THE STRUCTURE OF IOS CORONA

被引：50

作者：

SCHNEIDER, NM ^{[1
]}

HUNTEN, DM ^{[1
]}

WELLS, WK ^{[1
]}

SCHULTZ, AB ^{[1
]}

FINK, U ^{[1
]}

机构：

[1] UNIV ARIZONA,LUNAR & PLANETARY LAB,TUCSON,AZ 85721

来源：

ASTROPHYSICAL JOURNAL | 1991年 / 368卷 / 01期

关键词：

PLANETS; JUPITER; SATELLITES;

D O I：

10.1086/169694

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A spatial profile of the distribution of sodium in Io's corona has been constructed using measurements obtained during satellite mutual eclipses. The data reveal a fairly symmetric corona whose density falls steeply from the surface out to 6 r(Io) and more slowly outside. An upper limit of 700 km is placed on the exobase altitude, but the observations do not constrain the surface density. Several theoretical models adequately match some traits of the corona, but none satisfies all the observations. No strong upstream/downstream asymmetry of the corona is observed, so it is unlikely that the corona is primarily generated by the impact of corotating ions into the trailing hemisphere.

引用

页码：298 / 315

页数：18

共 53 条

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