Add to ORKGThe possibility that unknown sources of opacity may exist in the M2V spectral class star, HD 95735, has been investigated. The factor by which the known sources of opacity should be multiplied to obtain the opacity obtaining in the star is estimated by comparing the total pressure obtained from model atmosphere and that from pressure broadened wings of λ4227 line of Ca I. This factor is close to unity if the effective temperature of the star is about 3400°K, and it increases for lower effective temperatures. The effect of metal abundance has also been considered
Dense, He-rich atmospheres of cool white dwarfs represent a challenge to the modeling. This is becau...
International audienceThe influence of Stark broadening in ionized chromium spectral lines observed ...
The Sun and ? Cen A and B are the nearest stars to us. Despite the general agreement between their m...
The possibility that unknown sources of opacity may exist in the M2V spectral class star, HD 957...
As stars evolve, their surfaces may be altered by several different mechanisms. These introduce dist...
The model atmosphere code Sterne, first developed in the 1970s to study hydrogen-deficient stars, ha...
The model atmosphere code STERNE has evolved considerably over the years. Most recently, attention h...
Opacity enhancements for stellar interior conditions have been explored to explain observed pulsatio...
An in-depth analysis of the stellar matter resistance to energy transport, the opacity, in the cont...
Collision-induced absorption (CIA) from molecular hydrogen is a dominant opacity source in the atmos...
International audienceAn overview is presented of calculations of stellar opacities in the transitio...
The problem of the fundamental atmospheric parameters of main-sequence A and F stars has been invest...
Context. Spectroscopic analysis remains the most common method to derive masses of massive stars, th...
The influence of the new MAFAGS-OS opacity sampling model atmosphere and its changed thermal struc...
We present a series of papers with the central theme of molecular band spectrum synthesis of cool s...
Dense, He-rich atmospheres of cool white dwarfs represent a challenge to the modeling. This is becau...
International audienceThe influence of Stark broadening in ionized chromium spectral lines observed ...
The Sun and ? Cen A and B are the nearest stars to us. Despite the general agreement between their m...
The possibility that unknown sources of opacity may exist in the M2V spectral class star, HD 957...
As stars evolve, their surfaces may be altered by several different mechanisms. These introduce dist...
The model atmosphere code Sterne, first developed in the 1970s to study hydrogen-deficient stars, ha...
The model atmosphere code STERNE has evolved considerably over the years. Most recently, attention h...
Opacity enhancements for stellar interior conditions have been explored to explain observed pulsatio...
An in-depth analysis of the stellar matter resistance to energy transport, the opacity, in the cont...
Collision-induced absorption (CIA) from molecular hydrogen is a dominant opacity source in the atmos...
International audienceAn overview is presented of calculations of stellar opacities in the transitio...
The problem of the fundamental atmospheric parameters of main-sequence A and F stars has been invest...
Context. Spectroscopic analysis remains the most common method to derive masses of massive stars, th...
The influence of the new MAFAGS-OS opacity sampling model atmosphere and its changed thermal struc...
We present a series of papers with the central theme of molecular band spectrum synthesis of cool s...
Dense, He-rich atmospheres of cool white dwarfs represent a challenge to the modeling. This is becau...
International audienceThe influence of Stark broadening in ionized chromium spectral lines observed ...
The Sun and ? Cen A and B are the nearest stars to us. Despite the general agreement between their m...