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Grids of stellar models. II.
Continuing the effort to provide a homogeneous base of extensive and accurate grids of stellar models covering a wide range of metallicities we present a new grid of stellar... -
Low-mass stars evolutionary tracks & isochrones
These files contain a large database of stellar models that are suitable to modelling star clusters and galaxies by means of population synthesis. They are based on a large grid... -
Illuminated atmospheres limb-darkening coeff. 1.
In Table 1 we present the bolometric and monochromatic limb-darkening coefficients for 196 different combinations of the parameters: T_eff (illuminated model's effective... -
Grids of stellar models. VIII.
We present stellar evolutionary models covering the mass range from 0.4 to 1M_{sun} calculated for metallicities Z=0.020 and 0.001 with the MHD equation of state (Hummer &... -
Calcium triplet synthesis
We present theoretical equivalent widths for the sum of the two strongest lines of the calcium triplet, CaT index, in the near-IR ({lambda}{lambda} 8542, 8662{AA}), using... -
Yields of intermediate mass stars
We present theoretical yields of H, ^4^He, ^12^C, ^13^C, ^14^N, and ^16^O for stars with initial masses between 0.8 and 8M_{sun}_ and initial metallicities Z=0.001, 0.004,... -
K and evolutionary corrections
K and evolutionary corrections are given for the E, Sa and Sc Hubble types for the following filters up to the redshift z=3: Johnson-Bessell & Brett photometric system: U,... -
Stellar models VI.
New grids of models covering the evolution of low mass stars (0.8 to 1.7M{sun}) with metallicities Z=0.020 and 0.001 from the zero age main sequence up to the end of the early... -
Evolutionary sequences with MC metallicities
Tables of evolutionary sequences for massive stars with metallicities Z=0.002 and Z=0.01 in the mass range 9 to 40 M_{sun}_ and mass ratios 0.9 and 0.6 are presented. The... -
Convective-core overshooting of massive stars
Understanding and predicting their final fate is increasingly important, e.g., in the context of gravitational-wave astronomy. The interior mixing of stars in general and... -
Very massive star models (VMS)
In addition to being spectacular objects, very massive stars (VMSs) are suspected to have a tremendous impact on their environment and on cosmic evolution in general. The... -
Solar evolutionary and structure models
In protoplanetary disks, the growth and inward drift of dust lead to the generation of a temporal "pebble wave" of increased metallicity. This phase must be followed by a phase... -
Effects of IMG on Galactic chemical enrichment
We have been seeing mounting evidence that the stellar initial mass function (IMF) might extend far beyond the canonical Mi~100M_{sun} limit, but the impact of such a hypothesis... -
Yields for Z=1e-5 intermediate-mass stars
Observed abundances of extremely metal-poor (EMP) stars in the Halo hold clues for the understanding of the ancient universe. Interpreting these clues requires theoretical... -
Spectra of 14 Magellanic Cloud planetary nebulae
We obtained new spectra of fourteen Magellanic Cloud planetary nebulae with the South African Large Telescope to determine heating rates of their central stars and to verify... -
HD 219134 light and RV curves and code
By analysing the transit light-curve of a planet-hosting star or the induced radial velocity oscillations, many useful information on the planet may be retrieved. However,... -
Stellar models with rotation. 1.7<M<120, Z=0.0004
The effects of rotation on stellar evolution are particularly important at low metallicity, when mass loss by stellar winds diminishes and the surface enrichment due to... -
Models for massive stars in the SMC
The evolution of massive stars is strongly influenced by internal mixing processes such as semiconvection, convective core overshooting, and rotationally induced mixing. None of... -
Non standard s-process in massive rotating stars
Recent studies show that rotation significantly affects the s-process in massive stars. We provide tables of yields for non-rotating and rotating massive stars between 10 and... -
Pre-main sequence stars evolutionary models. II
We want to investigate how planet formation is imprinted on stellar surface composition using up-to-date stellar evolution models. We simulate the evolution of pre-main-sequence...
