Observations and models of the kinematics of the zodiacal dust cloud

被引：0
|
作者：
Madsen, G. J. [1 ]
Reynolds, R. J. [2 ]
Ipatov, S. I. [3 ]
Kutyrev, A. S. [4 ]
Mather, J. C. [4 ]
Moseley, S. H. [4 ]
机构：
[1] Anglo Australian Observ, POB 296, Epping, NSW 1710, Australia
[2] Univ Wisconsin Madison, Madison, WI 53711 USA
[3] Univ Maryland, College Pk, MD 20742 USA
[4] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
来源：
WORKSHOP ON DUST IN PLANETARY SYSTEMS | 2007年 / 643卷
基金：
美国国家科学基金会;
关键词：
D O I：
暂无
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We report on new observations of the motion of zodiacal dust using optical absorption line spectroscopy of zodiacal light. We have measured the change in the profile shape of the scattered solar Mg I lambda 5184 line toward several lines of sight in the ecliptic plane as well as the ecliptic pole. The variation in line centroid and line width as a function of helio-ecliptic longitude show a clear prograde signature and suggest that significant fraction of the dust follows non-circular orbits that are not confined to the ecliptic plane. When combined with dynamical models, the data suggest that the zodiacal dust is largely cometary, rather than asteroidal, in origin.
引用
收藏
页码：61 / +
页数：3
相关论文
共 50 条
12345