Contributors: Robert Gamache, Léna Hartmann, Bastien Vispoel, Kara Kleghorn, Candice Renaud
... HITRAN2016 line file with hydrogen as the broadening gas. The line file uses the new temperature dependence of the half-width and line shift by Gamache and Vispoel. Please see the read_me.txt file for details.
Contributors: Laurence Campbell, Michael Brunger
... These files list the neutral and ion reactions used for the calculations. They have the form: X: R1 + R2 -> P1 + P2 rate (as a Fortran statement) ; source where X = P, C or 0,I,F for photodissociation, chemical reaction or 3-body reaction
Contributors: Charles Hibbitts, Benjamin Wing, Chris Paranicas, Karen Stockstill-Cahill
... These are the spectra of the irradiated and unirradiated salts that were used in the manuscript's figures
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Data for: Equilibrium of simple crater counts on the lunar maria is primarily set by diffusive degradation due to spatially heterogeneous distal ejecta
Contributors: David Minton, Caleb Fassett, Bryan Howl, Masatoshi Hirabayashi, James Richardson
... This file Figures.zip contains the scripts and data used to generate all figures in the manuscript. The file Movies.zip contains animations of the simulations presented in the manuscript. Description of movie files Movie S01 (proximal) is the output of the simulation in which only the degradation arising from the slope-dependent mass redistribution of proximal ejecta of the primary production function is modeled. Movie S1 corresponds to Figure 9 of the main text. Movies S02-S03 (micrometeoroid) are the output of the simulations in which an enhanced micrometeoroid population is added to the production function. Two cases are shown, one in which the resolvable crater production SFD has a slope of η=3.2 (S2) and one in which we modeled a slightly shallower production SFD slope of η=3.0. Movie S2 corresponds to Figure 11 of the main text. Movies S04-S10 (uniform) are the output of the simulations in which with additional extra diffusion added over a uniform region with radius f_e r, with K_(d,1) determined by solving equation (32) of the main text for the equilibrium SFD (n_(eq,1)=0.0084 and β=2) given a value of f_e. Here we have varied f_e from 3 to 50. Movie S4 (f_e=3) corresponds to Figure 14 of the main text, and Movie S8 (f_e=10) corresponds to Figure 15 of the main text. Movies S11-S12 (ray) are the output of simulations in which additional extra diffusion is added over a spatially heterogeneous region mimicking crater rays. Two ray models are tested (see Figure 16 of the main text for the degradation scale “intensity function” for these two models). Both models use values of K_(d,1) needed to match the observed equilibrium SFD. Movie S12 corresponds to Figure 18 of the main text. Movies S13-S17 (etatest) are the output of simulations testing whether the analytical model given by equation (30) of the main text correctly predicts the dependence on the equilibrium SFD when the production function slope, η, is varied. In these simulations, η is varied between 2.6-3.8. We fix the value of K_(d,1), f_e=3, and ψ=2 for the solution to the observed equilibrium SFD for η=3.2, (see Movie S4). Movies S18-S21 (psitest) are the output of simulations testing whether the analytical model given by equation (30) of the main text correctly predicts the dependence on the equilibrium SFD when the degradation function slope, ψ, is varied. In these simulations, ψ is varied between 1.8-2.4. We fix the value of K_(d,1), f_e=3, and η=3.2 for the solution to the observed equilibrium SFD for ψ=2.0, (see Movie S4).
Contributors: Colin Miranda, David Dowling
... The formation of impact craters in unconsolidated granular materials is a topic of enduring interest in solid-earth geophysics, planetary science, and several branches of engineering science. In particular, a general relationship between crater size, impact parameters, and target material properties is often sought. This paper presents a new empirical relationship, based on dimensional analysis and inspired by gas-dynamic shock physics, for the diameters of low- and high-speed impact craters in dry granular materials based on the hypothesis that surface-gravity- and shock-wave phenomena primarily set crater size. The final relationship involves the impacting object’s kinetic energy and speed; the target material’s density, angle of repose, and sound speed; and the gravitational acceleration at the impact location. It is formulated in terms of a dimensionless crater diameter, an algebraic combination of Froude number, Mach number, and the tangent of the target material’s angle of repose, using an analogy to gas dynamics and an empirical power law for the dependence of granular-material sound speed on gravitational acceleration. The coefficient of determination for the final fit is 0.969 based on experimental impact data from 325 individual impacts spanning parametric ranges of more than 400 in crater diameter, 10^10 in impact energy, 500 in gravitational acceleration, and 40 in target material density for two different angles of repose. The final formula provides insight into how impact energy conversion depends on Mach number and may be useful for predictive and forensic analysis of planetary impact craters and for granular-flow code validation.
Data for: Discovering the Smallest Observed Near-Earth Objects with the Space Surveillance Telescope
Contributors: Arthur Lue, Herbert Viggh, Mark Czerwinski, Jacob Varey, Jessica Ruprecht
... Observations of small NEOs from SST while operating in New Mexico.
Contributors: Samuel Howell, Robert Pappalardo
... MATLAB software used to perform plate tectonics force balance for ocean world ice shells.
Appendix II: Compositional Distributions and Evolutionary Processes for the Near-Earth Object Population: Results from the MIT-Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS)
Contributors: Richard Binzel, Francesca DeMeo, Juan Sanchez, Stephen Slivan, Cristina Thomas, Tasha Dunn, Vishnu Reddy, Pierre Vernazza, Benoit Carry, Andrew Rivkin
... Tabulation of Taxonomic and Principal Component Analysis for near-Earth objects observed in the MIT-Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS)
Data for: A small lunar swirl and its implications for the formation of the Reiner Gamma magnetic anomaly
Contributors: Jung-Kyu Lee, Ho Jin, Omid Ghassemi, Rachel Maxwell, Hyojeong Lee, Seul-Min Baek, Ian Garrick-Bethell, Megan Kelley, Seongwhan Lee, Khan-Hyuk Kim
... LVL 0 magnetometer data product description: The data is given in 24 hour frames with the decimal DOY (day of year) as the title, and is further split into half orbits, exploiting the nearly polar orbit of the LP spacecraft. Each struct contains the following: Col 1: LP LVL0 magnetometer data and position array (data)* Col 2: start of half-orbit in julian-time (jdstart) Col 3: end of half-orbit in julian-time (jdstop) Col 4: start of half-orbit in decimal doy (doystart) Col 5: end of half-orbit in decimal doy (doystop) Col 6: longitude at equator crossing (eqlon) * The description for the mag data arrays is as follows: Col 1: julian date Col 2: decimal doy Col 3: B_x (nT) Col 4: B_y (nT) Col 5: B_z (nT) Col 6: |B| (field magnitude) (nT) Col 7: julian date corresponding to spacecraft position/trajectory (Col 8-12)(redundant) Col 8: radius of spacecraft relative to fixed lunar center (km) Col 9: spacecraft translational velocity (km/s) Col 10: latitude (deg) Col 11: longitude (deg) Col 12: altitude (km)
Data for: Spectral Characterization of Analog Samples in Anticipation of OSIRIS-REx’s Arrival at Bennu: A Blind Test Study
Contributors: Kerri Donaldson Hanna, Ashley King, Daniel Applin, Paul Schofield, Devin Schrader, Timothy McCoy, Cateline Lantz, Edward Cloutis, Harold Connolly, Jr., George Cody
... Visible to near infrared reflectance spectra measured at the University of Winnipeg and thermal infrared emissivity spectra measured at the University of Oxford of the blind test samples. The samples and their measurements are described in the submitted manuscript.