TL;DR: The Deep Impact probe collided with 9P Tempel 1 at an angle of about 30° from the horizontal as discussed by the authors, which produced an evolving ejecta flow field very similar to much smaller scale oblique-impact experiments in porous particulate targets in the laboratory.
TL;DR: In this paper, the dual-polarization, delay-Doppler images were obtained from several years of observations with the upgraded Arecibo S-band (λ 12.6 -cm ) radar telescope.
TL;DR: In this article, the distribution of the phase ratios of the Apollo 11 and 12 landing sites and the Ranger 9 impact site were mapped using a narrow-angle camera of the LRO spacecraft.
Abstract: From the lunar surface survey performed with a narrow-angle camera of the Lunar Reconnaissance Orbiter (LRO) spacecraft, the distributions of the phase ratios of the Apollo 11 and 12 landing sites and the Ranger 9 impact site were mapped. In the acquired images, the traces of the structural disturbances of the lunar regolith layer caused by the jet flows are seen. In the Ranger 9 impact site, one can see the crater of about 15 m across with a ray system, which is hardly noticeable in the brightness picture, but has a high contract in the phase ratio picture. The character of the photometric anomaly of the rays of this crater shows that they are formed by the ejected stones composing the rugged relief, which induces a strong shadow effect. At the same time, the influence of jet flows from the rocket engines smooths the relief and leads to the photometric anomaly of the opposite sign. The estimate of the maturity degree of the lunar regolith in the Apollo 11 and 12 landing sites obtained from the SELENE spectral survey suggests that the depth of the influence of the rocket engines on the soil is small, and the surface of the impact crater formed by the Ranger 9 spacecraft contains a large amount of the immature soil.
TL;DR: In this paper, the authors show that the uniform blanket of ejecta changes to a ray system, where the surface of the granular bed includes undulations, a factor that has not been addressed to date.
Abstract: In classical experiments of granular cratering, a ball dropped on an evened-out bed of grains ends up within a crater surrounded by a uniform blanket of ejecta. In this Letter, we show that the uniform blanket of ejecta changes to a ray system, or set of radial streaks of ejecta, where the surface of the granular bed includes undulations, a factor that has not been addressed to date. By carrying out numerous experiments and computational simulations thereof, we ascertain that the number of rays in a ray system ∝D/λ, where D is the diameter of the ball and λ is the wavelength of the undulations. Further, we show that the ejecta in a ray system originates in a narrow annulus of diameter D with the center at the site of impact. Our findings may help shed light on the enigmatic ray systems that ring many impact craters on the Moon and other planetary bodies.
TL;DR: The relationship between the length of crater rays and primary crater radius is still poorly understood as discussed by the authors, but it is known that the ray length scales to the radius of the primary crater with a power-law of R 1.22.