Collision rates for electron excitation of Mg V lines

Collection:
Clark Atlanta University Faculty Publications
Title:
Collision rates for electron excitation of Mg V lines
Creator:
Zatsarinny, Oleg
Tayal, S.S.
Date of Original:
2015
Subject:
African Americans--Education (Higher)--Georgia
Clark Atlanta University
Location:
United States, Georgia, Fulton County, Atlanta, 33.749, -84.38798
Medium:
articles
Type:
Text
Format:
application/pdf
Description:
Abstract: Transition probabilities and electron impact excitation collision strengths and rates for astrophysically important lines in Mg V are reported. The 86 fine-structure levels of the 2s22p4 , 2s2p5 , 2p6 , 2s22p3 3s, 2s22p3 3p and 2s2 2p33d configurations are included in our calculations. The e?ective collision strengths are presented as a function of electron temperature for solar and other astrophysical applications. Methods. The collision strengths have been calculated using the B-spline Breit-Pauli R-matrix method for all fine-structure transi- tions among the 86 levels. The one-body mass, Darwin and spin-orbit relativistic e?ects are included in the Breit-Pauli Hamiltonian in the scattering calculations. The one-body and two-body relativistic operators are included in the multiconfiguration Hartree-Fock calculations of transition probabilities. Several sets of non-orthogonal spectroscopic and correlation radial orbitals are used to obtain accurate description of Mg V 86 levels and to represent the scattering functions. Results. The calculated excitation energies are in very good agreement with experiment and represents an improvement over the pre- vious calculations. The present collision strengths show good agreement with the previously available R-matrix and distorted-wave calculations. The oscillator strengths for E1 transitions normally compare very well with previous calculations. The thermally aver- aged collision strengths are obtained by integrating total resonant and non-resonant collision strengths over a Maxwellian distribution of electron energies and these are presented over the temperature range log10 Te = 3.2?6.0 K.
Source: Astronomy & Astrophysics
DOI: https://doi.org/10.1051/0004-6361/201425135
Metadata URL:
http://hdl.handle.net/20.500.12322/cau.ir:2015_zatsarinny_oleg
Language:
eng
Original Collection:
Clark Atlanta University Faculty Publications
Holding Institution:
Clark Atlanta University
Rights:

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