Experimental K and L relative x-ray emission ratess

Salem, S. I.; Panossian, Stefano; Krause, Ronald A.

doi:10.1016/s0092-640x(74)80017-3

Cited by 392 publications

(123 citation statements)

References 47 publications

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“…where is the cross section for the collisional ionization p I leading to the K-shell vacancy, w is the Ñuorescence yield for the K shell (Krause 1979), and k is the relative line intensity among the possible transitions which can Ðll the inner-shell vacancy (Salem, Panossian, & Krause 1974). For the K-shell ionization cross section, we used the semiempirical formula of Quarles (1976), which is in good agreement with the data compiled in Long et al (1990).…”

Section: X-rays From Lecre Interaction With the Ismmentioning

confidence: 68%

On the Origin of the Iron K Line in the Spectrum of the Galactic X‐Ray Background

Valinia

Tatischeff

Arnaud

et al. 2000

ApJ

114

129

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We propose a mechanism for the origin of the Galactic ridge X-ray background that naturally explains the properties of the Fe K line, speciÐcally the detection of the centroid line energy below 6.7 keV and the apparent broadness of the line. Motivated by recent evidence of nonthermal components in the spectrum of the Galactic X-ray/c-ray background, we consider a model that is a mixture of thermal plasma components of perhaps supernova origin and nonthermal emission from the interaction of low-energy cosmic-ray electrons (LECRe) with the interstellar medium. The LECRe may be accelerated in supernova explosions or by ambient interstellar plasma turbulence. Atomic collisions of fast electrons produce characteristic nonthermal, narrow X-ray emission lines that can explain the complex Galactic background spectrum. Using the ASCA GIS archival data from the Scutum arm region, we show that a two-temperature thermal plasma model with kT D 0.6 and D2.8 keV, plus a LECRe component models the data satisfactorily. Our analysis rules out a purely nonthermal origin for the emission. It also rules out a signiÐcant contribution from low-energy cosmic-ray ions, because their nonthermal X-ray production would be accompanied by a nuclear c-ray line di †use emission exceeding the upper limits obtained using OSSE, as well as by an excessive Galaxy-wide Be production rate. The proposed model naturally explains the observed complex line features and removes the difficulties associated with previous interpretations of the data which evoked a very hot thermal component (kT D 7 keV).

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Section: X-rays From Lecre Interaction With the Ismmentioning

confidence: 68%

On the Origin of the Iron K Line in the Spectrum of the Galactic X‐Ray Background

Valinia

Tatischeff

Arnaud

et al. 2000

ApJ

114

129

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“…4. These ratios do also appreciately deviate from their single hole values [17]. They reflect the energy dependence of M-and N-shell hole production associated with the K-shell ionization.…”

Section: B Intensity Ratios Of K-shell X-ray Transitionsmentioning

confidence: 73%

“…The quantities N2p and N3p of (1) specify the numbers of 2 p and 3 p electrons in the neutral atom and (I~/l#) o is the intensity ratio obtained from transitions in single-hole atoms [17]. Some values of g3v are given in Table 1.…”

Section: B Intensity Ratios Of K-shell X-ray Transitionsmentioning

confidence: 99%

K-shell X-ray production for fluorine ions on target elements Ti to La

1979

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The production of target atom K-shell X-rays has been studied for 2 to 28 MeV fluorine ions incident on thin solid targets of 14 elements with atomic numbers Z2=22 to 57.Total X-ray production cross sections, energy shifts of K~ and K~ lines and K~/K, intensity ratios were measured with a Si(Li) detector. The results of cross section measurements are compared with theoretical predictions of inner shell ionization. In most cases, satisfactory agreement between measured cross sections and theoretical Coulomb ionization cross sections, corrected for the perturbation of the target atom by the projectile charge and for relativistic effects, was obtained.

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“…Experimental K β /K α X-ray intensity ratios for these elements have been compared with theoretical estimates [25][26][27] and other experimental results [13,28,29]. Theoretical estimates based on relativistic Hartree-Fock and Hartree-Slater theories were calculated by Scofield [25,26].…”

Section: Resultsmentioning

confidence: 99%

K_β/K_αX-Ray Intensity Ratios for Co, Ni, Cu, and Zn in Phthalocyanines Complexes

et al. 2011

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The K β /Kα X-ray intensity ratios of Co, Ni, Cu and Zn in metalophthalocyanines complexes have been studied. Co, Ni, Cu and Zn elements have been excited by using 59.5 keV photons emitted by 50 mCi 241 Am radioactive source. K X-rays emitted by samples have been counted by a Si(Li) detector with resolution 0.16 keV at 5.9 keV. We have found that K β /Kα X-ray intensity ratios of Co, Ni, Zn, and Cu complexes have changed depending on chemical structures of Co, Ni, Zn and Cu. The measured values have been compared with the theoretical predictions and experimental values of pure elements.

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Experimental K and L relative x-ray emission ratess

Cited by 392 publications

References 47 publications

On the Origin of the Iron K Line in the Spectrum of the Galactic X‐Ray Background

On the Origin of the Iron K Line in the Spectrum of the Galactic X‐Ray Background

K-shell X-ray production for fluorine ions on target elements Ti to La

K_β/K_αX-Ray Intensity Ratios for Co, Ni, Cu, and Zn in Phthalocyanines Complexes

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Experimental K and L relative x-ray emission ratess

Cited by 392 publications

References 47 publications

On the Origin of the Iron K Line in the Spectrum of the Galactic X‐Ray Background

On the Origin of the Iron K Line in the Spectrum of the Galactic X‐Ray Background

K-shell X-ray production for fluorine ions on target elements Ti to La

Kβ/KαX-Ray Intensity Ratios for Co, Ni, Cu, and Zn in Phthalocyanines Complexes

Contact Info

Product

Resources

About

K_β/K_αX-Ray Intensity Ratios for Co, Ni, Cu, and Zn in Phthalocyanines Complexes