Context: Since the discovery in 1997 of stellar oscillations in some B-type hot subdwarfs (sdBs), much effort is being made both observationally and theoretically to characterize this new group of pulsating objects. Aims: To increase the number of members of such pulsators and to perform a theoretical analysis of new pulsating stars. Methods: The

We provide in Table 4 basic (HIP and HD numbers, V magnitude and parallax) and kinematic (radial velocities and heliocentric space velocity) data for our sample stars. The kinematic probabilities of being a thin-disk, thick-disk, and halo member are also given. Table 5 contains the line data used in our abundance computations as well as the

The resonant peaks of solar p modes show small amounts of asymmetry in frequency. Here, we use five independent sets of contemporaneous data, collected over a ~=8 yr period, to investigate whether peak asymmetry in low angular degree p modes changes over the solar activity cycle. Three of the data sets are from instruments on board the ESA/NASA

We present first results from a deep (J = 18.7), wide-field (6.5deg2) infrared (ZY JHK) survey in the Upper Sco association conducted within the science verification phase of the United Kingdom Infrared Telescope Infrared Deep Sky Survey Galactic Cluster Survey (GCS). Cluster members define a sequence well separated from field stars in the (Z - J

This submission has been withdrawn by arXiv administrators because it is a duplicate of nucl-th/0610004.

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