Chromospheric model calculations of the Hα line for selected red giant branch and asymptotic giant branch (AGB) stars in the globular clusters M13, M15, and M92 are constructed to derive mass loss rates (MLRs). The model spectra are compared to the observations obtained with the Hectochelle on the MMT telescope. These stars show strong Hα emissions

We have derived masses and radii for both components in five short-period single-lined eclipsing binary stars discovered by the TrES wide-angle photometric survey for transiting planets. All these systems consist of a visible F-star primary and an unseen M-star secondary (M A >= 0.8 M sun, M B

We propose to complete the observations (see re-submission details later) for a project to produce definitive Color-Magnitude Diagrams (CMDs) for a carefully chosen sample of galactic globular clusters, using the Mosaic Camera on the Blanco telescope. The large field size will enable us to efficiently cover to beyond the published tidal radius for

Context: The mechanisms giving rise to diffuse radio emission in galaxy clusters, and in particular their connection with cluster mergers, are still debated. Aims: We aim to obtain new insights into the internal dynamics of the cluster Abell 1240, which appears to contain two roughly symmetric radio relics, separated by ~2 h_70-1 Mpc. Methods: Our

IAC-pop is a code designed to solve the star formation history (SFH) of a complex stellar population system, like a galaxy, from the analysis of the color-magnitude diagram (CMD). It uses a genetic algorithm to minimize a χ2 merit function comparing the star distributions in the observed CMD and the CMD of a synthetic stellar population. A

The tables represent the results of the frequency analysis of various models: under assumption of stable, long-lasting and independent frequencies with constant amplitudes and phases, we arrive at the list in table1.dat. When assuming dependency in the form of combination frequencies, we arrive at the list presented in table2.dat. When allowing for