scholarly journals ESTIMATING OF X-RAY SPECTRA FOR KAONIC AND PIONIC ATOMS AS A TOOL FOR SENSING THE NUCLEAR STRUCTURE

2009 ◽  
Vol 6 (1) ◽  
pp. 30-35 ◽  
Author(s):  
O. Yu. Khetselius ◽  
A. V. Turin ◽  
D. E. Sukharev ◽  
T. A. Florko
Keyword(s):  
Nuclear Structure ◽  
X Ray ◽  
Pionic Atoms

A New Determination of the π- Rest Mass

1976 ◽  
Vol 31 (10) ◽  
pp. 1150-1154
Author(s):  
A. Brandão d'Oliveira ◽  
H. Daniel ◽  
T. von Egidy ◽  
F. J. Hartmann
Keyword(s):  
Rest Mass ◽  
X Ray ◽  
Upper Limit ◽  
Pionic Atoms

Abstract The π- rest mass has been determined from measurements of X-ray transitions in pionic atoms, using muonic transitions for the calibration, to be mπ-= 139.571 ± 0.010 MeV. A new upper limit for the μ-neutrino rest mass was deduced: mv<0.78 MeV at 90 per cent confidence.

scholarly journals The mass of the $\pi^-$

2021 ◽  
Author(s):  
Manfred Daum ◽  
Detlev Gotta
Keyword(s):  
Charged Pion ◽  
Particle Data Group ◽  
X Ray ◽  
Pionic Atoms ◽  
Data Group

The most precise values of the mass of the negatively charged pion have been determined from several measurements of X-ray wavelengths for transitions in pionic atoms at PSI. The Particle Data Group gives the average m_{\pi^-}mπ− = (139.570 61 \pm± 0.000 24) MeV/c^22.

scholarly journals Low-Energy X-Ray Standards from Hydrogenlike Pionic Atoms

2003 ◽  
Vol 91 (24) ◽  
Author(s):  
D. F. Anagnostopoulos ◽  
D. Gotta ◽  
P. Indelicato ◽  
L. M. Simons
Keyword(s):  
Low Energy ◽  
X Ray ◽  
Pionic Atoms

Influence of nuclear structure on the characteristics of light pionic atoms

1994 ◽  
Vol 49 (3) ◽  
pp. 1454-1465 ◽  
Author(s):  
A. Cieplý ◽  
R. Mach
Keyword(s):  
Nuclear Structure ◽  
Pionic Atoms

scholarly journals PIONIC ATOMS PROBING πNN RESONANCES

2005 ◽  
Vol 20 (24) ◽  
pp. 5657-5661
Author(s):  
M. I. KRIVORUCHENKO ◽  
B. V. MARTEMYANOV ◽  
AMAND FAESSLER ◽  
C. FUCHS
Keyword(s):  
Nuclear Matter ◽  
Bound States ◽  
Optical Potential ◽  
Energy Levels ◽  
Matter Density ◽  
X Ray ◽  
Nuclear Matter Density ◽  
Dibaryon Resonance ◽  
Pionic Atoms

The pion optical potential generated by the hypothetical πNN-coupled NN-decoupled dibaryon resonance d′(2065) is calculated to the lowest order in nuclear matter density. The contribution to the pion optical potential is found to be within the empirical errors, so the d′(2065) existence currently does not contradict to the observed properties of the π--nucleus bound states. Future progress in the pionic X-ray spectroscopy can reveal contributions of πNN resonances to energy levels and widths of the pionic atoms.

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.

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