Wavelengths and transition probabilities for atoms and atomic ions :

Reader, Joseph; Corliss, Charles; Wiese, Wolfgang L.; Martin, G.

doi:10.6028/nbs.nsrds.68

Cited by 242 publications

(189 citation statements)

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“…The literature sources are the NIST database, version 4 (NIST4), and Zíelińska et al (2002) (ZBD). Zíelińska et al (2002) estimate that, in general, their experimental transition rates agree with the NIST critical compilation made by Reader et al (1980), which is the one adopted in the NIST4 database.…”

Section: Stellar Wavelengths and The Astrophysical Log Gf -Values Forsupporting

confidence: 61%

Wavelengths and oscillator strengths of Xe II from the UVES spectra of four HgMn stars

Yüce

Castelli

Hubrig

2011

A&A

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Aims. In spite of large overabundances of Xe ii observed in numerous mercury-manganese (HgMn) stars, Xe ii oscillator strengths are only available for a very limited number of transitions. As a consequence, several unidentified lines in the spectra of HgMn stars could be due to Xe ii. In addition, some predicted Xe ii lines are redshifted by about 0.1 Å from stellar unidentified lines, raising the question about the wavelength accuracy of the Xe ii line data available in the literature. For these reasons we investigated the Xe ii lines lying in the 3900-4521 Å, 4769-7542 Å, and 7660-8000 Å spectral ranges of four well-studied HgMn stars. Methods. We compared the Xe ii wavelengths listed in the NIST database with the position of the lines observed in the high-resolution UVES spectrum of the xenon-overabundant, slowly rotating HgMn star HR 6000, and we modified them when needed. We derived astrophysical oscillator strengths for all the Xe ii observed lines and compared them with the literature values, when available. We checked the stellar atomic data derived from HR 6000 by using them to compute synthetic spectra for three other xenon-overabundant, slowly rotating HgMn stars, HD 71066, 46 Aql, and HD 175640. In this framework, we performed a complete abundance analysis of HD 71066, while we relied on our previous works for the other stars. Results. We find that all the lines with wavelengths related to the 6d and 7s energy levels have a corresponding unidentified spectral line, blueshifted by the same quantity of about 0.1 Å in all the four stars, so that we identified these lines as coming from Xe ii and modified their NIST wavelength value according to the observed stellar value. We find that the Xe ii stellar oscillator strengths may differ from one star to another from 0.0 dex to 0.3 dex. We adopted the average of the oscillator strengths derived from the four stars as final astrophysical oscillator strength.

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Section: Stellar Wavelengths and The Astrophysical Log Gf -Values Forsupporting

confidence: 61%

Wavelengths and oscillator strengths of Xe II from the UVES spectra of four HgMn stars

Yüce

Castelli

Hubrig

2011

A&A

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“…The detailed identification of weak absorption lines in the *Visiting Professor at Cornell University, Department of Astronomy. region of doublet 2800 Mg n, in the interval of 2790 Â-2810 Á, is carried out using Kelly (1979) and Reader et al (1980). The results are given in Table 2.…”

Section: Identification Of Weak Absorption Linesmentioning

confidence: 99%

The MG II H and K interstellar lines in the spectrum of the G-type giant HD 156854

Gurzadian

Cholakian²,

Kondo

et al. 1990

PASP

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The results of the measurements and analysis of the IUE observations of the 2800 Mg II doublet in the spectrum of HD 156854, a G9 III star, are presented. The relative power of the magnesium chromosphere, fí Mg = 1.0 X 10~5, is in agreement with the known data for giants of the same class. The emission profiles of this doublet present absorption cores, which are of interstellar origin. Taking into account the interstellar depletion of Mg, the derived density of interstellar hydrogen is n(H) = 1.0 cm -3 , which agrees with the conclusion (Paresce 1984) about the possibility of large hydrogen concentrations in some directions of the Galaxy far from the Sun.

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“…nor argon gas was identified. In one of the experiments with a relatively high ambient pressure (0.13 bar) of an argon atmosphere, two spectrometers covered the spectral range between 405 and 440 nm, where argon atoms have very strong emission lines [e.g., Reader et al, 1980]. Still, only the CN band emission was observed in this spectral range (Figure 2).…”

Section: Spectral Contentmentioning

confidence: 99%

“…The behavior of these volatile elements upon impact vaporization is of great importance. However, energy levels for the lowest excitation state of these atoms are very high [e.g., Reader et al, 1980]. Thus, despite the ease of evaporation, they do not necessarily emit strong atomic line emission in the range of temperatures produced in hypervelocity impacts in a laboratory.…”

Section: Introductionmentioning

confidence: 99%

Interactions between impact‐induced vapor clouds and the ambient atmosphere: 1. Spectroscopic observations using diatomic molecular emission

Sugita

Schultz

2003

J. Geophys. Res.

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[1] The importance of interactions between impact-induced vapor clouds and an ambient atmosphere has been widely recognized, and theoretical approaches have provided significant insights. Few experiments, however, have been done to observe directly the energy partitioning during the interactions between impact vapor clouds and the ambient atmosphere. The present study attempts to understand the difference between actual and theoretical model impact vapor clouds produced under an atmosphere. A series of hypervelocity impact experiments was conducted using a spectroscopic measurement method. Plastic (polycarbonate) impactors allowed simulating vaporization phenomena associated with natural impactors (e.g., silicates and metals) at high impact velocities into water. Water as the target material served to suppress the effect of fine-grained fragments from the target. Emission spectra of the leading part of downrange-moving impact vapor clouds were captured with high-speed spectrometers as a function of time for various ambient pressures. The emission spectra exhibit strong molecular bands from carbon compounds as well as blackbody continuum radiation. In order to estimate the temperature of the radiation source, we carried out a spectral-form inversion analysis based on diatomic emission theory. Obtained molecular radiation temperatures range from 4500 K to 5500 K with relatively high accuracy ($2%) and place a number of well-defined constraints for the radiation source. A simple theoretical model that is often assumed for an impact-induced vapor cloud, however, does not readily satisfy the constraints. This strongly suggests that real impact-induced vapor clouds may be more complex than previously thought.INDEX TERMS: 5420 Planetology: Solid Surface Planets: Impact phenomena (includes cratering); 5407 Planetology: Solid Surface Planets: Atmospheres-evolution; 5455 Planetology: Solid Surface Planets: Origin and evolution; 5494 Planetology: Solid Surface Planets: Instruments and techniques; 6022 Planetology: Comets and Small Bodies: Impact phenomena; KEYWORDS: Impact cratering, impact experiments, impact vaporization, impact flash spectroscopy, molecular emission Citation: Sugita, S., and P. H. Schultz, Interactions between impact-induced vapor clouds and the ambient atmosphere: 1.

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Wavelengths and transition probabilities for atoms and atomic ions :

Cited by 242 publications

References 0 publications

Wavelengths and oscillator strengths of Xe II from the UVES spectra of four HgMn stars

Wavelengths and oscillator strengths of Xe II from the UVES spectra of four HgMn stars

The MG II H and K interstellar lines in the spectrum of the G-type giant HD 156854

Interactions between impact‐induced vapor clouds and the ambient atmosphere: 1. Spectroscopic observations using diatomic molecular emission

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