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Metal abundances of sdB stars
Hot subdwarf B stars (sdBs) are considered to be core helium-burning stars with very thin hydrogen envelopes situated on or near the extreme horizontal branch (EHB). The... -
Age and colors of massive white dwarf stars
We present evolutionary calculations and colors for massive white dwarfs with oxygen-neon cores for masses between 1.06 and 1.28M_{sun}. The evolutionary stages computed cover... -
O-M stars model atmospheres
Broad band colors and bolometric corrections in the Johnson-Cousins-Glass system (Bessell, 1990PASP..102.1181B; Bessell & Brett, 1988PASP..100.1134B) have been computed from... -
Limb-darkening for Space Mission GAIA
In the past few years, the number of space missions with astrophysical purposes has increased, with COROT, KEPLER, MOST and more recently TESS. Two of the most important... -
O/Fe abundances of 15 RR Lyrae
In order to study how the conventional spectroscopic method based on the equivalent widths of the Fe I and Fe II lines effectively applies to determining the atmospheric... -
Full Evolutionary Sequences of Massive WDs
We explore the evolution of hydrogen-rich and hydrogen-deficient white dwarf stars with masses between 1.012 and 1.307M_{sun}, and initial metallicity of Z=0.02. These sequences... -
Chromospheric Ca II emission in nearby stars
We present chromospheric CaII H and K activity measurements, rotation periods, and ages for ~1200 F, G, K, and M type main-sequence stars from ~18000 archival spectra taken at... -
Synthetic spectra of dark stars
The first stars in the history of the Universe are likely to form in the dense central regions of {sim.to}10^5^-10^6^ M_{sun} cold dark matter halos at z{approx}10--50. The... -
X-ray spectra of bursting neutron stars
X-ray burst sources represent a class of accreting neutron stars in close binary systems which do not exhibit any traces of the magnetic field. We present new method of hot... -
CO and HCN observations of circumstellar envelopes
We have searched the literature for all observations of the ^12^CO(1-0), ^12^CO(2-1), and HCN(1-0) lines in circumstellar envelopes of late type stars published between January... -
Heterochromatic extinction. I.
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Entropy-calibrated stellar modeling
Modeling the convection process is a long-standing problem in stellar physics. To date, all ad hoc models have relied on a free parameter, alpha, (among others) that has no real... -
Power-2 limb-darkening coefficients
The phenomenon of limb-darkening is relevant to many topics in astrophysics, including the analysis of light curves of eclipsing binaries, optical interferometry, measurement of... -
3D GCMs mini-chemical scheme with net reactions
Growing evidence has indicated that the global composition distribution plays an indisputable role in interpreting observational data. Three-dimensional general circulation... -
Power-2 limb-darkening law from STAGGER-grid
Inaccurate limb-darkening models can be a significant source of error in the analysis of the light curves for transiting exoplanet and eclipsing binary star systems,... -
Spectral models for binary products
Stars stripped of their hydrogen-rich envelope through interaction with a binary companion are generally not considered when accounting for ionizing radiation from stellar... -
3D correction in 5 photometric systems
The atmospheres of cool stars are temporally and spatially inhomogeneous due to the effects of convection. The influence of this inhomogeneity, referred to as granulation, on... -
4 globular clusters RGB and AGB stars
Spectroscopic studies have demonstrated that nearly all Galactic globular clusters (GCs) harbour multiple stellar populations with different chemical compositions. Moreover,... -
Metal enriched X-ray bursting neutron star atmos.
Low-mass X-ray binaries hosting neutron stars (NS) exhibit thermonuclear (type-I) X-ray bursts, which are powered by unstable nuclear burning of helium and/or hydrogen into... -
Center-to-limb polarization of FGK stars
Scattering and absorption processes in stellar atmosphere act the center-to-limb variations of the intensity (CLVI) and the linear polarization (CLVP) of stellar radiation....
