The Origin of Lunar Mascon Basins, Part I. Impact and Crater Collapse
نویسندگان
چکیده
Johnson, David M. Blair, Andrew M. Freed, H. J. Melosh, Jeffrey C. Andrews-Hanna, Gregory A. Neumann, Roger J. Phillips, David E. Smith, Sean C. Solomon, Mark A. Wieczorek, Maria T. Zuber; Department of Physics, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USA ([email protected]); Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, 550 Stadium Mall Drive, West Lafayette, IN 47907, USA; Department of Geophysics, Colorado School of Mines, 1500 Illinois St., Golden, CO 80401, USA; Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302, USA; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA; Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA; Lamont-Doherty Earth Observatory, Columbia University, Palisades, NY 10964, USA; Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Univ. Paris Diderot, 75205 Paris Cedex 13, France.
منابع مشابه
Lunar impact basins: Stratigraphy, sequence and ages from superposed impact crater populations measured from Lunar Orbiter Laser Altimeter (LOLA) data
[1] Impact basin formation is a fundamental process in the evolution of the Moon and records the history of impactors in the early solar system. In order to assess the stratigraphy, sequence, and ages of impact basins and the impactor population as a function of time, we have used topography from the Lunar Orbiter Laser Altimeter (LOLA) on the Lunar Reconnaissance Orbiter (LRO) to measure the s...
متن کاملInterpreting Mascon Wrinkle Ridges on Isidis Planitia, Mars Using Axial Surface Mapping Techniques: Reconstructing Structural Development and Stress Environments
Introduction: Isidis Planitia, a Noachian impact crater infilled with Hesperian aged basalts, is located on Mars on the crustal dichotomy and is antipodal to the Tharsis rise [1]. Measuring 1400 km across and 2 km deep, it is comparable in scale and age to lunar mascons. The basin contains an interesting pattern of both radial and concentric wrinkle ridges (see Figure 1), and massive graben are...
متن کاملGRAIL gravity observations of the transition from complex crater to peak-ring basin on the Moon: Implications for crustal structure and impact basin formation
High-resolution gravity data from the Gravity Recovery and Interior Laboratory (GRAIL) mission provide the opportunity to analyze the detailed gravity and crustal structure of impact features in the morphological transition from complex craters to peak-ring basins on the Moon. We calculate average radial profiles of free-air anomalies and Bouguer anomalies for peak-ring basins, protobasins, and...
متن کاملASYMMETRIC STRUCTURE OF LUNAR IMPACT CRATERS DUE TO OBLIQUE IMPACTS? M.Goeritz
Introduction: It has long been a matter of debate whether there exist any characteristic features in crater morphology diagnostic for oblique impacts [e.g. 1,2]. The vast majority of impact craters are almost circular in plain view, although it is well known that most impacts occur at an oblique angle of incidence [3]. Impact events may be approximated as a stationary point source of energy and...
متن کاملA sawtooth-like timeline for the first billion years of lunar bombardment
We revisit the early evolution of the Moon’s bombardment. Our work combines modeling (based on plausible projectile sources and their dynamical decay rates) with constraints from the lunar crater record, radiometric ages of the youngest lunar basins, and the abundance of highly siderophile elements in the lunar crust and mantle. We deduce that the evolution of the impact flux did not narrow imp...
متن کامل