Determination of the ultraviolet emission flux from solar flares on the basis of the disturbances in the ionospheric E-layer

被引：0

作者：

Prokopenko, OI ^{[1
]}

Nusinov, AA ^{[1
]}

机构：

[1] Moscow Appl Geophys Inst, Moscow 129128, Russia

来源：

GEOMAGNETISM AND AERONOMY | 2001年 / 41卷 / 01期

关键词：

D O I：

暂无

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：

An estimate of the increments in the absolute values of the extreme ultraviolet emission (shorter than 105 nm) from solar flares is obtained. A comparison between the absolute values of the solar ultraviolet emission flux from direct satellite-borne measurements and the results of a calculation of this flux, carried out on the basis of critical frequencies measurements in the daytime midlatitude E layer during flares, is performed. It was shown that the calculated ultraviolet emission fluxes are similar to the fluxes measured from satellites.

引用

页码：109 / 113

页数：5

共 34 条

[31] Extreme ultraviolet and X-ray emission of solar flares as observed from the CORONAS-F spacecraft in 2001-2003
Nusinov, AA
Kazachevskaya, TV
SOLAR SYSTEM RESEARCH, 2006, 40 (02) : 111 - 116
[32] Model estimations of wave disturbances of the emission layer’s luminosity as recorded from spacecraft in the vicinity of the solar terminator
M. A. Poluarshinov
Geomagnetism and Aeronomy, 2014, 54 : 849 - 857
[33] Long-term monthly statistics of the mid-latitude ionospheric E-layer peak electron density in the Northern geographic hemisphere during geomagnetically quiet and steadily low solar activity conditions
Pavlov, Anatoli V.
Pavlova, Nadezhda M.
ANNALS OF GEOPHYSICS, 2017, 60 (03)
[34] We develop mathematical models describing plasma heating in the corona by heat fluxes from a super-hot (T ≳ 108 K) reconnecting current layer in solar flares. The effect of collisional relaxation is shown to be important in these conditions. Taking this effect into account, we have computed the electron-temperature distributions in the vicinity of the current layer, differential and integral emission measures of the heated plasma, the intensities of spectral lines Fe XXVI (1.78 and 1.51 Å) and Ni XXVII (1.59 Å). The theoretical results are compared with observations.
Oreshina, A. V.
Somov, B. V.
UNDERSTANDING SOLAR ACTIVITY: ADVANCES AND CHALLENGES, 2012, 55 : 267 - 269

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