The Experts below are selected from a list of 207 Experts worldwide ranked by ideXlab platform
M. Raineri - One of the best experts on this subject based on the ideXlab platform.
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Stellar laboratories - V. The Xe vi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503−289
Astronomy and Astrophysics, 2015Co-Authors: Thomas Rauch, D. Hoyer, Pascal Quinet, M. Gallardo, M. RaineriAbstract:For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation. Reliable Xe VI oscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarf RE0503-289 and to determine its photospheric Xe abundance. We publish newly calculated oscillator strengths that are based on a recently measured Xe VI laboratory line Spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe VI lines exhibited in high-resolution and high S/N UV observations of RE0503-289. We identify three hitherto unknown Xe VI lines in the Ultraviolet Spectrum of RE0503-289 and confirm the previously measured photospheric Xe abundance of this white dwarf (log Xe = -4.2 +/- 0.6). Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe VI line profiles in the Ultraviolet Spectrum of the white dwarf RE0503-289 were well reproduced with the newly calculated Xe VI oscillator strengths.
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Stellar laboratories V. The Xe vi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE0503289 , (Research Note)
2015Co-Authors: Thomas Rauch, Pascal Quinet, M. Gallardo, M. RaineriAbstract:Context. For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced nonlocal thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation. Aims. Reliable Xe vi oscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarf RE 0503−289 and to determine its photospheric Xe abundance. Methods. We publish newly calculated oscillator strengths that are based on a recently measured Xe vi laboratory line Spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe vi lines exhibited in high-resolution and high S/N UV observations of RE 0503−289. Results. We identify three hitherto unknown Xe vi lines in the Ultraviolet Spectrum of RE 0503−289 and confirm the previously measured photospheric Xe abundance of this white dwarf (log Xe = −4.2 ± 0.6 by mass). Conclusions. Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe vi line profiles in the Ultraviolet Spectrum of the white dwarf RE 0503−289 were well reproduced with the newly calculated Xe vi oscillator strengths.
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Stellar laboratories (Research Note) V. The Xevi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503 289 ⋆, ⋆⋆
2015Co-Authors: Thomas Rauch, D. Hoyer, Pascal Quinet, M. Gallardo, M. RaineriAbstract:Centro de Investigaciones Opticas (CIOp), CC 3, 1897, Gonnet, La Plata, ArgentinaReceived 12 March 2015; accepted 2015ABSTRACTContext. For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-localthermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomicdata that is used for their calculation.Aims. Reliable Xevioscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarfRE0503−289 and to determine its photospheric Xe abundance.Methods. Based on a recently measured Xevilaboratory line Spectrum, newly calculated oscillator strengths were published. Thesewere used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for theanalysis of Xevilines exhibited in high-resolution and high-S/N UV observations of RE0503−289.Results. We identified three hitherto unknown Xe vilines in the Ultraviolet Spectrum of RE0503−289 and confirmed its previouslymeasured photospheric Xe abundance (−4.2 ±0.6 by mass).Conclusions. Reliable measurements and calculations of atomic data are a pre-requisite for stellar-atmosphere modeling. ObservedXeviline profiles in the Ultraviolet Spectrum of the white dwarf R E0503−289 were well reproduced with the newly calculated Xevioscillator strengths.Key words.
Thomas Rauch - One of the best experts on this subject based on the ideXlab platform.
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Stellar laboratories - V. The Xe vi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503−289
Astronomy and Astrophysics, 2015Co-Authors: Thomas Rauch, D. Hoyer, Pascal Quinet, M. Gallardo, M. RaineriAbstract:For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation. Reliable Xe VI oscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarf RE0503-289 and to determine its photospheric Xe abundance. We publish newly calculated oscillator strengths that are based on a recently measured Xe VI laboratory line Spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe VI lines exhibited in high-resolution and high S/N UV observations of RE0503-289. We identify three hitherto unknown Xe VI lines in the Ultraviolet Spectrum of RE0503-289 and confirm the previously measured photospheric Xe abundance of this white dwarf (log Xe = -4.2 +/- 0.6). Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe VI line profiles in the Ultraviolet Spectrum of the white dwarf RE0503-289 were well reproduced with the newly calculated Xe VI oscillator strengths.
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Stellar laboratories V. The Xe vi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE0503289 , (Research Note)
2015Co-Authors: Thomas Rauch, Pascal Quinet, M. Gallardo, M. RaineriAbstract:Context. For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced nonlocal thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation. Aims. Reliable Xe vi oscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarf RE 0503−289 and to determine its photospheric Xe abundance. Methods. We publish newly calculated oscillator strengths that are based on a recently measured Xe vi laboratory line Spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe vi lines exhibited in high-resolution and high S/N UV observations of RE 0503−289. Results. We identify three hitherto unknown Xe vi lines in the Ultraviolet Spectrum of RE 0503−289 and confirm the previously measured photospheric Xe abundance of this white dwarf (log Xe = −4.2 ± 0.6 by mass). Conclusions. Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe vi line profiles in the Ultraviolet Spectrum of the white dwarf RE 0503−289 were well reproduced with the newly calculated Xe vi oscillator strengths.
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Stellar laboratories (Research Note) V. The Xevi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503 289 ⋆, ⋆⋆
2015Co-Authors: Thomas Rauch, D. Hoyer, Pascal Quinet, M. Gallardo, M. RaineriAbstract:Centro de Investigaciones Opticas (CIOp), CC 3, 1897, Gonnet, La Plata, ArgentinaReceived 12 March 2015; accepted 2015ABSTRACTContext. For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-localthermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomicdata that is used for their calculation.Aims. Reliable Xevioscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarfRE0503−289 and to determine its photospheric Xe abundance.Methods. Based on a recently measured Xevilaboratory line Spectrum, newly calculated oscillator strengths were published. Thesewere used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for theanalysis of Xevilines exhibited in high-resolution and high-S/N UV observations of RE0503−289.Results. We identified three hitherto unknown Xe vilines in the Ultraviolet Spectrum of RE0503−289 and confirmed its previouslymeasured photospheric Xe abundance (−4.2 ±0.6 by mass).Conclusions. Reliable measurements and calculations of atomic data are a pre-requisite for stellar-atmosphere modeling. ObservedXeviline profiles in the Ultraviolet Spectrum of the white dwarf R E0503−289 were well reproduced with the newly calculated Xevioscillator strengths.Key words.
Pascal Quinet - One of the best experts on this subject based on the ideXlab platform.
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Stellar laboratories - V. The Xe vi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503−289
Astronomy and Astrophysics, 2015Co-Authors: Thomas Rauch, D. Hoyer, Pascal Quinet, M. Gallardo, M. RaineriAbstract:For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation. Reliable Xe VI oscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarf RE0503-289 and to determine its photospheric Xe abundance. We publish newly calculated oscillator strengths that are based on a recently measured Xe VI laboratory line Spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe VI lines exhibited in high-resolution and high S/N UV observations of RE0503-289. We identify three hitherto unknown Xe VI lines in the Ultraviolet Spectrum of RE0503-289 and confirm the previously measured photospheric Xe abundance of this white dwarf (log Xe = -4.2 +/- 0.6). Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe VI line profiles in the Ultraviolet Spectrum of the white dwarf RE0503-289 were well reproduced with the newly calculated Xe VI oscillator strengths.
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Stellar laboratories V. The Xe vi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE0503289 , (Research Note)
2015Co-Authors: Thomas Rauch, Pascal Quinet, M. Gallardo, M. RaineriAbstract:Context. For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced nonlocal thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation. Aims. Reliable Xe vi oscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarf RE 0503−289 and to determine its photospheric Xe abundance. Methods. We publish newly calculated oscillator strengths that are based on a recently measured Xe vi laboratory line Spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe vi lines exhibited in high-resolution and high S/N UV observations of RE 0503−289. Results. We identify three hitherto unknown Xe vi lines in the Ultraviolet Spectrum of RE 0503−289 and confirm the previously measured photospheric Xe abundance of this white dwarf (log Xe = −4.2 ± 0.6 by mass). Conclusions. Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe vi line profiles in the Ultraviolet Spectrum of the white dwarf RE 0503−289 were well reproduced with the newly calculated Xe vi oscillator strengths.
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Stellar laboratories (Research Note) V. The Xevi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503 289 ⋆, ⋆⋆
2015Co-Authors: Thomas Rauch, D. Hoyer, Pascal Quinet, M. Gallardo, M. RaineriAbstract:Centro de Investigaciones Opticas (CIOp), CC 3, 1897, Gonnet, La Plata, ArgentinaReceived 12 March 2015; accepted 2015ABSTRACTContext. For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-localthermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomicdata that is used for their calculation.Aims. Reliable Xevioscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarfRE0503−289 and to determine its photospheric Xe abundance.Methods. Based on a recently measured Xevilaboratory line Spectrum, newly calculated oscillator strengths were published. Thesewere used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for theanalysis of Xevilines exhibited in high-resolution and high-S/N UV observations of RE0503−289.Results. We identified three hitherto unknown Xe vilines in the Ultraviolet Spectrum of RE0503−289 and confirmed its previouslymeasured photospheric Xe abundance (−4.2 ±0.6 by mass).Conclusions. Reliable measurements and calculations of atomic data are a pre-requisite for stellar-atmosphere modeling. ObservedXeviline profiles in the Ultraviolet Spectrum of the white dwarf R E0503−289 were well reproduced with the newly calculated Xevioscillator strengths.Key words.
M. Gallardo - One of the best experts on this subject based on the ideXlab platform.
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Stellar laboratories - V. The Xe vi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503−289
Astronomy and Astrophysics, 2015Co-Authors: Thomas Rauch, D. Hoyer, Pascal Quinet, M. Gallardo, M. RaineriAbstract:For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation. Reliable Xe VI oscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarf RE0503-289 and to determine its photospheric Xe abundance. We publish newly calculated oscillator strengths that are based on a recently measured Xe VI laboratory line Spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe VI lines exhibited in high-resolution and high S/N UV observations of RE0503-289. We identify three hitherto unknown Xe VI lines in the Ultraviolet Spectrum of RE0503-289 and confirm the previously measured photospheric Xe abundance of this white dwarf (log Xe = -4.2 +/- 0.6). Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe VI line profiles in the Ultraviolet Spectrum of the white dwarf RE0503-289 were well reproduced with the newly calculated Xe VI oscillator strengths.
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Stellar laboratories V. The Xe vi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE0503289 , (Research Note)
2015Co-Authors: Thomas Rauch, Pascal Quinet, M. Gallardo, M. RaineriAbstract:Context. For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced nonlocal thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation. Aims. Reliable Xe vi oscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarf RE 0503−289 and to determine its photospheric Xe abundance. Methods. We publish newly calculated oscillator strengths that are based on a recently measured Xe vi laboratory line Spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe vi lines exhibited in high-resolution and high S/N UV observations of RE 0503−289. Results. We identify three hitherto unknown Xe vi lines in the Ultraviolet Spectrum of RE 0503−289 and confirm the previously measured photospheric Xe abundance of this white dwarf (log Xe = −4.2 ± 0.6 by mass). Conclusions. Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe vi line profiles in the Ultraviolet Spectrum of the white dwarf RE 0503−289 were well reproduced with the newly calculated Xe vi oscillator strengths.
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Stellar laboratories (Research Note) V. The Xevi Ultraviolet Spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503 289 ⋆, ⋆⋆
2015Co-Authors: Thomas Rauch, D. Hoyer, Pascal Quinet, M. Gallardo, M. RaineriAbstract:Centro de Investigaciones Opticas (CIOp), CC 3, 1897, Gonnet, La Plata, ArgentinaReceived 12 March 2015; accepted 2015ABSTRACTContext. For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-localthermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomicdata that is used for their calculation.Aims. Reliable Xevioscillator strengths are used to identify Xe lines in the Ultraviolet Spectrum of the DO-type white dwarfRE0503−289 and to determine its photospheric Xe abundance.Methods. Based on a recently measured Xevilaboratory line Spectrum, newly calculated oscillator strengths were published. Thesewere used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for theanalysis of Xevilines exhibited in high-resolution and high-S/N UV observations of RE0503−289.Results. We identified three hitherto unknown Xe vilines in the Ultraviolet Spectrum of RE0503−289 and confirmed its previouslymeasured photospheric Xe abundance (−4.2 ±0.6 by mass).Conclusions. Reliable measurements and calculations of atomic data are a pre-requisite for stellar-atmosphere modeling. ObservedXeviline profiles in the Ultraviolet Spectrum of the white dwarf R E0503−289 were well reproduced with the newly calculated Xevioscillator strengths.Key words.
Zhang Guo-wen - One of the best experts on this subject based on the ideXlab platform.
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Study on Ultraviolet Spectrum Property of Lomefloxacin Chlorhydric Acid and Its Application in the B-R Buffer Medium
Journal of Nanchang University, 2005Co-Authors: Zhang Guo-wenAbstract:In the pH range of 1.89-11.58 Britton-Robinson buffer solutions,the lomefloxacin chlorhydric acid(LOM) Ultraviolet Spectrum property was studied,and the mechanism of the absorption spectra shift was discussed.The best condition in detecting LOM by Ultraviolet spectrophotometry is proposed.The absorption maxima of the drug lies at 286 nm,The linear range of LOM is 1.0~23.0 mg·L~(-1),the limit of detection is 0.59 mg·L~(-1),and the apparent molar absorptivity is 3.12×10~4 L· mol~(-1)· cm~(-1).The method was successfully applied to the determination of LOM in tabloids with satisfied results.
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Ultraviolet Spectrum PROPERTY OF EVOFLOXACINLACTATE AND ITS APPLICATION
Journal of Nanchang University, 2004Co-Authors: Zhang Guo-wenAbstract:In the pH range of 1.89 - 11.58 Britton-Robinson buffer solutions, the Levofloxacin lactate Ultraviolet Spectrum property was studied , and the reason of the absorption spectra shift was discussed. The best condition in detecting Levofloxacin lactate by Ultraviolet spectrophotometry is proposed. The absorption maxima of the drug lies at 292 nm, The linear range of Levofloxacin lactate is 1.0-23.0 mg·L~(-1), the limit of detection is 0.565 mg·L~(-1), and the apparent molar absorptivity is 3.4×10~4 L· mol~(-1)· cm~(-1).The method was successfully applied to the determination of Levofloxacin lactate in tabloids with satisfied results.
