Ultraviolet observations of coronal mass ejections

被引：0

作者：

Ciaravella, A ^{[1
]}

Raymond, J ^{[1
]}

Benna, C ^{[1
]}

Fineschi, S ^{[1
]}

Gardner, L ^{[1
]}

Giordano, S ^{[1
]}

Modigliani, A ^{[1
]}

O'Neal, R ^{[1
]}

Reale, F ^{[1
]}

Romoli, M ^{[1
]}

Antonucci, E ^{[1
]}

Kohl, J ^{[1
]}

Noci, G ^{[1
]}

机构：

[1] European Space Agcy, Estec, Dept Space Sci, NL-2200 AG Noordwijk, Netherlands

来源：

31ST ESLAB SYMPOSIUM ON CORRELATED PHENOMENA AT THE SUN, IN THE HELIOSPHERE AND IN GEOSPACE | 1997年 / 415卷

关键词：

solar corona; CME; UV radiation; prominences;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Ultraviolet Coronagraph Spectrometer (UVCS) has observed several coronal mass ejections (CME) and, for some of them, the evolution of the ejected plasma has been followed. We present two CME events on December 23 1996 and March 6 1997, respectively. In both cases we were able to detect many spectral lines providing very detailed diagnostics of physical and dynamical characteristics of plasma. The Lyman lines of hydrogen are very bright but also other low temperature lines as C III (977.02 Angstrom), N III (989.79 Angstrom, 991.58 Angstrom), N II (1084.56 Angstrom), N V (1242.80 Angstrom) are very intense as well. Absorption has been detected In the hot coronal line of Si XII (499 Angstrom) probably due to the He I and H I in the cold ejected plasma. Doppler line shifts give an accurate diagnostics of the velocity field along the line of sight.

引用

页码：543 / 546

页数：4

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