We release the first grid of stellar limb-darkening coefficients (LDCs) and intensity profiles (IPs) computed by the consortium of the PLAnetary Transits and...
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PublicaciónFirst Release of PLATO Consortium Stellar Limb-darkening Coefficients
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PublicaciónHigh resolution spectroscopy of central stars of planetary nebulae. I - Basic atmospheric parameters and their interpretation
The authors have obtained high-resolution spectrograms of H-rich central stars of planetary nebulae (CSPN) with the 3.6 m telescope and Cassegrain echelle...
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PublicaciónHigh-speed infrared photometry of rapidly oscillating AP (roAp) stars - 10 Aquilae
High-speed photometric observations of the recently discovered roAp star 10 Aql were performed in the J(1.22-micrometer) filter. A total of 47.2 hours of data...
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CharlaIAU G5 -- The GALAH survey: science goals and highlights to date
The field of Galactic archaeology has been very active in recent years, with a major influx of data from the Gaia satellite and large spectroscopic surveys. The...
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CharlaIAU G5 talk: Stellar chemical compositions with 3D non-LTE models
Spectroscopic analyses of stellar chemical compositions are model-dependent, and shortcomings in the models often limit the accuracy of the final results. For...
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CharlaIAU G5 Talk: Winds of Magnetic Massive Stars
Massive stars (at least eight times as massive as the Sun) possess strong stellar winds driven by radiation. With the advent of the so called MiMeS...
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CharlaIAU G5: "Extreme Precision Stellar Spectroscopy"
The new generation of spectrometers designed for extreme precision radial velocities enable correspondingly precise stellar spectroscopy. It is now fruitful to...
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PublicaciónImproved NLTE profiles of He II lines in hot stars including their overlap with hydrogen
The accelerated Lambda iteration method is used to obtain better theoretical profiles of He II in hot stars by considering more levels and Stark broadening in...
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PublicaciónImproved non-LTE Balmer-line profiles for hot stars
Improved non-LTE line formation calculations for hydrogen in O-stars are presented. The calculations are carried out by means of the method recently developed...