Atomic transition probabilities :

Wiese, Wolfgang L.; Smith, Mary W.; Glennon, B. M.

doi:10.6028/nbs.nsrds.4

Cited by 774 publications

(669 citation statements)

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“…The collision parameters for excitation by neutral hydrogen atoms are taken from Störzer & Hollenbach (2000), those for excitation by free electrons from Mendoza (1983), and atomic parameters are from Wiese et al (1966) and Kafatos & Lynch (1980). We calculate the level population by solving the statistical equilibrium equations in a 5-level atom.…”

Section: Outflowing Disk Modelmentioning

confidence: 99%

Neutral material around the B[e] supergiant star LHA 115-S 65

Kraus¹,

Fernandes²,

Araújo³

2010

A&A

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Context. B[e] supergiants are surrounded by large amounts of hydrogen neutral material, traced by the emission in the optical [Oi] lines. This neutral material is most plausibly located within their dense, cool circumstellar disks, which are formed from the (probably non-spherically symmetric) wind material released by the star. Neither the formation mechanism nor the resulting structure and internal kinematics of these disks (or disk-like outflows) are well known. However, rapid rotation, lifting the material from the equatorial surface region, seems to play a fundamental role. Aims. The B[e] supergiant LHA 115-S 65 (in short: S 65) in the Small Magellanic Cloud is one of the two most rapidly rotating B[e] stars known. Its almost edge-on orientation allows a detailed kinematical study of its optically thin forbidden emission lines. With a focus on the rather strong [Oi] lines, we intend to test the two plausible disk scenarios: the outflowing and the Keplerian rotating disk. Methods. Based on high-and low-resolution optical spectra, we investigate the density and temperature structure in those disk regions that are traced by the [Oi] emission to constrain the disk sizes and mass fluxes needed to explain the observed [Oi] line luminosities. In addition, we compute the emerging line profiles expected for either an outflowing disk or a Keplerian rotating disk, which can directly be compared to the observed profiles. Results. Both disk scenarios deliver reasonably good fits to the line luminosities and profiles of the [Oi] lines. Nevertheless, the Keplerian disk model seems to be the more realistic one, because it also agrees with the kinematics derived from the large number of additional lines in the spectrum. As additional support for the presence of a high-density, gaseous disk, the spectrum shows two very intense and clearly double-peaked [Caii] lines. We discuss a possible disk-formation mechanism, and similarities between S 65 and the group of Luminous Blue Variables.

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Section: Outflowing Disk Modelmentioning

confidence: 99%

Neutral material around the B[e] supergiant star LHA 115-S 65

Kraus¹,

Fernandes²,

Araújo³

2010

A&A

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“…There is a reasonable body of evidence to valence electron, especially in alkali-metal atoms. For instance, transition probabilities calculated with the analytical eigenfunctions agree with experiment and with accepted values [8]. (Some recursion formulae for matrix elements are given in ref.…”

Section: Broken Supersymmetry and Quantum-defect Theorymentioning

confidence: 91%

Atomic Supersymmetry, Oscillators, and the Penning Trap

Kostelecký

1994

Symmetries in Science VII

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This paper begins with some background information and a summary of results in atomic supersymmetry. The connection between the supersymmetric Coulomb and oscillator problems in arbitrary dimensions is outlined. Next, I treat the issue of nding a description of supersymmetry-based quantum-defect theory in terms of oscillators. A model with an anharmonic term that yields analytical eigenfunctions is introduced to solve this problem in arbitrary dimensions. Finally, I show that geonium atoms (particles contained in a Penning trap) o er a realization of a multidimensional harmonic oscillator in an idealized limit. The anharmonic theory presented here provides a means of modeling the realistic case. Written in honor of Franco Iachello on his 50th birthdayPublished in the Festschrift volumè

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“…Emission spectra were recorded by scanning from 18500 to 22500 cm -1 in steps of 2.0 cm -1 using a slit width of 100 µm for 1 hr. Spectral frequencies were calibrated using He atomic lines, 15 which were recorded at the same time, and wavelengths are believed to be accurate to within ±1.0 cm -1 .…”

Section: Methodsmentioning

confidence: 99%

Alkyl Group Dissociation During Corona Excitation of Alkylbenzenes

Yoon¹,

Lee

2011

Journal of the Korean Chemical Society

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ABSTRACT. Well-resolved vibronic emission spectra were recorded in the visible region from the corona discharge of precursor alkylbenzenes in a technique of corona excited supersonic expansion using a pinhole-type glass nozzle. From the observed spectra, we found the evidence of the presence of benzyl-type radicals generated by dissociation of C-C or C-H bonds of alkyl group. After identification of benzyl-type radicals formed in the corona discharge, we suggest that energy densities in alkyl chain play a crucial role in determining the bond dissociation during corona excitation.

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Atomic transition probabilities :

Cited by 774 publications

References 0 publications

Neutral material around the B[e] supergiant star LHA 115-S 65

Neutral material around the B[e] supergiant star LHA 115-S 65

Atomic Supersymmetry, Oscillators, and the Penning Trap

Alkyl Group Dissociation During Corona Excitation of Alkylbenzenes

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