Models for the formation and evolution of galaxies readily predict physical properties such as the star formation rates, metal enrichment histories, and, increasingly, gas and dust content of synthetic galaxies. Such predictions are frequently compared to the spectral energy distributions of observed galaxies via the stellar population synthesis (SPS) technique. Substantial uncertainties in SPS...

Aims. We investigate the influence of high–energy stellar radiation at close–in orbits on atmospheric mass loss during stellar evolution of a G–type star. Methods. High–energy stellar luminosity varies over a wide range for G field stars. The temporal evolution of the distribution of stellar X–ray luminosity and its influence on the evolution of close–in exoplanets is investigated. X–ray lumino...

Young stars on their way to the ZAMS evolve in significantly different ways depending on their mass. While the theoretical and observational properties of lowand intermediate-mass stars are rather well understood and/or empirically tested, the situation for massive stars (> ∼ 10– 15 M⊙) is, to say the least, still elusive. On theoretical grounds, the PMS evolution of these objects should be ext...

Stellar evolution computations provide the foundation of several methods applied to study the evolutionary properties of stars and stellar populations, both Galactic and extragalactic. The accuracy of the results obtained with these techniques is linked to the accuracy of the stellar models, and in this context the correct treatment of the transport of chemical elements is crucial. Unfortunatel...

Many reviews have been written on pre-main-sequence binaries over the past 25 years, e.g., Reipurth (1988), Zinnecker (1989), Mathieu (1994), and Goodwin (2010), and particular mention should be made of IAU Symposium No. 200 (Zinnecker and Mathieu, 2001), which is still today a useful reference. Most recently, Duchêne and Kraus (2013) review the binarity for stars of all masses and ages. Stimul...

Observations have revealed that most stars are born in clusters. These systems, containing from tens to thousands of stars and typically significant mass in gas in the youngest systems, evolve due to a combination of stellar and star-gas interactions. Simulations of pure stellar systems are used to investigate possible initial configurations including ellipticity, substructure and mass segregat...

I present a discussion of fundamental stellar parameters and their observational determination in the context of interferometric measurements with current and future optical/infrared interferometric facilities. Stellar parameters and the importance of their determination for stellar physics are discussed. One of the primary uses of interferometry in the field of stellar physics is the measureme...

Any stellar system with a star formation history (SFH) more extended than a massive star’s lifetime will be composite in metallicity. Our method of chemically consistent evolutionary synthesis tries to account for the increasing initial metallicity of successive generations of stars. Using various sets of input physics for a range of metallicities 10 ≤ Z ≤ 0.05 we keep track of the ISM enrichme...