adsabs/AstroCLIMB huggingface dataset:
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The maximum true anomaly as a function of the change in both the observable and Keplerian semimajor axis. This illustrates how pushing a system out of equilibrium is equivalent to changing the semimajor axis by the difference between the observable and Keplerian values.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The true anomaly of a system that begins tumbling. At some threshold, the true anomaly switches from clocking to librating, then back to clocking as angular momentum is exchanged between the orbit and secondary. Comparing to Figure 17, this threshold is near when the orbital angular momentum crosses its nearest equilibrium value, or equivalently when the osculating eccentricity decreases to its equilibrium value, as seen in Figure 18.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The specific orbital angular momentum (top) and secondary angular momentum (bottom) of a system that begins tumbling. As the secondary enters a tumbling state, the orbital angular momentum increases on average. The dashed line corresponds to the nearest equilibrium orbit, and the orange line is a 1 day moving average of the angular momentum. We see an exchange of angular momentum between the orbit and the secondary when the secondary is tumbling.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Calculated Δv  T  as a function of Dimorphos’s reshaping of its a/b ratio. For impacts that cause more reshaping, the required Δv  T  magnitude to achieve the post-impact orbit period is smaller on average.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Stroboscopic orbit period over time for the tumbling case study in the previous section. Prior to the onset of tumbling, the orbit period experiences small, periodic variations. As the secondary begins to tumble, the amplitude of orbit period variations increases and the periodicity is absent.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The post-impact observable eccentricity as a function of the pre-impact observable eccentricity. The two curves define an envelope in which the post-impact observable eccentricity may exist, depending on where in its orbit the secondary was at the time of the perturbation.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The Keplerian and observable eccentricity of a system that begins tumbling. As the secondary enters a tumbling state, the eccentricity decreases as the orbital angular momentum decreases. The dashed line corresponds to the equilibrium Keplerian value.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Calculated Δv  T  as a function of Dimorphos’s mass loss. Within reasonable values for mass loss, there is no strong trend in Δv  T .
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The pre- and post-impact orbits for the nominal system plotted to scale. For illustration purposes, the scaled radar shape model is used to show Didymos (Naidu et al. 2020) and the Daly et al. (2023) shape model is used to show Dimorphos.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The relative 1-2-3 Euler angles (roll-pitch-yaw) of the secondary of an unstable system that begins tumbling. Significant NPA rotation begins at around 40 days into the simulation.
Paper: Regolith Inhibits Salt and Ice Crystallization in Mg(ClO4)2 Brine, Implying More Persistent and Potentially Habitable Brines on Mars
Authors: Andrew O. Shumway, David C. Catling, Jonathan D. Toner
Figure caption: The water content in regolith varies depending on the RH and the amount of salt for several systems: modeled pure brine (dashed curves), regolith without salt (black circles and dotted curves), an ideal mixture of brine and regolith (solid curves), and experimental brine-regolith mixtures (colored circles). The curves for the ideal brine-regolith mixtures sum the behavior of pure brine and salt-free regolith, assuming each component behaves independently. However, experimental brine-regolith mixtures deviate greatly from ideal behavior for 0.6–5.8 wt.% salt (A–D). The step changes that occur in some systems at ∼40.4% RH are the result of salt precipitation. Notably, salt phase transitions are absent in the experimental data for 0.6–5.8 wt.% salt (A–D). For comparison, a positive example of salt crystallization in regolith is shown (panel E). All data represent samples at 25 °C that have lost water from a prior wet state (i.e., “Drying Curve” in Figure 1).
Paper: Regolith Inhibits Salt and Ice Crystallization in Mg(ClO4)2 Brine, Implying More Persistent and Potentially Habitable Brines on Mars
Authors: Andrew O. Shumway, David C. Catling, Jonathan D. Toner
Figure caption: At any specified relative humidity, experimental brine-regolith mixtures (circles) are less concentrated than pure brine (black curve). The trend of pure Mg(ClO4)2 brine (black curve) was calculated using a revised Pitzer model for perchlorates described in Toner et al. (2015b), and terminates at the saturation point (4.44 molal, RH = 40.4%). Also shown is the known lower a  w  limit for life on Earth (a  w  = 0.585, dashed red line; Stevenson et al. 2017). All data represent samples at 25 °C that have lost water from a prior wet state (i.e., “Drying Curve” in Figure 1).
Paper: Regolith Inhibits Salt and Ice Crystallization in Mg(ClO4)2 Brine, Implying More Persistent and Potentially Habitable Brines on Mars
Authors: Andrew O. Shumway, David C. Catling, Jonathan D. Toner
Figure caption: Measured melting points of brine-regolith samples (squares) are depressed compared to pure brine (black line) at a given salt concentration (mol kg w  −1). The freezing point of pure Mg(ClO4)2 brine was calculated using a revised Pitzer model described in Toner et al. (2015b). At all wt.% salt measured, some relatively high-concentration samples showed no signs of freezing, melting, or forming glass whatsoever, over the full range of temperatures (−150 °C–20 °C). The concentrations of these unfrozen samples are shown in the lower panel. All data represent samples that have lost water from a prior wet state (i.e., “Drying Curve” in Figure 1).
Paper: Regolith Inhibits Salt and Ice Crystallization in Mg(ClO4)2 Brine, Implying More Persistent and Potentially Habitable Brines on Mars
Authors: Andrew O. Shumway, David C. Catling, Jonathan D. Toner
Figure caption: Adsorption isotherms show the minor extent of a wetting-drying hysteresis effect in regolith and brine-regolith mixtures. At any given relative humidity, samples that are drying from a prior wet state retain more water than identical samples that are wetting from a prior dry state (Hillel 1971). The regolith used was Mojave Mars Simulant (MMS) and all experiments were conducted at 25 °C. Data for 0.6 and 1.0 wt.% Mg(ClO4)2 in MMS are excluded here because only drying curves were measured for those samples.
Paper: Regolith Inhibits Salt and Ice Crystallization in Mg(ClO4)2 Brine, Implying More Persistent and Potentially Habitable Brines on Mars
Authors: Andrew O. Shumway, David C. Catling, Jonathan D. Toner
Figure caption: To probe how the a  w  of briny regolith changes with temperature, we predicted the a  w  at each sample’s melting temperature  (T melt, squares) via Equation (1), then compared to the measured a  w  of the same sample at 25 °C (T ref, circles). Note that the melting temperature varies for each sample (see Figure 4), but for all samples T melt < T ref = 25 °C. All data represent samples that have lost water from a prior wet state (i.e., “Drying Curve” in Figure 1).
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: System mass calculated using a numerical routine considering F2BP dynamics, along with the system mass calculated using Keplerian dynamics, as functions of the pre-impact observable semimajor axis. Ignoring the F2BP coupling and Didymos oblateness results in a consistently larger mass estimate.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The semimajor axis (top left), eccentricity (bottom left), longitude of periapsis (top right), and true anomaly (bottom right) of a numerical GUBAS simulation compared to the analytical LPE solution for a perturbed system. Because the system is perturbed, both GUBAS and the LPE correctly show the true anomaly circulating and the longitude of periapsis precessing.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Change in observable eccentricity as a function of the possible pre-impact observable semimajor axis. The change in eccentricity is largely independent of the pre-impact semimajor axis. The pre-impact orbit is assumed physically circular. The simulation runs with a skewed smaller eccentricity change are the result of tumbling in the secondary.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: System bulk density as a function of the possible pre-impact observable semimajor axis, calculated using a numerical routine considering F2BP dynamics. Accounting for the system uncertainties, including the volumes, the bulk density is 2.4 ± 0.3 g cm−3 (1σ), with a dependence on the pre-impact separation.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Change in along-track velocity as a function of the possible pre-impact observable semimajor axis. There is a strong relationship between Δv  T  and pre-impact observable semimajor axis.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The semimajor axis (top left), eccentricity (bottom left), longitude of periapsis (top right), and true anomaly (bottom right) of a numerical GUBAS simulation compared to the analytical LPE solution for an equilibrated system. The LPE solution shows the true anomaly circulating, while in reality this angle should be zero and the longitude of periapsis should be circulating.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Change in along-track velocity as a function of Didymos’s possible J 2 gravity coefficient. The magnitude of Δv  T  decreases slightly as Didymos’s J 2 increases.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The change in observable semimajor axis as a function of the possible pre-impact observable semimajor axis. There is a strong linear relationship between the post- and pre-impact semimajor axes.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Percent error in the calculated mass when ignoring the aspherical shapes and F2BP dynamics, as a function of pre-impact observable semimajor axis. Using Keplerian dynamics results in approximately a 1%–3% error in mass estimate.
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: The precession rate as a function of the secondary’s elongation a/b, calculated using the F2BP dynamics (GUBAS) and the analytical LPEs with the nominal primary J 2. Including secondary libration in the dynamics results in a decrease in the apsidal precession rate, whereas ignoring it results in an increase. The effect of a resonance is visible near a/b = 1.1, discussed in detail in Agrusa et al. (2021).
Paper: The Perturbed Full Two-body Problem: Application to Post-DART Didymos
Authors: Alex J. Meyer, Harrison F. Agrusa, Derek C. Richardson, R. Terik Daly, Oscar Fuentes-Muñoz, Masatoshi Hirabayashi, Patrick Michel, Colby C. Merrill, Ryota Nakano, Andrew F. Cheng, Brent Barbee, Olivier S. Barnouin, Steven R. Chesley, Carolyn M. Ernst, Ioannis Gkolias, Nicholas A. Moskovitz, Shantanu P. Naidu, Petr Pravec, Petr Scheirich, Cristina A. Thomas, Kleomenis Tsiganis, Daniel J. Scheeres
Figure caption: Calculated observable Δe as a function of Dimorphos’s reshaping of its a/b ratio. For impacts that cause more reshaping, the change in eccentricity is on average reduced.
Paper: Maps of Solar Wind Plasma Precipitation onto Mercury’s Surface: A Geographical Perspective
Authors: Federico Lavorenti, Elizabeth A. Jensen, Sae Aizawa, Francesco Califano, Mario D'Amore, Deborah Domingue, Pierre Henri, Simon Lindsay, Jim M. Raines, Daniel Wolf Savin
Figure caption: Normalized energy distribution of the particles in the solar wind (orange) and at the surface (blue). Panels (a) and (b) show the proton distribution functions. Panels (c) and (d) show the electron distribution functions. The red vertical solid lines show the mean energy of the solar wind plasma, which is equal to ﹩{K}_{{}_{\mathrm{SW}}}={m}_{{\rm{i}}}{V}_{{}_{\mathrm{SW}}}^{2}/2=826\,\mathrm{eV}﹩ for protons and ﹩{T}_{{\rm{e}}{,}_{\mathrm{SW}}}=21.5\,\mathrm{eV}﹩ for electrons. The green vertical dashed lines in panels (a) and (b) show an estimate of the proton energy downstream of the bow shock equal to ﹩{K}_{{}_{\mathrm{SW}}}/{M}_{{\rm{f}}{,}_{\mathrm{SW}}}^{2}﹩, where ﹩{M}_{{\rm{f}}{,}_{\mathrm{SW}}}=3.3﹩ is the fast magnetosonic Mach number in the solar wind upstream of the bow shock. The green vertical solid lines show an estimate of the maximum magnetic energy available for magnetic reconnection equal to ﹩{K}_{{}_{\mathrm{SW}}}/{M}_{{\rm{A}},\mathrm{lobe}}^{2}﹩, where M A,lobe = 0.32 is the Alfvén Mach number in the lobes computed using a magnetic field of 100 nT and density of 3 cm−3.
Paper: Maps of Solar Wind Plasma Precipitation onto Mercury’s Surface: A Geographical Perspective
Authors: Federico Lavorenti, Elizabeth A. Jensen, Sae Aizawa, Francesco Califano, Mario D'Amore, Deborah Domingue, Pierre Henri, Simon Lindsay, Jim M. Raines, Daniel Wolf Savin
Figure caption: Proton precipitation maps integrated over two full Mercury orbits. Panels (a)–(d) are obtained from a simulation with a purely northward IMF and panels (e)–(h) with a purely southward IMF, shown by the green vectors on the left. The different columns correspond to different energy bins, given at the top of each column. At perihelion, when longitude 0° is subsolar, longitudes −90° and +90° correspond to local dawn and dusk, respectively. The white bins in the maps correspond to negligible fluences below 1013 cm−2.
Paper: Maps of Solar Wind Plasma Precipitation onto Mercury’s Surface: A Geographical Perspective
Authors: Federico Lavorenti, Elizabeth A. Jensen, Sae Aizawa, Francesco Califano, Mario D'Amore, Deborah Domingue, Pierre Henri, Simon Lindsay, Jim M. Raines, Daniel Wolf Savin
Figure caption: Proton precipitation maps integrated over two full Mercury orbits and averaged over latitude and longitude. The curves in panels (a) and (c) are obtained from the maps in Figures 3(a)–(d) and (e)–(h), respectively, by averaging in latitude. The curves in panels (b) and (d) are obtained, respectively, from the same maps by averaging in longitude. The black dots and line show the averages summed over all energies, and the colored areas show the contributions for the labeled energy bins. The horizontal dashed black lines show the mean value of the fluence (averaged in both latitude and longitude).
Paper: Maps of Solar Wind Plasma Precipitation onto Mercury’s Surface: A Geographical Perspective
Authors: Federico Lavorenti, Elizabeth A. Jensen, Sae Aizawa, Francesco Califano, Mario D'Amore, Deborah Domingue, Pierre Henri, Simon Lindsay, Jim M. Raines, Daniel Wolf Savin
Figure caption: Same as Figure 4, but for electron precipitation.