期刊
ICARUS
卷 252, 期 -, 页码 334-338出版社
ACADEMIC PRESS INC ELSEVIER SCIENCE
DOI: 10.1016/j.icarus.2015.02.011
关键词
Mars; Mars, satellites; Impact processes; Satellites, formation
资金
- NSF's East Asia and Pacific Summer Institute [1107883]
- Japan Society for the Promotion of Science's Summer Science Program
- Grants-in-Aid for Scientific Research [26287101] Funding Source: KAKEN
- Office Of The Director
- Office Of Internatl Science &Engineering [1107883] Funding Source: National Science Foundation
Although the two moons of Mars, Phobos and Deimos, have long been thought to be captured asteroids, recent observations of their compositions and orbits suggest that they may have formed from debris generated by one or more giant impacts of bodies with similar to 0.01x target mass. Recent studies have both analytically estimated debris produced by giant impacts on Mars and numerically examined the evolution of circum-Mars debris disks. We perform a numerical study (Smoothed Particle Hydrodynamics simulation) of debris retention from giant impacts onto Mars, particularly in relation to a Borealis-scale giant impact (E similar to 3 x 10(29) J) capable of producing the Borealis basin. We find that a Borealis-scale impact is capable of producing a disk of mass similar to 5 x 10(20) kg (similar to 1-4% of the impactor mass), sufficient debris to form at least one of the martian moons according to recent numerical studies of martian debris disk evolution. While a Borealis-scale impact may generate sufficient debris to form both Phobos and Deimos, further studies of the debris disk evolution are necessary. Our results can serve as inputs for future studies of martian debris disk evolution. (C) 2015 Elsevier Inc. All rights reserved.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据