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Outer planetary systems
In order to better understand the range of dynamically long-lived giant planet systems, we present the results of a set of bottom-up numerical simulations designed to generate... -
Stellar Models from 0.8 to 120 Msolar
New grids of stellar evolutionary models covering the range of 0.8 to 120 solar masses have been computed for metallicites Z=0.020 and Z=0.001. The models use the new opacities... -
Eclipsing binaries light curves models
We present parameters used in the investigation of the light curves of eclipsing binaries together with other data needed for the interpretation of their stellar and dynamical... -
A standard stellar library. II.
A standard library of theoretical stellar spectra intended for multiple synthetic photometry applications including spectral evolutionary synthesis is presented. The grid... -
Grids of stellar models. VII.
We present a new grid of stellar models from 0.8 to 60M_{sun} at Z=0.10, with mass loss and moderate overshooting, from the zero age main sequence to either the helium flash... -
Models of circumstellar dust shells
Main properties of the steady state hydrodynamical models of circumstellar gas/dust shells around late type giants, computed for different stellar parameters (mass, luminosity,... -
A standard stellar library
The present library provides an extensive and homogeneous grid of low-resolution theoretical flux distributions for a large range of stellar parameters : Teff=50,000K to K,... -
Stellar models until He burning - II.
Three new grids of stellar evolutionary models with Z=0.01 are presented for the following values of initial hydrogen content X_i_=0.80, 0.73 and 0.63. The latest set of... -
Rotating neutron stars models. II.
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Grids of stellar models V.
Most outputs of massive star evolution critically depend on the mass loss rates. In order to broaden the comparison basis and to illustrate the effects of different mass loss... -
Grids of stellar models IV
The present grid of evolutionary sequences at metallicity Z=0.040, completes the set of grids computed for Z=0.020 and 0.001 by Schaller et al. (1992, Cat. J/A+AS/96/269),... -
Grids of stellar models III.
Stellar evolutionary models with mass loss and moderate overshooting at metallicity Z = 0.004 in the 0.80 to 120 M{sun} range are presented. They complete the set of grids... -
Convective turnover times of disk-locking stars
The impact of disk-locking on the stellar properties related to magnetic activity from the theoretical point of view is investigated. We use the ATON stellar evolution code to... -
Grid of stellar models
A common property of globular clusters (GCs) is to host multiple populations characterized by peculiar chemical abundances. Recent photometric studies suggest that the He... -
Effect on rotation for red giant ages
Galactic archaeology largely relies on precise ages of distant evolved stars in the Milky Way. Nowadays, asteroseismology can deliver ages for many red giants observed with... -
Mass transfer from post-main-sequence donor stars
The stability of mass transfer is critical in determining pathways towards various kinds of compact binaries, such as compact main-sequence white-dwarf binaries, and transients,... -
Yields Z=1e-6-1e-10 intermediate-mass stars
Stellar models and nucleosynthetic yields of primordial to extremely metal-poor (EMP) stars are crucial to interpret the surface abundances of the most metal-poor stars... -
Solar evolutionary and structure models
Solar evolutionary models are thus far unable to reproduce spectroscopic, helioseismic, and neutrino constraints consistently, resulting in the so-called solar modeling problem.... -
Evolutionary models for main-sequence phase
The identification of stellar-mass black-hole mergers with up to 80M_{sun} as powerful sources of gravitational wave radiation led to increased interest in the physics of the... -
Evolutionary sequences for ultra-massive CO-core
The existence of ultra-massive white dwarf stars, M_WD_>~1.05M_{sun}, has been reported in several studies. These white dwarfs are relevant for the role they play in type Ia...
