The neutral oxygen spectrum. 1: Collisionally excited level populations and line intensities under optically thin conditions

Bhatia, A. K.; Kastner, S. O.

doi:10.1086/192121

Cited by 54 publications

(30 citation statements)

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“…Although these approximate formulas are relatively old, a review of recent astrophysics 23,24,24,25,26 and plasma physics 16,27 literature reveals that in the absence of experimental data or detailed calculations, these approximate formulas are the best available alternative. These approximate formulas will be compared with detailed calculations in the following paragraphs.…”

Section: A) Electron-impact Excitationmentioning

confidence: 99%

Non-Boltzmann Modeling for Air Shock-Layer Radiation at Lunar-Return Conditions

Johnston

Hollis

Sutton

2008

Journal of Spacecraft and Rockets

110

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This paper investigates the non-Boltzmann modeling of the radiating atomic and molecular electronic states present in lunar-return shock-layers. The Master Equation is derived for a general atom or molecule while accounting for a variety of excitation and de-excitation mechanisms. A new set of electronic-impact excitation rates is compiled for N, O, and N 2 + , which are the main radiating species for most lunar-return shock-layers. Based on these new rates, a novel approach of curve-fitting the non-Boltzmann populations of the radiating atomic and molecular states is developed. This new approach provides a simple and accurate method for

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Section: A) Electron-impact Excitationmentioning

confidence: 99%

Non-Boltzmann Modeling for Air Shock-Layer Radiation at Lunar-Return Conditions

Johnston

Hollis

Sutton

2008

Journal of Spacecraft and Rockets

110

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“…Bhatia & Kastner (1995) have further developed this method and derived an explicit graph of the I 1641 /I 1302 ratio as function of log τ 1302 . In the specific case of RR Tel they have used the measurements in IUE spectra by Penston et al (1983) and derived log τ 1302 ∼ 6.0.…”

Section: The Large Optical Depths In the O I Resonance Linesmentioning

confidence: 99%

The He$\rm_{II}$ Fowler lines and the O$\rm_{III}$ and N$\rm_{III}$ Bowen fluorescence lines in the symbiotic nova RR Telescopii

Selvelli¹,

Danziger²,

Bonifacio³

2007

A&A

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“…Data for Balmer line emissivities were taken from Storey & Hummer (1995). Emissivities for neutral and ionic oxygen were computed using spontaneous emission coefficients from Wiese et al (1996) and collision strengths from various sources (Pradhan 1976;McLaughlin & Bell 1993;Lennon & Burke 1994;Bhatia & Kastner 1995). The total oxygen abundance by number, N (O)/N (H), is obtained from the sum…”

Section: Oxygen Abundancesmentioning

confidence: 99%

Uncovering Additional Clues to Galaxy Evolution. I. Dwarf Irregular Galaxies in the Field

Lee

McCall

Kingsburgh

et al. 2003

The Astronomical Journal

156

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In order to recognize environmental effects on the evolution of dwarf galaxies in clusters of galaxies, it is first necessary to quantify the properties of objects which have evolved in relative isolation. With oxygen abundance as the gauge of metallicity, two key diagnostics of the evolution of dwarf irregular galaxies in the field are re-examined: the metallicity-luminosity relationship and the metallicity-gas fraction relationship. Gas fractions are evaluated from the masses of luminous components only, i.e., constituents of the nucleogenetic pool. Results from new optical spectroscopy obtained for H II regions in five dwarf irregular galaxies in the Local Volume are incorporated into a new analysis of field dwarfs with [O III]λ4363 detections and good distances. The updated fit to the metallicity-luminosity relationship is consistent with results reported in the literature. The fit to the metallicity-gas fraction relation shows an excellent correlation consistent with expectations of the simple "closed box" model of chemical evolution. The simplest explanation consistent with the data is that flow rates are zero, although the observations allow for the possibility of modest flows. The derived oxygen yield is one-quarter of the value for the solar neighbourhood. 6 Low-luminosity ellipticals or LLEs (e.g., M32) are structurally similar to giant ellipticals and exhibit a trend of decreasing surface brightness with increasing luminosity.

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The neutral oxygen spectrum. 1: Collisionally excited level populations and line intensities under optically thin conditions

Cited by 54 publications

References 0 publications

Non-Boltzmann Modeling for Air Shock-Layer Radiation at Lunar-Return Conditions

Non-Boltzmann Modeling for Air Shock-Layer Radiation at Lunar-Return Conditions

The He$\rm_{II}$ Fowler lines and the O$\rm_{III}$ and N$\rm_{III}$ Bowen fluorescence lines in the symbiotic nova RR Telescopii

Uncovering Additional Clues to Galaxy Evolution. I. Dwarf Irregular Galaxies in the Field

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