When binary systems with a chemically peculiar (CP) star are compared with normal-star binary systems, they present: a lower incidence, a deficiency of short periods, rather eccentric orbits, and companions of low mass. Unfortunately these results are based on a relatively small (∼ 50) number of CP-star binary systems with known orbital parameters and a similar analysis has not yet been carried...

Gravitational waves emitted from the coalescence of neutron star binaries open a new window to probe matter and fundamental physics in unexplored, extreme regimes. To extract information about supranuclear inside stars properties compact binary systems, robust theoretical prescriptions are required. We give an overview general features dynamics gravitational wave signal during coalescence. brie...

Young star clusters are often born with such high stellar densities that stellar collisions play an important role in their further evolution. In such environments the same star may participate in several tens to hundreds of collisions ultimately leading to the collapse of the star to a black hole of intermediate mass. At later time the black hole may acquire a companion star by tidal capture o...

Pulsars in close, eccentric binary systems are usually assumed to have another neutron star as a companion. These double neutron star binaries have proven to be the best laboratories for experimental General Relativity and are the most secure candidates for gravitational wave interferometers. We present deep B, V , and R images of the field containing the eccentric binary pulsar system PSR B230...

Pulsars in close, eccentric binary systems are usually assumed to have another neutron star as a companion. These double neutron star binaries have proven to be the best laboratories for experimental General Relativity and are the most secure candidates for gravitational wave interferometers. We present deep B, V , and R images of the field containing the eccentric binary pulsar system PSR B230...

We present spatially-resolved X-ray observations of the binary T Tauri star system V710 Tau. Using Chandra’s Advanced CCD Imaging Spectrometer (ACIS), we imaged this 3.2 separation binary system, consisting of a classical T Tauri star, V710 Tau N, and a weak-lined T Tauri star, V710 Tau S. The Chandra ACIS-S3 images — obtained in two 9 ks exposures separated by about three months (2004 December...

In binary radio pulsars with a main-sequence star companion, the spin-induced quadrupole moment of the companion gives rise to a precession of the binary orbit. As a first approximation one can model the secular evolution caused by this classical spin-orbit coupling by linear-in-time changes of the longitude of periastron and the projected semi-major axis of the pulsar orbit. This simple repres...

We examine the dynamical destruction of binary systems in star clusters of different densities. We find that at high densities (10 − 10 M⊙ pc ) almost all binaries with separations > 10 AU are destroyed after a few crossing times. At low densities (O(102)M⊙ pc ) many binaries with separations > 10 AU are destroyed, and no binaries with separations > 10 AU survive after a few crossing times. The...

The atmosphere of the extremely high-velocity (530 − 920 km s) early B-type star HD271791 is enriched in α-process elements, which suggests that this star is a former secondary component of a massive tight binary system and that its surface was polluted by the nucleosynthetic products after the primary star exploded in a supernova. It was proposed that the (asymmetric) supernova explosion unbin...

Pulsars in close, eccentric binary systems are usually assumed to have another neutron star as a companion. These double neutron star binaries have proven to be the best laboratories for experimental General Relativity and are the most secure candidates for gravitational wave interferometers. We present deep B, V , and R images of the field containing the eccentric binary pulsar system PSR B230...