We report the discovery of a new X-ray source detected in a 5ks observation starting on 2007-02-14.08 UT as part of our ongoing Chandra/HST M31 transient program. The source was detected at coordinates RA(J2000) 00:44:12.4, Dec(J2000) 41:25:48.2, at the edge of the ACIS-S field of view, which results in larger than usual position errors of 2.2" and

Mid-infrared images between 8.7 and 18.7um of W75N were taken during three observing runs on September 2000, November 2001 and September 2003 with the mid-infrared camera CID on the 2.1 m telescope of the Observatorio Astronomico Nacional at San Pedro Martir, Baja California, Mexico. The images at 3.6, 4.5, 5.8 and 8.0um of W75N presented here are

Aims:We combine the magnetohydrodynamic (MHD) theory of resonantly damped quasi-mode kink oscillations with observational estimates of the period and damping of transverse coronal loop oscillations to extract information on physical parameters in oscillating loops. Methods: A numerical study of the quasi-mode period and damping, in one-dimensional

A general analytical framework for the determination of the mean field states at arbitrary rational filling factors for the 2DEG in FQHE regime is given. Its use allows to obtain analytic expressions for the solutions at filling factors of the form $ u=1/q$ for arbitrary odd $q$. The analysis can be performed for two general classes of states

Aims: We selected a large sample of O-B stars that were considered as (candidate) slowly pulsating B, β Cep, and Maia stars after the analysis of their hipparcos data. We analysed our new seven passband geneva data collected for these stars during the first three years of scientific operations of the mercator telescope. We performed a frequency

Lithium and zirconium abundances (the latter taken as representative of s-process enrichment) are determined for a large sample of massive Galactic O-rich AGB stars, for which high-resolution optical spectroscopy has been obtained (R˜ 40 000{-}50 000). This was done by computing synthetic spectra based on classical hydrostatic model atmospheres for