Proton-electron bremsstrahlung polarization - Solar flare X-ray and gamma-ray polarization

1987 ◽  
Vol 323 ◽  
pp. 391 ◽  
Author(s):  
D. Heristchi
Keyword(s):  
Solar Flare ◽  
Gamma Ray ◽  
X Ray ◽  
Electron Bremsstrahlung

scholarly journals Electron Bremsstrahlung Hard X-Ray Spectra, Electron Distributions, and Energetics in the 2002 July 23 Solar Flare

2003 ◽  
Vol 595 (2) ◽  
pp. L97-L101 ◽  
Author(s):  
Gordon D. Holman ◽  
Linhui Sui ◽  
Richard A. Schwartz ◽  
A. Gordon Emslie
Keyword(s):  
Solar Flare ◽  
X Ray ◽  
Electron Bremsstrahlung ◽  
Electron Distributions

Parameters of the intense X-ray and gamma-ray radiation from the solar flare of May 20, 2002, as observed from the Coronas-F spacecraft

2003 ◽  
Vol 29 (3) ◽  
pp. 199-204 ◽  
Author(s):  
A. V. Bogomolov ◽  
A. P. Ignat’ev ◽  
K. Kudela ◽  
S. N. Kuznetsov ◽  
Yu. I. Logachev ◽  
...  
Keyword(s):  
Solar Flare ◽  
Gamma Ray ◽  
X Ray

SEARCH FOR ENHANCEMENTS OF MUONS AT SEA LEVEL FROM TRANSIENT EVENTS

2005 ◽  
Vol 20 (29) ◽  
pp. 6941-6943
Author(s):  
C. R. A. AUGUSTO ◽  
C. E. NAVIA ◽  
M. B. ROBBA
Keyword(s):  
Solar Flare ◽  
Sea Level ◽  
Gamma Ray ◽  
Unknown Origin ◽  
Ground Level ◽  
X Ray ◽  
Raster Scan ◽  
Main Target ◽  
Transient Events ◽  
Ground Level Enhancements

The main target of this study is a search for the origin of two ground level enhancements (GLEs), observed on December of 2003 at sea level by using the TUPI muon telescope. The results show that one of them has a strong correlation with solar flare, while the other has an unknown origin, because there is not satellite report of solar flare, nor the prompt X-ray emission and neither the excess of nuclei during the raster scan where the GLE was observed. Even so, two possibilities are analyzed: the solar flare hypothesis and the gamma ray burst (GRB) hypothesis.

scholarly journals A Solar Flare Observed with the Smm and Einstein Satellites

1989 ◽  
Vol 104 (1) ◽  
pp. 361-373
Author(s):  
J. H. M. M. Schmitt ◽  
J. R. Lemen ◽  
D. Zarro
Keyword(s):  
Solar Flare ◽  
Proportional Counter ◽  
Gamma Ray ◽  
X Rays ◽  
X Ray ◽  
Basic Properties ◽  
Earth’S Atmosphere ◽  
Gamma Ray Spectrometer ◽  
Basic Physics ◽  
Earth's Atmosphere

AbstractWe present X-ray observations of the 21 July, 1980 flare which was observed both with the Einstein Observatory Imaging Proportional Counter (IPC) and the X-Ray Polychromator (XRP) and Gamma-Ray Spectrometer onboard the SMM satellite. The Einstein observations were obtained in scattered X-ray light, i.e., in X-rays scattered off the Earth's atmosphere. In this way it is possible to obtain spatially unresolved X-ray data of a solar flare with the same instrument that observed many X-ray flares on other stars. This paper juxtaposes the results and implications of the ‘stellar interpretation’ to those obtained from the far more detailed SMM observations. The result of this ‘calibration’ observation is that the basic properties of the flaring plasma can be reliably determined from the ‘stellar’ data, however, the basic physics issues can only be studied through models.

scholarly journals Stereoscopic observations of the giant hard X-ray/gamma-ray solar flare on 1991 June 30 at 0255 UT

2003 ◽  
Vol 403 (3) ◽  
pp. 1157-1163 ◽  
Author(s):  
G. Trottet ◽  
R. A. Schwartz ◽  
K. Hurley ◽  
J. M. McTiernan ◽  
S. R. Kane ◽  
...  
Keyword(s):  
Solar Flare ◽  
Gamma Ray ◽  
X Ray

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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