3D NLTE sodium abundance corrections relative to 1D LTE are typically negative and larger for saturated lines in giants, reaching -0.7 dex, with a public grid released for use.
Title resolution pending
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
representative citing papers
PySME v1.0 introduces a revised line-selection framework and updated hydrogen-line physics to enable scalable, high-precision stellar spectrum modeling for large surveys.
Derives Teff, log g and metallicity for 282 M dwarfs via χ² fits of updated PHOENIX models to simultaneous visible+NIR CARMENES spectra, finding visible and combined ranges superior to NIR alone.
New ESPRESSO transmission spectroscopy of GJ 436 b shows no detectable atmospheric features from H I, Na I, Fe I or other species, producing upper limits consistent with a featureless optical spectrum.
citing papers explorer
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3D NLTE Sodium abundances in late-type stars. Abundance corrections and synthetic spectra
3D NLTE sodium abundance corrections relative to 1D LTE are typically negative and larger for saturated lines in giants, reaching -0.7 dex, with a public grid released for use.
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PySME v1.0: improved modelling of stellar spectra for survey-scale applications
PySME v1.0 introduces a revised line-selection framework and updated hydrogen-line physics to enable scalable, high-precision stellar spectrum modeling for large surveys.
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The CARMENES search for exoplanets around M dwarfs -- Photospheric parameters of target stars from high-resolution spectroscopy. II. Simultaneous multiwavelength range modeling of activity insensitive lines
Derives Teff, log g and metallicity for 282 M dwarfs via χ² fits of updated PHOENIX models to simultaneous visible+NIR CARMENES spectra, finding visible and combined ranges superior to NIR alone.
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The atmosphere of the warm Neptune GJ 436 b probed with ESPRESSO
New ESPRESSO transmission spectroscopy of GJ 436 b shows no detectable atmospheric features from H I, Na I, Fe I or other species, producing upper limits consistent with a featureless optical spectrum.