J/A+AS/97/443ivo://CDS.VizieR/J/A+AS/97/443CDSKaastra J.S.Mewe R.1998-02-28T16:28:13Z1998-02-28T17:28:03ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fratomic-physicsThe basic physical processes responsible for X-ray emission from thin plasmas are considered. Collisional ionization or photoionization of inner shells of neutral atoms and ions leads to the creation of a vacancy in one of the inner shells of the ion or atom, which is filled by a cascade of radiative (fluorescent) and nonradiative (Auger) transitions. The net result is the ejection of several electrons and photons, leaving the atom in a multiply ionized state. In this paper, the distribution of the number of emitted photons and electrons after the creation of a hole in an inner shell of an atom or ion is calculated for all ions from H to Zn. The method consists of two stages: the calculation of transition rates for a given electron configuration, and calculation of probabilities of the several cascade sequences using these transition rates.1993A&AS...97..443Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/97/443CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/97/443https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/97/443http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/97/443https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/97/443https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/97/443http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/97/443GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+AS/97/443/table2Electron distributionZAtomic numberphys.atmol.numberintPrEj3Probability of 2 electrons photoionisation (1)stat.fit.goodnessintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintstIonisation stage of ion BEFORE ionisation (neutral=1 etc.)phys.atmol.ionizationintsShell number of primary vacancy (1-7 correspond to K L1 L2 L3 M1 M2 M3)meta.id;instr.plateintIIonisation energy of the primary vacancy in eV (from Lotz)eVphys.energyfloatEAEnergy that goes into Auger electrons, in eVeVphys.energy;phys.electronfloatepsilonCorrection factor defined in equation 6 of the paperstat.fit.paramintPrEj1Probability that a photo-ionisation leads to ejection of 1 electron (1)stat.fit.goodnessintPrEj2Probability of 2 electrons photoionisation (1)stat.fit.goodnessintPrEj4Probability of 2 electrons photoionisation (1)stat.fit.goodnessintPrEj5Probability of 2 electrons photoionisation (1)stat.fit.goodnessintPrEj6Probability of 2 electrons photoionisation (1)stat.fit.goodnessintPrEj7Probability of 2 electrons photoionisation (1)stat.fit.goodnessintPrEj8Probability of 2 electrons photoionisation (1)stat.fit.goodnessintPrEj9Probability of 2 electrons photoionisation (1)stat.fit.goodnessintPrEj10Probability of 2 electrons photoionisation (1)stat.fit.goodnessintJ/A+AS/97/443/table3Fluorescence yieldsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintZAtomic numberphys.atmol.numberintstIonisation stage of ion BEFORE ionisation (neutral=1 etc.)phys.atmol.ionizationintsShell number of primary vacancy (1-7 correspond to K L1 L2 L3 M1 M2 M3)meta.id;instr.plateintDeltaNumber of Auger electrons ejected before emission of the line; the line therefore occurs in the ion with ionisation stage st+Delta+1 (the factor 1 corresponds to the photo-electron)meta.numberintilLine identification number; labels according to table 1 of the paper. Note that il runs from 1 to 22.meta.idintEApproximate line energy of the transition; note that often more accurate energies can be found in the literature.eVphys.energy;phys.atmol.transitiondoubleomegaThe fluorescence yield omega for this line (number of photons emitted per primary vacancy)phys.emissivityfloat