adsabs/AstroCLIMB huggingface dataset:
Paper: Stable Brine Layers beneath Europa’s Chaos
Authors: C. J. Chivers, J. J. Buffo, B. E. Schmidt
Figure caption: Geologic observations and the assumed formation mechanism suggest the geometry of a melt lens is significantly different from those of small sills. Top: the assumed melt lens geometry and initial temperature; dashed white line denotes the liquidus boundary. Bottom: the temperature of the plume head (Equation (5)) that formed and is heating the bottom of the melt lens throughout a simulation for various melt lens compositions.
Paper: Stable Brine Layers beneath Europa’s Chaos
Authors: C. J. Chivers, J. J. Buffo, B. E. Schmidt
Figure caption: Snapshots of the NaCl (top) and MgSO4 (bottom) melt lens chemical evolution through time, which highlight the significant slowdown of freezing after ∼180 kyr. White dashed lines denote the liquidus contour. Due to freezing only from the top, the distribution of entrained salts resembles the roofs of injected sills (Figure 3(a)). Contrasting the third column, the time at which the freshwater melt lens completely solidified (∼175 kyr), with the fourth column (t = 350 kyr) highlights the characteristics of the salts, as the NaCl melt lens is still ∼40 m thick while the MgSO4 lens is only ∼20 m thick.
Paper: Stable Brine Layers beneath Europa’s Chaos
Authors: C. J. Chivers, J. J. Buffo, B. E. Schmidt
Figure caption: SOFTBALL results and constitutive equation fits for Equation (3) (left) and Equation (4) (right) for three concentrations of a NaCl-dominated solution (35, 100, and 200 ppt). Bulk salinity for each thermal gradient or depth are horizontal averages of each two-dimensional simulation. The apparent variability seen in the entrained salt values are natural consequences of the heterogeneous nature of salt entrainment in multiphase ice–brine systems and the horizontal averaging. Values found for the constitutive fits are listed in Table 1.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (top left), H-parameter (top right), Mini-RF CPR (bottom left), and Arecibo CPR (bottom right) maps covering the Lassell Massif. The white outlines represent the boundaries of the red spot locations determined by our study. The inner outline is the boundary of the massif, and the outer outline is the boundary of the reddish region from the Clementine color-ratio map. The white box in the top-right image is the red spot location analyzed in Figure 15. Note that the color scale for the H-parameter map is inverted. All maps are overlain on LROC NAC image NAC_ROI_LASSMASSLOA_E148S3508_5M. The Mini-RF CPR data are overlain on the S1 total backscatter data. The Arecibo CPR map is overlain on an Arecibo opposite-sense circular polarization image.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (top left), H-parameter (top right), Mini-RF CPR (bottom left), and Arecibo CPR (bottom right) maps covering Helmet. The white outlines represent the boundaries of the red spot locations determined by our study. The white box in the top-right image is the red spot location analyzed in Figure 15. Note that the color scale for the H-parameter map is inverted. The black outline represents the boundary between the Helmet Smooth Plains and Hummocky units, as defined by Meyer et al. (2020). The Diviner maps are overlain on LROC NAC image NAC_ROI_HELMET__LOA_E165S3289_5M. The Mini-RF CPR data are overlain on the S1 total backscatter data. The Arecibo CPR map is overlain on an Arecibo opposite-sense circular polarization image.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (top left), H-parameter (top right), Mini-RF CPR (bottom left), and Arecibo CPR (bottom right) maps covering Mons Hansteen. The white outlines represent the boundaries of the red spot locations determined by our study. Note that the color scale for the H-parameter map is inverted. The Diviner maps are overlain on LROC NAC image NAC_ROI_HANSTEENLOA_E124S3098_5M. The Mini-RF CPR data are overlain on the S1 total backscatter data. The Arecibo CPR map is overlain on an Arecibo opposite-sense circular polarization image.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (top left), H-parameter (top right), Mini-RF CPR (bottom left), and Arecibo CPR (bottom right) maps covering the Gruithuisen domes. The white outlines represent the boundaries of the red spot locations determined by our study. The white box in the top-right image is the red spot location analyzed in Figure 15. Note that the color scale for the H-parameter map is inverted. The Diviner maps are overlain on LROC NAC image NAC_ROI_GRUITHSNLOB_E362N3197_5M. The Mini-RF CPR data are overlain on the S1 total backscatter data. The Arecibo CPR map is overlain on an Arecibo opposite-sense circular polarization image.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (left), H-parameter (center), and Mini-RF CPR (right) maps covering Darney-chi and -tau. The white outlines represent the boundaries of the red spot locations determined by our study. The white box in the center image is the red spot location analyzed in Figure 15. Note that the color scale for the H-parameter map is inverted. The maps are overlain on an LROC WAC global mosaic. The Mini-RF CPR data are overlain on the S1 total backscatter data.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (left), H-parameter (center), and Arecibo CPR (right) maps covering the Mairan domes. The white outlines represent the boundaries of the red spot locations determined by our study. The white box in the center image is the red spot location analyzed in Figure 15. Note that the color scale for the H-parameter map is inverted. The RA and H-parameter maps are overlain on LROC WAC global mosaic, and the CPR map is overlain on an Arecibo opposite-sense circular polarization image.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (left), H-parameter (center), and Mini-RF CPR (right) maps covering southern Montes Riphaeus. White arrows point out a region with relatively high H-parameter in the central part of Montes Riphaeus. The white outlines represent the boundaries of the red spot locations determined by our study. The white box in the center image is the red spot location analyzed in Figure 15. Note that the color scale for the H-parameter map is inverted. The maps are overlain on an LROC WAC global mosaic. The Mini-RF CPR data are overlain on the S1 total backscatter data.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (left), H-parameter (center), and Arecibo CPR (right) maps covering Mons La Hire. The white outlines represent the boundaries of the red spot locations determined by our study. Note that the color scale for the H-parameter map is inverted. The RA and H-parameter maps are overlain on an LROC WAC global mosaic, and the CPR map is overlain on an Arecibo opposite-sense circular polarization image.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (left), H-parameter (center), and Arecibo CPR (right) maps covering Montes Spitzbergen. The white outlines represent the boundaries of the red spot locations determined by our study. Note that the color scale for the H-parameter map is inverted. The RA and H-parameter maps are overlain on an LROC WAC global mosaic, and the CPR map is overlain on an Arecibo opposite-sense circular polarization image.
Paper: The Origin of Jupiter’s Obliquity
Authors: Rola Dbouk, Jack Wisdom
Figure caption: The obliquity, θ, obtained for different ﹩\dot{\alpha }﹩, the rate of change of the precession constant (blue dots). The black horizontal line is the value of θ 0. The purple curve is Equation (6). The red horizontal line is the mean obliquity of Jupiter.
Paper: The Origin of Jupiter’s Obliquity
Authors: Rola Dbouk, Jack Wisdom
Figure caption: Sample evolution of nonadiabatic resonance crossing leaving Jupiter’s obliquity oscillating around the average value (red horizontal line). The vertical dashed line shows the time at which α is equal to the frequency of the −f 5 + f 6 + g 6 mode. The parameters of this evolution are from the second line of Table 2.
Paper: The Origin of Jupiter’s Obliquity
Authors: Rola Dbouk, Jack Wisdom
Figure caption: The evolution of θ, the obliquity of Jupiter relative to the invariable plane, obtained by running nbody integrations without satellite migrations. The origin of time is that of J2000 (JD 2451545.0).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: The change in various diagnostics of the circulation with obliquity or dust scale. (a, b) Rates of change of the winter mean (60 sols averaged about L  s  = 270 (L  s  = 90) in the northern (southern) hemisphere winter) values of ϕ HC, ﹩{\phi }_{{u}_{\max }}﹩, ϕ PV, and ﹩{\kappa }_{{\mathrm{eff}}_{300}}﹩ with obliquity (panel (a)) and dust scale (panel (b)) for both the northern (light blue) and southern (dark blue) hemispheres. Descriptions of the quantities shown are given in Table 2, and error bars show the standard deviation of these rates of change. (c–f) Winter average values of ϕ HC (blue), ﹩{\phi }_{{u}_{\max }}﹩ (green), ϕ PV (yellow), and ﹩{\kappa }_{{\mathrm{eff}}_{300}}﹩ (purple). Panels (a)–(b) show the gradient of the lines in panels (c)–(f). In panels (c)–(d), solid lines show current-eccentricity (γ = 0.093) simulations, and dashed lines show zero-eccentricity (γ = 0) simulations. Note that ﹩{\kappa }_{{\mathrm{eff}}_{300}}﹩ is plotted on the right-hand axis of all panels.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: A time series of winter-time mixing (﹩{\kappa }_{{\mathrm{eff}}_{300}}﹩) according to historical integrations of obliquity. Winter mean is 60 sols averaged about L  s  = 270° (L  s  = 90°) in the winter northern (southern) hemisphere. (a) Obliquity from Laskar et al. (2004; data obtained at http://vo.imcce.fr/insola/earth/online/mars/mars.html), and mixing changes with obliquity in (b) the NH and (c) the SH. We have chosen to include only variations based on obliquity owing to the complication of the timing of perihelion with varying eccentricity also, although we show the time series for both γ = 0.093 (solid blue) and γ = 0.000 (dashed red).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Seasonal changes in mixing in varying-obliquity simulations. Shown is the evolution of effective diffusivity on the 300 K level (shading), zonal winds (black contours), and ϕ PV (purple line). A 30-sol smoothing is applied to the model output for clarity.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: NH winter effective diffusivity for varying-obliquity simulations: 10 sol winter average (centered around L  s  = 270°) cross sections of effective diffusivity (shading), zonal-mean zonal winds (solid contours), isentropic surfaces (dashed contours; corresponding to 200, 300, … K), and the latitude of the hemispheric maximum in zonal-mean PV (purple line). (a–e) Current eccentricity (γ = 0.093); (f–j) zero eccentricity (γ = 0).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: SH winter effective diffusivity for varying-obliquity simulations. Shading and contours are the same as in Figure 11, but for the southern hemisphere (centered around L  s  = 90°).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Seasonal changes in mixing in dust-scale simulations. Shown is the evolution of effective diffusivity on the 300 K level (shading), zonal winds (black contours), and ϕ PV (purple line). A 30-sol smoothing is applied to the model output for clarity.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Winter effective diffusivity for dust-scale simulations (left column: SH; right column: NH). Shading, contours, and time averages are the same as in Figures 11 and 12, but for the dust-scale simulations.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: North polar stereographic map of PV (shading) and zonal winds (black contours) on the 300 K surface in current-eccentricity simulations, averaged over 30 sols either side of the winter solstice. ε = 25 shows absolute PV and zonal wind, and all other panels show the PV and wind anomaly from ε = 25 for the given value of ε. The purple contour indicates the latitude of maximum PV (ϕ PV).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: North polar stereographic map of PV (shading) and zonal winds (black contours) on the 300 K surface in zero-eccentricity simulations, averaged over 30 sols either side of the winter solstice. ε = 25 shows absolute PV and zonal wind, and all other panels show the PV and wind anomaly from ε = 25 for the given value of ε. The purple contour indicates the latitude of maximum PV (ϕ PV).
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: View of the APEX, Earth, and Apophis trajectories around the Sun during the APEX cruise phase. After dropping off the OSIRIS-REx SRC on 2023 September 24, the APEX spacecraft fired its thrusters to avoid Earth (EGA0/Divert) and will use a series of EGAs and DSMs to approach Apophis. APEX will follow the right-hand orange/blue ellipse three times around the Sun over 2 Earth years. EGA1 will alter APEX's orbit to the larger yellow path, which brings the intersection point with Earth's orbit to the left side of the figure after 1 1/2 orbits. EGA2 on 2027 March 3 shifts the orbit to the left-hand orange/blue ellipse for an additional three orbits over 2 Earth years. APEX's EGA3 on 2029 April 13, approximately 1 hr after Apophis’s own close approach, puts APEX on a nearly identical orbit to Apophis. Asteroid Approach Maneuver 1 (AAM-1) matches APEX's speed to Apophis to allow a careful final approach to arrive on 2029 June 5. Note that EGA3 also significantly alters Apophis’s orbit, which is shown as it is during cruise.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: OTES-derived spectral variation on Bennu (top; Hamilton et al. 2021) is indicative of variability in thin (∼10 μm) dust deposits. Thermal inertia on Bennu (middle; Rozitis et al. 2020) revealed spatial variations in porosity. At Apophis, OTES will be able to identify the spectral signatures of LL chondrites (bottom, as compared to the carbonaceous chondrite (CC) Orgueil and CC-like spectrum of Bennu) and distinguish their petrologic type (most useful for equilibrated compositions/petrologic types >3.5).
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: APEX schedule during cruise and proximity operations. Perihelion passages are marked with P's: except for P4, perihelion distances are approximately 0.5 au, and there is a spacecraft and instrument checkout scheduled after each one. EGAs and DSMs are also indicated. EGA0 is the close Earth approach where the OREx sample is dropped off and is optimized for that task. After passing Earth on 2029 April 13, APEX flies by (FB) Apophis and then slows down with AAM-1 to bring APEX to within 4 m s−1 of Apophis’s trajectory for arrival in 2029 June.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: DTM of the sample site on Bennu, constructed using data from OLA HELT (Daly et al. 2020; Lauretta et al. 2022). We expect similar results from applying OLA at Apophis.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: Graphical representation of the Starfish Survey trajectory (one set of six waypoints). The Sun is located along the +X-axis.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: Encounter mission phase timeline for Apophis proximity operations.