Possible reasons of shock melt deficiency in the Bosumtwi drill cores

被引:19
作者
Artemieva, N.
机构
[1] Inst Dynam Geospheres, Moscow 119334, Russia
[2] Planetary Sci Inst, Tucson, AZ 85719 USA
关键词
D O I
10.1111/j.1945-5100.2007.tb01083.x
中图分类号
P3 [地球物理学]; P59 [地球化学];
学科分类号
0708 ; 070902 ;
摘要
Pre-drilling numerical modeling of the Bosumtwi impact event predicted a 200 in thick coherent melt layer, as well as abundant highly shocked target material within the central part of the crater structure. However, these predictions are in disagreement with data from drill core obtained in 2004-2005. Here I provide a brief overview of previous results and discuss possible reasons behind melt deficiency, such as specific impact scenarios (low impact velocity and/or low impact angle), and specific target properties (different composition, high porosity, high content of volatiles). I conclude that the most likely explanation is the dispersion of impactites due to the vaporization of pore water, which was not included in the original numerical model.
引用
收藏
页码:883 / 894
页数:12
相关论文
共 56 条
[1]  
Ahrens T. J., 1972, Moon, V4, P214, DOI 10.1007/BF00562927
[2]  
AHRENS TJ, 1977, IMPACT EXPLOSION CRA, P639
[3]  
Amsden A.A., 1980, SALE SIMPLIFIED ALE, DOI 10.2172/5176006
[4]  
[Anonymous], 1989, OXFORD MONOGRAPHS GE
[5]   Investigating the Lake Bosumtwi impact structure: Insight from numerical modeling [J].
Artemieva, N ;
Karp, T ;
Milkereit, B .
GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS, 2004, 5
[6]  
Artemieva N, 2002, IMPACT STUD, P257
[7]  
ARTEMIEVA N, 2006, 37 LUN PLAN SCI C
[8]  
ARTEMIEVA N, 34 LUN PLAN SCI C
[9]   Proceedings of the Workshop on the Role of Volatiles and Atmospheres on Martian Impact Craters [J].
Barlow, Nadine C. ;
Stewart, Sarah T. ;
Barnouin-Jha, Olivier S. .
METEORITICS & PLANETARY SCIENCE, 2006, 41 (10) :1423-1424
[10]  
BROWN M, 2006, 37 LUN PLAN SCI C