Physical conditions in the chromosphere of a two-strand solar flare with ejection

2014 ◽  
Vol 110 (1) ◽  
pp. 101-104 ◽  
Author(s):  
E. A. Baranovskii ◽  
N. N. Kondrashova ◽  
M. N. Pasechnik ◽  
V. P. Tarashchuk
Keyword(s):  
Solar Flare ◽  
Physical Conditions

Physical conditions in the chromosphere of a two-ribbon solar flare accompanied by a surge: 1

2013 ◽  
Vol 29 (4) ◽  
pp. 167-175 ◽  
Author(s):  
E. A. Baranovskyi ◽  
N. N. Kondrashova ◽  
M. N. Pasechnik ◽  
V. P. Tarashchuk
Keyword(s):  
Solar Flare ◽  
Physical Conditions

Atomic physics calculations relevant to solar flare spectra

1991 ◽  
Vol 336 (1643) ◽  
pp. 471-484 ◽  
Keyword(s):  
Solar Flare ◽  
Atomic Physics ◽  
Solar Flares ◽  
Solar Maximum ◽  
Emission Lines ◽  
Atomic Data ◽  
Solar Maximum Mission ◽  
X Ray ◽  
Physical Conditions ◽  
Recombination Processes

Solar flare spectra in the ultraviolet and X-ray wavelength regions are rich in emission lines from highly ionized ions, formed at temperatures around 10 7 K. These lines can be used as valuable diagnostics for probing the physical conditions in solar flares. Such analyses require accurate atomic data for excitation, ionization and recombination processes. In this paper, we present a review of work which has already been carried out, in particular for the Solar Maximum Mission observations, and we look to future requirements for Solar-A .

Physical conditions in the chromosphere of a two-ribbon solar flare accompanied by a surge: II

2014 ◽  
Vol 30 (6) ◽  
pp. 268-275
Author(s):  
E. A. Baranovsky ◽  
N. N. Kondrashova ◽  
M. N. Pasechnik ◽  
V. P. Tarashchuk
Keyword(s):  
Solar Flare ◽  
Physical Conditions

Structure and physical conditions in the Hα loops of an M7.7 solar flare

2017 ◽  
Vol 43 (11) ◽  
pp. 768-779 ◽  
Author(s):  
N. M. Firstova ◽  
V. I. Polyakov
Keyword(s):  
Solar Flare ◽  
Physical Conditions

A Discussion on solar studies with special reference to space observations - Solar flare X-ray spectra

1971 ◽  
Vol 270 (1202) ◽  
pp. 143-155 ◽  
Keyword(s):  
Solar Flare ◽  
Line Emission ◽  
Continuum Emission ◽  
Solar Abundance ◽  
Lower Corona ◽  
Steady State Condition ◽  
X Ray ◽  
Physical Conditions ◽  
High Energies ◽  
The Continuum

The solar X -ray spectrum provides a versatile method for determining physical conditions in the lower corona and corona—chromosphere interface which are associated with the chromospheric (Hα) flare phenomenon. Information is contained both in the continuum and line emission which exists at these wavelengths. Continuum emission is predominant below 0.13 nm because of the relatively low solar abundance of heavy elements capable of producing line emission at these wavelengths. During the initial phase of an X-ray event this continuum frequently appears in short, often quasi-periodic bursts whose spectrum is best described by a power law to 100 keV and decreasing more rapidly at high energies. The electron spectrum apparently responsible for these bursts has many similarities to that required for the production of type III radio bursts. The emission of flare-associated soft X-ray radiation (both line and continuum radiation) begins at the time of hard X-ray bursts but reaches maximum one to several minutes later. Line emission from ions up to Ni xxvii in the helium-like ion sequence and up to Fe xxvi in the hydrogen-like ion sequence has been observed during large flares. The evolution of the plasma in which this radiation originates can be studied by comparing emission lines in the same or adjacent stages of ionization of an element. From such observations we conclude that a steady-state condition rarely if ever exists in the X-ray emitting regions associated with a solar flare.

Solar Flare Energetic Neutral Emission Measurements in the Project Coronas-I

1994 ◽  
Vol 144 ◽  
pp. 635-639
Author(s):  
J. Baláž ◽  
A. V. Dmitriev ◽  
M. A. Kovalevskaya ◽  
K. Kudela ◽  
S. N. Kuznetsov ◽  
...  
Keyword(s):  
Solar Flare ◽  
Energy Range ◽  
Gamma Rays ◽  
Pulse Shape ◽  
Gamma Ray ◽  
Pulse Shape Discrimination ◽  
Shape Discrimination ◽  
Solar Neutron ◽  
Low Altitude

AbstractThe experiment SONG (SOlar Neutron and Gamma rays) for the low altitude satellite CORONAS-I is described. The instrument is capable to provide gamma-ray line and continuum detection in the energy range 0.1 – 100 MeV as well as detection of neutrons with energies above 30 MeV. As a by-product, the electrons in the range 11 – 108 MeV will be measured too. The pulse shape discrimination technique (PSD) is used.

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