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trajectories
Acoustic Signals of a Meteoroid Recorded on a Large‐ N Seismic Network and Fiber‐Optic Cables
Climate-Driven Changes in High-Intensity Wildfire on Orbital Timescales in Eurasia since 320 ka
Terrestrial ejecta suborbital transport and the rotating frame transform
ABSTRACT Suborbital analysis (SA) is presented here as the study of ballistics around a spherical planet. SA is the subset of orbital mechanics where the elliptic trajectory intersects Earth’s surface at launch point A and fall point B , known as the A -to- B suborbital problem, both launch and fall points being vector variables. Spreadsheet tools are offered for solution to this problem, based on the preferred simplified two-body model. Although simplistic in top-level description, this problem places essential reliance on reference frame transformations. Launch conditions in the local frame of point A and rotating with Earth require conversion to the nonrotating frame for correct trajectory definition, with the reverse process required for complete solution. This application of dynamics requires diligent accounting to avoid invalid results. Historic examples are provided that lack the requisite treatment, with the appropriate set of solution equations also included. Complementary spreadsheet tools SASolver and Helix solve the A -to- B problem for loft duration from minimum through 26 h. All provided spreadsheet workbook files contain the novel three-dimensional latitude and longitude plotter GlobePlot. A global ejecta pattern data set calculated using SASolver is presented. As visualized through GlobePlot, SASolver and Helix provide solutions to different forms of the A -to- B problem, in an effort to avoid errors similar to the historic misstep examples offered as a supplement. Operating guidelines and limitations of the tools are presented along with diagrams from each step. The goal is to enable mechanically valid interdisciplinary terrestrial ejecta research through novel perspective and quality graphical tools, so others may succeed where 1960s National Aeronautics and Space Administration researchers did not.
A Molecular Dynamics Simulation Study of Fe-Containing Palygorskite
Flow processes and sedimentation in a straight submarine channel on the Qiongdongnan margin, northwestern South China Sea
A general model for growth trajectories of linear carbonate platforms
Airblasts caused by large slope collapses
Filter Or Conveyor? Establishing Relationships Between Clinoform Rollover Trajectory, Sedimentary Process Regime, and Grain Character Within Intrashelf Clinothems, Offshore New Jersey, U.S.A.
An approach towards the projectile trajectory during the oblique Steinheim meteorite impact by the interpretation of structural crater features and the distribution of shatter cones
OSIRIS-REX : The Journey to Asteroid Bennu and Back
How To Interpret, Understand, and Predict Stratal Geometries Using Stratal-Control Spaces and Stratal-Control-Space Trajectories
Past changes in the North Atlantic storm track driven by insolation and sea-ice forcing
CosmoELEMENTS
Implications of the centaurs, Neptune-crossers, and Edgeworth-Kuiper belt for terrestrial catastrophism
The discovery of many substantial objects in the outer solar system demands a reassessment of extraterrestrial factors putatively implicated in mass extinction events. These bodies, despite their formal classification as minor (or dwarf) planets, actually are physically similar to comets observed passing through the inner solar system. By dint of their sizes (typically 50–100 km and upward), these objects should be considered to be giant comets. Here, I complement an accompanying paper by Napier, who describes how giant comets should be expected to cause major perturbations of the interplanetary environment as they disintegrate, leading to fireball storms, atmospheric dustings, and bursts of impacts by Tunguska- and Chelyabinsk-class bodies into the atmosphere, along with less-frequent arrivals of large (>10 km) objects. I calculate the terrestrial impact probability for all known asteroids and discuss why the old concept of single, random asteroid impacts causing mass extinctions is deficient, in view of what we now know of the inventory of small bodies in the solar system. Also investigated is how often giant comets might be thrown directly into Earth-crossing orbits, with implications for models of terrestrial catastrophism. A theme of this paper is an emphasis on the wide disparity of ideas amongst planetary and space scientists regarding how such objects might affect the terrestrial environment, from a purely astronomical perspective. That is, geoscientists and paleontologists should be aware that there is no uniformity of thought in this regard amongst the astronomical community.
Geophysical observations during the flight of the Chelyabinsk meteoroid
CosmoELEMENTS
Refining paleoaltimetry reconstructions of the Sierra Nevada, California, using air parcel trajectories
Habitat dust contamination at a Mars analog
After the high-radiation environment and the low gravity field on Mars, dust is arguably the next biggest environmental hazard facing a manned mission to Mars. The seriousness of this threat is still being studied with robotic missions. At its most benign, Martian dust the work undertaken were recorded to study their effects on dust contamination. We found that more than 50 g of dust and soil were transported into the Mars Desert Research Station (MDRS) during the 12 EVAs (extravehicular activities) that were measured. The largest amount of contamination from EVA activity was due to open-cockpit vehicle travel and depended strongly on the terrain over which the EVA was conducted. Based on first-order dust dynamics modeling, similar behaviors are expected on Mars.
The four largest well-preserved impact basins in the solar system, Borealis, Hellas, and Utopia on Mars, and South Pole–Aitken on the Moon, are all significantly elongated, with aspect ratios >1.2. This population stands in contrast to experimental studies of impact cratering that predict <1% of craters should be elliptical, and the observation that ~5% of the small crater population on the terrestrial planets is elliptical. Here, we develop a simple geometric model to represent elliptical crater formation and apply it to understanding the observed population of elliptical craters and basins. A projectile impacting the surface at an oblique angle leaves an elongated impact footprint. We assume that the crater expands equally in all directions from the scaled footprint until it reaches the mean diameter predicted by scaling relationships, allowing an estimate of the aspect ratio of the final crater. For projectiles that are large relative to the size of the target planet, the curvature of the planetary surface increases the elongation of the projectile footprint for even moderate impact angles, thus increasing the likelihood of elliptical basin formation. The results suggest that Hellas, Utopia, and South Pole–Aitken were formed by impacts inclined at angles less than ~45° from horizontal, with a probability of occurrence of ~0.5. For the Borealis Basin on Mars, the projectile would likely have been decapitated, with the topmost portion of the projectile on a trajectory that did not intersect with the surface of the planet.
Roter Kamm impact crater of Namibia: New data on rim structure, target rock geochemistry, ejecta, and meteorite trajectory
The almost circular Roter Kamm impact crater, in 1200 Ma granitic gneiss of the Namaqua Metamorphic Complex of the southern Namib Desert, has a diameter of 2.5 km and an age of 4–5 Ma. A variable orientation of the foliation in the rim gneisses is suggestive of large-scale brecciation of the rim. Along some parts of the rim, the average orientation of the foliation in the rim gneisses is tangential, along other parts it is radial, and along still other parts it is random. New analyses of large samples of the rim gneisses demonstrate a large-scale chemical heterogeneity of the target rocks. Black cataclasite veins, although mineralogically identical to their host gneisses, are almost invariably more potassic than the latter. The ejecta apron outside the crater was deposited on the earliest, fossil-bearing, eolian sands of the Pliocene to Holocene Sossus Sand Formation. Subsequent calcretization cemented the apron, but erosion and redeposition of the ejecta have not been significant in the desert environment of the southern Namib. Younger Sossus Formation sands now fill the crater and partly cover the rim and the ejecta apron. Ejecta outside the crater are most abundant in an outward-fanning apron extending from the north-northwest to the west of the crater. Blocks between 20 cm and 1.5 m in size are concentrated in this main apron in concentrically and radially orientated swaths. The longest of the latter extends 5.5 km to the northwest of the crater. Sizes of fragments on the crater rim and mappable features in the rim that can be followed and fan out into the ejecta apron, together with a slight asymmetry of the crater, suggest that the trajectory of the impacting body was northwesterly.