverance at a distance of about 378 m. The long white strand in the larger, oblique view shows the flight path toward the takeoff point for flight 61.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Telemetry streams for flight 61. The legend provides the curve labels, and line colors and styles and shaded gray regions have the same meanings as in Figure 3. There are no MEDA wind data against which to compare.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Telemetry streams (panels (a) and (b)) and MEDA wind data (panel (c)) for flight 3. The legends provide the curve labels, and line colors and styles and shaded gray regions have the same meanings as in Figure 3. (An azimuth of 360° is equivalent to an azimuth of 0°, and an azimuth of −180° is equivalent to +180°.)
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Telemetry streams (panels (a) and (b)) and MEDA wind data (panel (c)) for flight 5. The legends provide the curve labels, and line colors and styles and shaded gray regions have the same meanings as in Figure 3. (An azimuth of 360° is equivalent to an azimuth of 0°, and −180° is equivalent to +180°.)
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Telemetry streams (panels (a) and (b)) and MEDA wind data (panel (c)) for flight 4. The legends provide the curve labels, and line colors and styles and shaded gray regions have the same meanings as in Figure 3. (An azimuth of −180° is equivalent to +180°).
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Wind profile analysis using data from flights 1–5. Throughout the three panels, the blue stars show data for flight 1, the orange squares for flight 2, the green upward-pointing triangles for flight 3, the black downward-pointing triangles for flight 4, and the purple circles for flight 5. (a) Average wind speeds u(z) measured by MEDA (at z = 1.5 m) and inferred from Ingenuity data. The best-fit friction velocity u ⋆ and roughness length z ⋆ for each pair of wind speeds are shown in the legend and color-coded by flight. (N.B., we use z ⋆ instead of the usual z 0 for roughness length.) (b) Average wind azimuths and uncertainties from each flight using the same symbols as in panel (a). The azimuth from MEDA is offset just to the left, and the azimuth from Ingenuity is offset just to the right of each numbered flight along the x-axis. (c) Wind profile derived by folding all average wind speeds together—see narrative for an explanation of the y-axis. The best-fit u ⋆ and z ⋆ are shown.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Dependence of wind profile parameter uncertainties for u ⋆ and z ⋆, given by ﹩{\sigma }_{{u}_{\star }}﹩ and ﹩{\sigma }_{{z}_{\star }}﹩, respectively. N is the number of points sampled along the wind profile; ﹩\delta x\equiv \mathrm{ln}\left({z}_{i+1}/{z}_{i}\right)﹩, i.e., the spacing of sample points; and z 0/z ⋆ is the ratio of the height of the lowermost sample point to the roughness length. Blue lines (solid and dashed) show ﹩{u}_{\star }/{\sigma }_{{u}_{\star }}﹩, while orange lines show ﹩{z}_{\star }/{\sigma }_{{z}_{\star }}﹩. We have assumed σ/u ⋆ = 1 for these calculations. The solid lines illustrate the conditions closest to those analyzed in this study.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Exploring the best-fit Richardson numbers Ri. (a) For each data pair from all flights, the inferred Ψ-value vs. the approximate Ri ≈ z/L, where z is the height at which the average wind speed is estimated and L is the inferred Monin–Obukhov length. For this plot, we assumed a u ⋆ for each pair of data points derived from MEDA data and z ⋆ = 1 cm (G. M. Martínez et al. 2023). (b) The best-fit Ri (x-axis) as derived from the Ψ-values shown on the y-axis of panel (a). Negative Ψ-values are unphysical and plotted with Ri = 0. In both panels, the symbols correspond to the same flights as in Figure 15.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Contours of upwind fetch distance to which the wind profile measured at height z over a surface of roughness length z ⋆ is sensitive. The dashed blue lines show z = 3.25 and 5.28 m, the altitudes at which Ingenuity probed winds during flights 1–5. The shaded gray region shows where z < 20z ⋆, heights low enough that the logarithmic wind profile may not apply and the flow becomes laminar.
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: Diagram illustrating the structure of the CPD model, and delimited into two distinct zones. The first zone, situated closer to Jupiter, is optically thick, characterized by an optical depth τ exceeding 2/3 in the midplane. The second zone, located farther from Jupiter, is optically thin, with τ below 2/3 in the midplane. The altitude at τ = 2/3 defines the photosurface. Within the optically thick region, thick lines on the diagram depict this photosurface, indicating a temperature gradient ranging from hot (red) to cold (blue) regions. These regions are demarcated by the adiabatic-to-isothermal transition zone (purple box), where the photosurface ceases to exist. Material is uniformly accreted onto the CPD at distances closer to the centrifugal radius (Rc).
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: CPD temperature profiles with dust enrichment levels (from left to right columns) corresponding to 0.1, 1, and 10 times the protosolar value, depicted at t = 100, 150, and 200 kyr of the CPD evolution (from top to bottom rows). The solid white line represents the altitude of the photosurface. If the photosurface is not explicitly shown or represented in a given panel, it indicates its absence. The hatched areas are located within the shadow cast by the CPD.
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: Temperature (left panels) and pressure (right panels) profiles of the CPD at t = 50, 100, 150, and 200 kyr of the CPD evolution. The photosurface and the CPD’s scale height are presented by the white solid and dashed lines, respectively. If the photosurface is not explicitly shown or represented in a given panel, it indicates its absence. The hatched area is located within the shadow cast by the CPD.
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: CPD temperature profiles with α-viscosity parameters (from left to right columns) corresponding to 10−2, 10−3, and 10−4, depicted at t = 100, 150, and 200 kyr of the CPD evolution (from top to bottom rows). The solid white line represents the altitude of the photosurface. If the photosurface is not explicitly shown or represented in a given panel, it indicates its absence. The hatched areas are located within the shadow cast by the CPD.
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: From top to bottom: CPD’s surface density, midplane temperature, and midplane pressure profiles, represented at t = 33, 50, 100, 150, and 200 kyr of the CPD evolution.
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: Time evolution of the CPD’s mass (blue line) and gas accretion rate (red line).
Paper: Potential Landing Sites: A Comprehensive Reconnaissance Assessment of the Europa Clipper Trajectory
Authors: Jennifer E. C. Scully, Ines Belgacem, Rutu Parekh, Cyril Grima, Cynthia B. Phillips, Kathleen L. Craft, Geoffrey C. Collins, Charlie Detelich, Erin J. Leonard, Ishan Mishra, G. Wesley Patterson, Louise M. Prockter, Angela M. Stickle, Sarah S. Sutton, Danielle Y. Wyrick, Catherine M. Elder, Alfred S. McEwen, Colleen M. O'Shea, Jordi E. Turner
Figure caption: Simulated Europan surface at different solar incidence angles. Image (b) occurs in the 30°–60° incidence range and thus has an acceptable density of shadows for matching multiple features. Image (a) occurs in the <30° range and has too few shadows, while image (c) occurs in the >60° range and has too many shadows. Credit: Europa Lander study team.
Paper: Potential Landing Sites: A Comprehensive Reconnaissance Assessment of the Europa Clipper Trajectory
Authors: Jennifer E. C. Scully, Ines Belgacem, Rutu Parekh, Cyril Grima, Cynthia B. Phillips, Kathleen L. Craft, Geoffrey C. Collins, Charlie Detelich, Erin J. Leonard, Ishan Mishra, G. Wesley Patterson, Louise M. Prockter, Angela M. Stickle, Sarah S. Sutton, Danielle Y. Wyrick, Catherine M. Elder, Alfred S. McEwen, Colleen M. O'Shea, Jordi E. Turner
Figure caption: Areas of interest highlighted around the ground track of E22. The detailed area highlighted by the blue box (a) highlights a wedged band crossed by a double ridge, while the detailed area surrounded by the red box (b) highlights the presence of lenticulae. The pink box (c) highlights a similar area south of the ground track where high-resolution imaging is available (adapted from L. M. Parro et al. 2016). The gray shaded area on the right indicates Europan nighttime. The closest approach point of the flyby is at 0°N/S, 157°E.
Paper: Potential Landing Sites: A Comprehensive Reconnaissance Assessment of the Europa Clipper Trajectory
Authors: Jennifer E. C. Scully, Ines Belgacem, Rutu Parekh, Cyril Grima, Cynthia B. Phillips, Kathleen L. Craft, Geoffrey C. Collins, Charlie Detelich, Erin J. Leonard, Ishan Mishra, G. Wesley Patterson, Louise M. Prockter, Angela M. Stickle, Sarah S. Sutton, Danielle Y. Wyrick, Catherine M. Elder, Alfred S. McEwen, Colleen M. O'Shea, Jordi E. Turner
Figure caption: Ground track of E8 projected on Europa’s geological map (simplified version of E. J. Leonard et al. 2024). Different altitudes are represented by the ground-track line color, as defined in the key. The reconable area is highlighted by a thicker yellow line and white box. Two white dashed delimiters extend this reconable area to include acceptable margins (as defined in Section 2.1). Names of key features are included in white text. The closest approach point of the flyby is at 48°N, 178°E.
Paper: Potential Landing Sites: A Comprehensive Reconnaissance Assessment of the Europa Clipper Trajectory
Authors: Jennifer E. C. Scully, Ines Belgacem, Rutu Parekh, Cyril Grima, Cynthia B. Phillips, Kathleen L. Craft, Geoffrey C. Collins, Charlie Detelich, Erin J. Leonard, Ishan Mishra, G. Wesley Patterson, Louise M. Prockter, Angela M. Stickle, Sarah S. Sutton, Danielle Y. Wyrick, Catherine M. Elder, Alfred S. McEwen, Colleen M. O'Shea, Jordi E. Turner
Figure caption: Ground track of E8 projected on a Europa basemap (U.S. Geological Survey 2022). Different altitudes are represented by the ground-track line color, as defined in the key. The reconable area is highlighted by a thicker yellow line and white box. Two white dashed delimiters extend this reconable area to include acceptable margins (as defined in Section 2.1). EIS WAC opportunities are projected and colored by solar incidence angle: these are indicative of the areas in which observations could be acquired. We highlight crossovers with supporting and other reconable flybys (see Table 1) in the white boxes, which include the crossover altitude and rank of the crossing flyby. A moon crescent symbol indicates that the crossing flyby occurs at nighttime. The closest approach point of the flyby is at 48°N, 178°E.
Paper: Potential Landing Sites: A Comprehensive Reconnaissance Assessment of the Europa Clipper Trajectory
Authors: Jennifer E. C. Scully, Ines Belgacem, Rutu Parekh, Cyril Grima, Cynthia B. Phillips, Kathleen L. Craft, Geoffrey C. Collins, Charlie Detelich, Erin J. Leonard, Ishan Mishra, G. Wesley Patterson, Louise M. Prockter, Angela M. Stickle, Sarah S. Sutton, Danielle Y. Wyrick, Catherine M. Elder, Alfred S. McEwen, Colleen M. O'Shea, Jordi E. Turner
Figure caption: Ground track of E7 projected on a Europa basemap (U.S. Geological Survey 2022). Different altitudes are represented by the ground-track line color, as defined in the key. The area is only reconable when acceptable margins are taken into account, as highlighted by two white dashed delimiters (as defined in Section 2.1). EIS WAC opportunities are projected and colored by solar incidence angle: these are indicative of the areas in which observations could be acquired. We highlight crossovers with supporting and other reconable flybys (see Table 1) in the white boxes, which include the crossover altitude and rank of the crossing flyby. A moon crescent symbol indicates that the crossing flyby occurs at nighttime. The closest approach point of the flyby is at 21°N, 178°E.
Paper: Potential Landing Sites: A Comprehensive Reconnaissance Assessment of the Europa Clipper Trajectory
Authors: Jennifer E. C. Scully, Ines Belgacem, Rutu Parekh, Cyril Grima, Cynthia B. Phillips, Kathleen L. Craft, Geoffrey C. Collins, Charlie Detelich, Erin J. Leonard, Ishan Mishra, G. Wesley Patterson, Louise M. Prockter, Angela M. Stickle, Sarah S. Sutton, Danielle Y. Wyrick, Catherine M. Elder, Alfred S. McEwen, Colleen M. O'Shea, Jordi E. Turner
Figure caption: Ground track of E4 projected on a Europa basemap (U.S. Geological Survey 2022). Different altitudes are represented by the ground-track line color, as defined in the key. The reconable area is highlighted by a thicker yellow line and white box. Two white dashed delimiters extend this reconable area to include acceptable margins (as defined in Section 2.1). EIS WAC opportunities are projected and colored by solar incidence angle: these are indicative of the areas in which observations could be acquired. There are no crossovers with this flyby. The gray shaded area on the left indicates Europan nighttime. The closest approach point of the flyby is at 63°S, 182°E.
Paper: Potential Landing Sites: A Comprehensive Reconnaissance Assessment of the Europa Clipper Trajectory
Authors: Jennifer E. C. Scully, Ines Belgacem, Rutu Parekh, Cyril Grima, Cynthia B. Phillips, Kathleen L. Craft, Geoffrey C. Collins, Charlie Detelich, Erin J. Leonard, Ishan Mishra, G. Wesley Patterson, Louise M. Prockter, Angela M. Stickle, Sarah S. Sutton, Danielle Y. Wyrick, Catherine M. Elder, Alfred S. McEwen, Colleen M. O'Shea, Jordi E. Turner
Figure caption: Ground track of E36 projected on a Europa basemap (U.S. Geological Survey 2022). Different altitudes are represented by the ground-track line color, as defined in the key. EIS WAC opportunities are projected and colored by solar incidence angle: these are indicative of the areas in which observations could be acquired. Reconable flyby(s) that this flyby crosses over are shown in pink ground track(s), with the reconable portion(s) being thicker pink lines. The gray shaded area on the right indicates Europan nighttime. The closest approach point of the flyby is at 31°S, 357°E.
Paper: Potential Landing Sites: A Comprehensive Reconnaissance Assessment of the Europa Clipper Trajectory
Authors: Jennifer E. C. Scully, Ines Belgacem, Rutu Parekh, Cyril Grima, Cynthia B. Phillips, Kathleen L. Craft, Geoffrey C. Collins, Charlie Detelich, Erin J. Leonard, Ishan Mishra, G. Wesley Patterson, Louise M. Prockter, Angela M. Stickle, Sarah S. Sutton, Danielle Y. Wyrick, Catherine M. Elder, Alfred S. McEwen, Colleen M. O'Shea, Jordi E. Turner
Figure caption: Ground track of E12 projected on a Europa basemap (U.S. Geological Survey 2022). Different altitudes are represented by the ground-track line color, as defined in the key. EIS WAC opportunities are projected and colored by solar incidence angle: these are indicative of the areas in which observations could be acquired. Reconable flyby(s) that this flyby crosses over are shown in pink ground track(s), with the reconable portion(s) being thicker pink lines. The closest approach point of the flyby is at 6°S, 171°E.