Dielectronic satellite spectra for highly charged helium-like ions - VI. Iron spectra with improved inner-shell and helium-like excitation rates

Bely‐Dubau, F.; Dubau, J.; Faucher, P.; Gabriel, A. H.

doi:10.1093/mnras/198.1.239

Cited by 150 publications

(59 citation statements)

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“…For radiative recombination rate coefficients, we have used the method of Bely- Dubau et al (1982a). This method is based on (Z − 0.5) screened hydrogenic approximation of the Burgess (1958) formulae, as we explain below.…”

Section: Radiative Recombination (Rr) Coefficients Ratesmentioning

confidence: 99%

“…Bely- Dubau et al (1982a) used this equation for Helike 1snl levels by replacing Z with (Z −0.5). The quantity (Z − 0.5) was chosen to take into account the screening of the 1s orbital.…”

Section: Radiative Recombination (Rr) Coefficients Ratesmentioning

confidence: 99%

“…The present study has shown that the radiative recombination (RR) is slowly convergent with n, thus the first 49 levels (n ≤ 5) are considered as fine-structure levels (LSJ), the levels from n = 6 to n = 10 (l = 9) shells are separated in LS term (Bely-Dubau et al 1982a, 1982b, and finally levels from n = 11 to n = ∞ are taken into account inside n = 10. Figure 3 shows the scaled direct plus upper (n > 2) level radiative cascade RR rates = 8, 10, 12 and 14), and for comparison the direct RR contribution.…”

Section: Radiative Recombination (Rr) Coefficients Ratesmentioning

confidence: 99%

“…We used the same method as Bely- Dubau et al (1982a). The AUTOLSJ code (including the SUPERSTRUCTURE code) was run with 42 configurations belonging to 1snl, 2snl and 2pnl, with n ≤ 5.…”

Section: Dielectronic Recombination (Dr) Coefficient Ratesmentioning

confidence: 99%

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X-ray photoionized plasma diagnostics with helium-like ions. Application to warm absorber-emitter in active galactic nuclei

Porquet

Dubau

2000

Astron. Astrophys. Suppl. Ser.

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314

435

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Abstract. We present He-like line ratios (resonance, intercombination and forbidden lines) for totally and partially photoionized media. For solar plasmas, these line ratios are already widely used for density and temperature diagnostics of coronal (collisional) plasmas. In the case of totally and partially photoionized plasmas, He-like line ratios allow for the determination of the ionization processes involved in the plasma (photoionization with or without an additional collisional ionization process), as well as the density and the electronic temperature.With the new generation of X-ray satellites, Chandra/AXAF, XMM and Astro-E, it will be feasible to obtain both high spectral resolution and high sensitivity observations. Thus in the coming years, the ratios of these three components will be measurable for a large number of non-solar objects.In particular, these ratios could be applied to the Warm Absorber-Emitter, commonly present in Active Galactic Nuclei (AGN). A better understanding of the Warm Absorber connection to other regions (Broad Line Region, Narrow Line Region) in AGN (Seyferts type-1 and type-2, low-and high-redshift quasars...) will be an important key to obtaining strong constraints on unified schemes.We have calculated He-like line ratios, for Z = 6, 7, 8, 10, 12 and 14, taking into account the upper level radiative cascades which we have computed for radiative and dielectronic recombinations and collisional excitation. The atomic data are tabulated over a wide range of temperatures in order to be used for interpreting a large variety of astrophysical plasmas.

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Section: Radiative Recombination (Rr) Coefficients Ratesmentioning

confidence: 99%

Section: Radiative Recombination (Rr) Coefficients Ratesmentioning

confidence: 99%

Section: Radiative Recombination (Rr) Coefficients Ratesmentioning

confidence: 99%

“…We used the same method as Bely- Dubau et al (1982a). The AUTOLSJ code (including the SUPERSTRUCTURE code) was run with 42 configurations belonging to 1snl, 2snl and 2pnl, with n ≤ 5.…”

Section: Dielectronic Recombination (Dr) Coefficient Ratesmentioning

confidence: 99%

See 2 more Smart Citations

X-ray photoionized plasma diagnostics with helium-like ions. Application to warm absorber-emitter in active galactic nuclei

Porquet

Dubau

2000

Astron. Astrophys. Suppl. Ser.

Self Cite

314

435

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“…Both cross sections were integrated over the energy distribution G(E). In this work, c^, the dielectronic recombination coefficients were calculated using the usual nomenclature: SUPERSTRUCTURE AUTOLSJ (Bely-Dubau et al, 1982). In this preliminary work, the charge exchange was neglected in formula ( 1 ) .…”

mentioning

confidence: 99%

Dielectronic Recombination of Highly Stripped Argon Ions: Theoretical Calculations and Direct Observations in an Ebis Source

Loulergue¹,

Dubau²,

Briand

et al. 1984

International Astronomical Union Colloquium

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The dielectronic recombination is one of the most important atomic processes in highly ionised plasmas. It corresponds to the simultaneous capture of a free electron and excitation of an ion, i . e .x + m + l + e -+ (x+ni)** (doubly excited) ^ ( X + m ) * + hv.It is a collisionally resonant process which occurs only at the energy of the corresponding autoionisation electron. We present here a preliminary theoretical analysis of the results of an experiment using a novel technique in which it is possible to observe the interaction of a given ion with an electron at a given energy and so to measure the differential dielectronic cross section corresponding to each resonant level of this ion.This technique uses an electron-beam ion EBIS source (Briand et al, 1984) in which a very intense and very narrow electron beam is used to ionise a neutral gas that has been injected into the system. After being prepared the ions are trapped for a very long time (up to 10 s) inside the source. The electron-beam energy is then scanned incrementally in order to study the various dielectronic resonances of the ions by the observation of x rays which are emitted through a small hole drilled into the cathode. Each measurement at energy E of the electron beam c o r r esponds a narrow electron-energy distribution G(E) of 16 eV. The x r a y s are detected after the plasma has reached a stationary equilibrium following each increment of the electron-beam e n e r g y . The relative abundance of the ions is given by the ionisation balance equationwhere N(X + m ) and N ( X + m + 1 ) are the density of the ion ground s t a t e s . S and Oj, were calculated respectively using the Lotz ionisation cross sections (Lotz, 1967) and the hydrogenic photoionisation formulae given by Burgess (1969). Both cross sections were integrated over the energy distribution G(E). In this work, c^, the dielectronic recombination coefficients were calculated using the usual nomenclature: SUPERSTRUCTURE AUTOLSJ (Bely-Dubau et al, 1982). In this preliminary work, the charge exchange was neglected in formula ( 1 ) . 262https://www.cambridge.org/core/terms. https://doi

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COMPARISON OF SATELLITE SPECTRA FOR H-LIKE Fe AND He-LIKE Fe, Ca, AND S CALCULATED BY THREE DIFFERENT METHODS

Katō

Safronova

Shlyaptseva

et al. 1997

Atomic Data and Nuclear Data Tables

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Dielectronic satellite spectra for highly charged helium-like ions - VI. Iron spectra with improved inner-shell and helium-like excitation rates

Cited by 150 publications

References 0 publications

X-ray photoionized plasma diagnostics with helium-like ions. Application to warm absorber-emitter in active galactic nuclei

X-ray photoionized plasma diagnostics with helium-like ions. Application to warm absorber-emitter in active galactic nuclei

Dielectronic Recombination of Highly Stripped Argon Ions: Theoretical Calculations and Direct Observations in an Ebis Source

COMPARISON OF SATELLITE SPECTRA FOR H-LIKE Fe AND He-LIKE Fe, Ca, AND S CALCULATED BY THREE DIFFERENT METHODS

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