THE DETERMINATION OF ELECTRON-DENSITIES IN THE SOLAR ATMOSPHERE FROM THE 1718.56-ANGSTROM 1486.51-ANGSTROM EMISSION-LINE RATION IN N-IV

被引：4

作者：

KEENAN, FP ^{[1
]}

HARRA, LK ^{[1
]}

DOSCHEK, GA ^{[1
]}

COOK, JW ^{[1
]}

机构：

[1] USN,RES LAB,EO HULBURT CTR SPACE RES,WASHINGTON,DC 20375

来源：

ASTROPHYSICAL JOURNAL | 1994年 / 432卷 / 02期

关键词：

SUN; ACTIVITY; ATMOSPHERE; CORONA; UV RADIATION;

D O I：

10.1086/174618

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The theoretical electron density sensitive emission-line ratio R = I(1718.56 Angstrom)/I(1486.51 Angstrom) in N IV is presented for a range of N-e (similar or equal to 10(10)-10(12) cm(-3)) applicable to higher density solar plasmas, such as active regions. A comparison of these calculations with the observed values of R of several solar features obtained with the Naval Research Laboratory's S082B spectrograph on board Skylab reveals general agreement between theory and observation at pointings just above the limb, where line blends with N IV 1718.56 Angstrom should be insignificant, which provides experimental support for the accuracy of the line ratio calculations.

引用

页码：806 / 808

页数：3

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