Luminescence and microstructure of Sm2+ ions reduced by x-ray irradiation in Li2O–SrO–B2O3 glass

2008 ◽  
Vol 103 (11) ◽  
pp. 113519 ◽  
Author(s):  
Yanlin Huang ◽  
Chuanfang Jiang ◽  
Kiwan Jang ◽  
Ho Sueb Lee ◽  
Eunjin Cho ◽  
...  
Keyword(s):  
X Ray ◽  
B2o3 Glass

Glass transition, thermal expansion and relaxation in B2O3 glass measured by time-resolved X-ray diffraction

2008 ◽  
Vol 354 (2-9) ◽  
pp. 325-327 ◽  
Author(s):  
W.J. Botta ◽  
K. Ota ◽  
K. Hajlaoui ◽  
G. Vaughan ◽  
A.R. Yavari
Keyword(s):  
Thermal Expansion ◽  
Glass Transition ◽  
X Ray Diffraction ◽  
Time Resolved ◽  
X Ray ◽  
B2o3 Glass

scholarly journals X-Ray Study of the Solution of Alkali Halides in Borax and B2O3 Glass Systems

Nature ◽  
1945 ◽  
Vol 156 (3962) ◽  
pp. 423-423 ◽  
Author(s):  
S. K. MAJUMDAR ◽  
B. K. BANERJEE ◽  
K. BANERJEE
Keyword(s):  
Alkali Halides ◽  
X Ray ◽  
B2o3 Glass

In situ high-temperature X-ray diffraction study of the Rb2O-B2O3 glass forming system

2005 ◽  
Vol 40 (1-2) ◽  
pp. 73-82 ◽  
Author(s):  
R. S. Bubnova ◽  
M. G. Krzhizhanovskaya ◽  
I. G. Polyakova ◽  
S. K. Filatov
Keyword(s):  
High Temperature ◽  
Diffraction Study ◽  
X Ray Diffraction ◽  
X Ray ◽  
Glass Forming ◽  
B2o3 Glass

Space and Time Distribution of Hard X-Ray Emission in a Loop at the Beginning of a Flare

1994 ◽  
Vol 144 ◽  
pp. 275-277
Author(s):  
M. Karlický ◽  
J. C. Hénoux
Keyword(s):  
Time Distribution ◽  
Electron Bombardment ◽  
Spatial Evolution ◽  
Superthermal Electrons ◽  
Flare Loop ◽  
X Ray ◽  
Superthermal Electron ◽  
Flare Loops ◽  
Chromospheric Evaporation ◽  
Temporal And Spatial

AbstractUsing a new ID hybrid model of the electron bombardment in flare loops, we study not only the evolution of densities, plasma velocities and temperatures in the loop, but also the temporal and spatial evolution of hard X-ray emission. In the present paper a continuous bombardment by electrons isotropically accelerated at the top of flare loop with a power-law injection distribution function is considered. The computations include the effects of the return-current that reduces significantly the depth of the chromospheric layer which is evaporated. The present modelling is made with superthermal electron parameters corresponding to the classical resistivity regime for an input energy flux of superthermal electrons of 109erg cm−2s−1. It was found that due to the electron bombardment the two chromospheric evaporation waves are generated at both feet of the loop and they propagate up to the top, where they collide and cause temporary density and hard X-ray enhancements.

Some Problems in Understanding the Solar Corona

1994 ◽  
Vol 144 ◽  
pp. 1-9
Author(s):  
A. H. Gabriel
Keyword(s):  
Solar Corona ◽  
Solar Atmosphere ◽  
Theoretical Modelling ◽  
Total System ◽  
Major Advance ◽  
X Ray ◽  
Proper Perspective ◽  
Space Observations

The development of the physics of the solar atmosphere during the last 50 years has been greatly influenced by the increasing capability of observations made from space. Access to images and spectra of the hotter plasma in the UV, XUV and X-ray regions provided a major advance over the few coronal forbidden lines seen in the visible and enabled the cooler chromospheric and photospheric plasma to be seen in its proper perspective, as part of a total system. In this way space observations have stimulated new and important advances, not only in space but also in ground-based observations and theoretical modelling, so that today we find a well-balanced harmony between the three techniques.

White-Light Coronal Structures: Streamers and CMEs

1994 ◽  
Vol 144 ◽  
pp. 82
Author(s):  
E. Hildner
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
White Light ◽  
Coronal Mass Ejections ◽  
X Rays ◽  
Solar Cycles ◽  
Temperature Function ◽  
X Ray ◽  
Eclipse Observations ◽  
Coronal Structures

AbstractOver the last twenty years, orbiting coronagraphs have vastly increased the amount of observational material for the whitelight corona. Spanning almost two solar cycles, and augmented by ground-based K-coronameter, emission-line, and eclipse observations, these data allow us to assess,inter alia: the typical and atypical behavior of the corona; how the corona evolves on time scales from minutes to a decade; and (in some respects) the relation between photospheric, coronal, and interplanetary features. This talk will review recent results on these three topics. A remark or two will attempt to relate the whitelight corona between 1.5 and 6 R⊙to the corona seen at lower altitudes in soft X-rays (e.g., with Yohkoh). The whitelight emission depends only on integrated electron density independent of temperature, whereas the soft X-ray emission depends upon the integral of electron density squared times a temperature function. The properties of coronal mass ejections (CMEs) will be reviewed briefly and their relationships to other solar and interplanetary phenomena will be noted.

Sign in / Sign up

Export Citation Format

Share Document