Simple Photoelectric Absorption during Dipping in theASCAObservation of XB 1916−053

1997 ◽  
Vol 491 (1) ◽  
pp. 388-394 ◽  
Author(s):  
M. J. Church ◽  
T. Dotani ◽  
M. Bałucińska‐Church ◽  
K. Mitsuda ◽  
T. Takahashi ◽  
...  
AIP Advances ◽  
2021 ◽  
Vol 11 (2) ◽  
pp. 025120
Author(s):  
C. Stanford ◽  
M. J. Wilson ◽  
B. Cabrera ◽  
M. Diamond ◽  
N. A. Kurinsky ◽  
...  

Energy may be removed from a beam of γ -rays traversing matter by two distinct mechanisms. A quantum of radiation may be scattered by an electron out of its initial direction with change of wave-length, or it may be absorbed completely by an atom and produce a photoelectron. The total absorption coefficient, μ, is defined by the equation d I/ dx = -μI, and is the sum of the coefficients σ and τ referring respectively to the scattering and to the photoelectric effect. For radiation of low frequency, such as X-rays, the photoelectric absorption is very much more important than the absorption due to scattering, and many experiments have shown that the photoelectric absorption per atom varies as the fourth power of the atomic number and approximately as the cube of the wave-length. For radiation of high frequency, such as the more penetrating γ -rays, the photoelectric effect is, even for the heavy elements, smaller than the scattering absorption; and, since the scattering from each electron is always assumed to be independent of the atom from which it is derived, it is most convenient to divide μ. defined above by the number of electrons per unit volume in the material and to obtain μ e the absorption coefficient per electron.


2003 ◽  
Vol 32 (6) ◽  
pp. 442-451 ◽  
Author(s):  
Horst Ebel ◽  
Robert Svagera ◽  
Maria F. Ebel ◽  
Abdallah Shaltout ◽  
John H. Hubbell

2004 ◽  
Vol 190 ◽  
pp. 172-173
Author(s):  
Şölen Balman ◽  
Aybuke Küpcü-Yoldaş

AbstractDuring 25ksec of CHANDRA ACIS-S3 observations of the old nova RR Pic 1925 a count rate of 0.067±0.0017 c/s was detected. The results show evidence (spatial and spectral) for X-ray emission from the region around the prominent SW blob in the Hα images. Shell emission is detected with count rate ≥ (1.95±1.33)×10−3 c/s. The spectral analysis shows that the source spectrum can not be explained by a single or two temperature bremsstrahlung or VMEKAL models including photoelectric absorption, only models using powerlaw distribution of temperature fit the data well and indicate excess O, Al, Mg, S, and Si in the source spectrum. A soft excess in the CHANDRA data could be explained by a partial covering absorber model with covering fraction in a range 14-86 % consistent with characteristics of the Magnetic Cataclysmic Variable systems. The light curve shows significant orbital and other modulations.


1971 ◽  
Vol 30 (4) ◽  
pp. 469-470
Author(s):  
L. V. Popova ◽  
L. A. Sholokhova

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