scholarly journals A NEW APPROACH TO ANALYZING SOLAR CORONAL SPECTRA AND UPDATED COLLISIONAL IONIZATION EQUILIBRIUM CALCULATIONS. II. UPDATED IONIZATION RATE COEFFICIENTS

2009 ◽  
Vol 691 (2) ◽  
pp. 1540-1559 ◽  
Author(s):  
P. Bryans ◽  
E. Landi ◽  
D. W. Savin
Keyword(s):  
Ionization Rate ◽  
Rate Coefficients ◽  
Ionization Equilibrium ◽  
New Approach ◽  
Collisional Ionization ◽  
Equilibrium Calculations ◽  
Solar Coronal

scholarly journals Ionization Equilibrium for Ions of Na, Al, P, Cl, A, K, Ca, Cr and Mn

1972 ◽  
Vol 14 ◽  
pp. 586-587 ◽  
Author(s):  
M. Landini ◽  
B.C. Monsignori Fossi
Keyword(s):  
Solar Atmosphere ◽  
Radiative Recombination ◽  
Dielectronic Recombination ◽  
Ionization Equilibrium ◽  
Collisional Ionization ◽  
Ionization Balance ◽  
Equilibrium Calculations

Ionization equilibrium calculations, which have a number of astrophysical applications, have been computed by Jordan for the ions of C, N, O, Ne, Mg, Si, S, Fe, and Ni.The aim of this paper is to extend the evaluation to other elements relevant to the investigation of the solar atmosphere. Ions of Na, Al, P, Cl, A, K, Ca, Cr, and Mn have been considered and the ionization balance has been computed for temperature from 104 to 107 K.The computation is performed including collisional ionization, autoionization, radiative recombination and dielectronic recombination.

scholarly journals Collisional Ionization Equilibrium for Optically Thin Plasmas. I. Updated Recombination Rate Coefficients for Bare through Sodium‐like Ions

2006 ◽  
Vol 167 (2) ◽  
pp. 343-356 ◽  
Author(s):  
P. Bryans ◽  
N. R. Badnell ◽  
T. W. Gorczyca ◽  
J. M. Laming ◽  
W. Mitthumsiri ◽  
...  
Keyword(s):  
Recombination Rate ◽  
Rate Coefficients ◽  
Ionization Equilibrium ◽  
Collisional Ionization

THE IONIZATION RATE COEFFICIENTS FOR SOME RADIATIVELY EXCITED RUBIDIUM STATES

1979 ◽  
Vol 40 (C7) ◽  
pp. C7-87-C7-88
Author(s):  
A. N. Klucharev ◽  
A. V. Lazarenko ◽  
V. Vujnovic
Keyword(s):  
Ionization Rate ◽  
Rate Coefficients

scholarly journals ISM simulations: an overview of models

2012 ◽  
Vol 10 (H16) ◽  
pp. 606-608 ◽  
Author(s):  
M. A. de Avillez ◽  
D. Breitschwerdt ◽  
A. Asgekar ◽  
E. Spitoni
Keyword(s):  
Dynamical System ◽  
Interstellar Medium ◽  
Dynamical Evolution ◽  
Dynamic Processes ◽  
Ionization Equilibrium ◽  
Collisional Ionization

AbstractUntil recently the dynamical evolution of the interstellar medium (ISM) was simulated using collisional ionization equilibrium (CIE) conditions. However, the ISM is a dynamical system, in which the plasma is naturally driven out of equilibrium due to atomic and dynamic processes operating on different timescales. A step forward in the field comprises a multi-fluid approach taking into account the joint thermal and dynamical evolutions of the ISM gas.

scholarly journals XMM-Newton observations ofζOrionis (O9.7 Ib): a collisional ionization equilibrium model

2007 ◽  
Vol 478 (2) ◽  
pp. 513-520 ◽  
Author(s):  
A. J. J. Raassen ◽  
K. A. van der Hucht ◽  
N. A. Miller ◽  
J. P. Cassinelli
Keyword(s):  
Equilibrium Model ◽  
Ionization Equilibrium ◽  
Collisional Ionization

scholarly journals Evolution and State of the Local ISM

1996 ◽  
Vol 171 ◽  
pp. 442-442
Author(s):  
T. Schmutzler ◽  
D. Breitschwerdt
Keyword(s):  
Basic Feature ◽  
Emission Lines ◽  
Continuum Emission ◽  
Ionization Equilibrium ◽  
X Ray ◽  
Self Consistent ◽  
X Ray Background ◽  
Collisional Ionization ◽  
Consistent Approach ◽  
The Continuum

The most puzzling observations concerning the LISM (distance < 100 pc) can be explained by a fast adiabatically cooled gas in the cavity of an old superbubble. The ultrasoft X-ray background and contributions to the C- and M-bands are due to the continuum emission of delayed recombination [1]. In contrast to collisional ionization equilibrium (CIE) models, but consistent with recent observations [2], our model predicts a lack of emission lines and a low emissivity in the EUV range. In the figure below we compare the emissivities resulting from CIE at T = 106 K and those from our model at T = 4.2 × 104 K. The basic feature of our model is a thermally self-consistent approach of the time-dependent evolution.

scholarly journals Investigation of a Collisional Radiative Model for Laser-Produced Plasmas

Atoms ◽  
2020 ◽  
Vol 8 (3) ◽  
pp. 52
Author(s):  
Nicholas L. Wong ◽  
Fergal O’Reilly ◽  
Emma Sokell
Keyword(s):  
Radiative Recombination ◽  
Rate Coefficients ◽  
Ion Distribution ◽  
Ion Distributions ◽  
Nist Database ◽  
Collisional Radiative Model ◽  
Radiative Model ◽  
Collisional Ionization ◽  
Three Body ◽  
Body Recombination

Plasmas of a variety of types can be described by the collisional radiative (CR) model developed by Colombant and Tonan. From the CR model, the ion distribution of a plasma at a given electron temperature and density can be found. This information is useful for further simulations, and due to this, the employment of a suitable CR model is important. Specifically, ionization bottlenecks, where there are enhanced populations of certain charge states, can be seen in these ion distributions, which in some applications are important in maintaining large amounts of a specific ion. The present work was done by implementing an accepted CR model, proposed by Colombant and Tonon, in Python and investigating the effects of variations in the ionization energy and outermost electron subshell occupancy term on the positions of ionization bottlenecks. Laser Produced Plasmas created using a Nd:YAG laser with an electron density of ∼ne = 1021 cm−3 were the focus of this work. Plots of the collisional ionization, radiative recombination, and three-body recombination rate coefficients as well as the ion distribution and peak fractional ion population for various elements were examined. From these results, it is evident that using ionization energies from the NIST database and removing the orbital occupancy term in the CR model produced results with ionization bottlenecks in expected locations.

Ionization rate coefficients and induction times in nitrogen at high values ofE/N

1987 ◽  
Vol 36 (5) ◽  
pp. 2031-2040 ◽  
Author(s):  
G. N. Hays ◽  
L. C. Pitchford ◽  
J. B. Gerardo ◽  
J. T. Verdeyen ◽  
Y. M. Li
Keyword(s):  
Ionization Rate ◽  
Rate Coefficients ◽  
Induction Times

Effective Emission and Ionization Rate Coefficients of Atomic Carbons in Plasmas

1994 ◽  
Vol 63 (8) ◽  
pp. 2942-2954 ◽  
Author(s):  
Satoshi Sasaki ◽  
Yasuyuki Ohkouchi ◽  
Shuichi Takamura ◽  
Takako Kato
Keyword(s):  
Ionization Rate ◽  
Rate Coefficients

scholarly journals On the Interpretation of the Relative Intensities of the Solar XUV Lines of Lithium-Like Ions

1972 ◽  
Vol 14 ◽  
pp. 738-739
Author(s):  
D. R. Flower
Keyword(s):  
Cross Sections ◽  
Electron Excitation ◽  
Energy Separation ◽  
Temperature Structure ◽  
Isoelectronic Sequence ◽  
Ionization Equilibrium ◽  
Excitation Cross Sections ◽  
Powerful Means ◽  
Intensity Ratios ◽  
Equilibrium Calculations

The relative intensities of the 2s–2p and 2l–3l′ (l=0, l′= 1; l= 1, l′ = 0, 2) solar XUV lines of ions in the lithium isoelectronic sequence are sensitive to electron temperature because of the large energy separation of the 2p and 3/’ levels. Recent observations of these lines for three members of the sequence, O+5, Ne+7 and Mg+9 (Heroux and Cohen, 1971), consequently provide a potentially powerful means of studying the temperature structure of the upper chromosphere-corona transition region. These observations have been examined in the light of recent calculations of the electron excitation cross-sections for the relevant transitions (Flower, 1971). It is found that the observed intensity ratios are systematically greater than values calculated assuming that all the lines of a given ion are produced at essentially the same temperature, namely, the temperature for which the ionization equilibrium calculations of Jordan (1969) predict that emission in the lines is most highly favoured. Part of the discrepancy is removed if this assumption is dropped and the emission in each line is calculated separately before taking the ratio. These two calculations do not yield the same result because there is a high temperature tail in the ionization curve of the lithium-like ions which results in the transitions of higher excitation energy, the 2l–3l′ transitions, being enhanced relative to the 2s–2p transition. The unsatisfactory agreement between theory and observation could have important implications for current theories of the ionization equilibrium, but, before definite conclusions can be reached, further observations of the same type need to be made and remaining uncertainties in the cross-sections to be resolved.

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