Pattern of Impact-Induced Ejecta from Granular Targets with Large Inclusions. (arXiv:1907.04995v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kadono_T/0/1/0/all/0/1">Toshihiko Kadono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suetsugu_R/0/1/0/all/0/1">Ryo Suetsugu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arakawa_D/0/1/0/all/0/1">Dai Arakawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasagi_Y/0/1/0/all/0/1">Yoshiki Kasagi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagayama_S/0/1/0/all/0/1">Syuichi Nagayama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suzuki_A/0/1/0/all/0/1">Ayako I. Suzuki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasegawa_S/0/1/0/all/0/1">Sunao Hasegawa</a>
We performed impact experiments to observe patterns in an ejecta curtain with
targets consisting of small sand particles and large inclusions comparable to
or smaller than the size of the projectiles. The spatial intensity
distributions in the ejecta at early stages of crater formation depend on the
size of the inclusions. Our numerical simulations of radially spreading
particles with different sizes support this result. Based on the results, we
proposed a procedure for evaluating the subsurface structures of celestial
bodies from the images of ejecta curtains obtained from space-impact
experiments.
We performed impact experiments to observe patterns in an ejecta curtain with
targets consisting of small sand particles and large inclusions comparable to
or smaller than the size of the projectiles. The spatial intensity
distributions in the ejecta at early stages of crater formation depend on the
size of the inclusions. Our numerical simulations of radially spreading
particles with different sizes support this result. Based on the results, we
proposed a procedure for evaluating the subsurface structures of celestial
bodies from the images of ejecta curtains obtained from space-impact
experiments.
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