ar X iv : a st ro - p h / 06 10 10 7 v 1 4 O ct 2 00 6 Simulations of the interaction 1 of cold gas with radio jets

ar X iv : a st ro - p h / 06 10 95 0 v 1 3 1 O ct 2 00 6 Formation of cold molecular filaments in cooling flow clusters

New CO observations at the center of cooling flow in Perseus cluster [4] show a clear correlation of the molecular gas with the previously detected H-α filaments [1]. In this poster, we present high resolution multi-phase simulations of the Perseus Cluster, taking into account the AGN feedback in form of hot buoyant bubbles. These simulations show that significant amount of gas can cool far fro...

ar X iv : a st ro - p h / 04 10 29 7 v 1 1 2 O ct 2 00 4 Multiwavelength evidence of the physical processes in radio jets

Over the last few years, high-quality X-ray imaging and spectroscopic data from Chandra and XMM-Newton have added greatly to the understanding of the physics of radio jets. Here we describe the current state of knowledge with an emphasis on the underlying physics used to interpret multiwavelength data in terms of physical parameters.

ar X iv : a st ro - p h / 06 10 08 7 v 1 3 O ct 2 00 6 Jets and Disk - Winds from Pulsar Magnetospheres

We discuss axisymmetric force-free pulsar magnetospheres with magnetically collimated jets and a disk-wind obtained by numerical solution of the pulsar equation. This solution represents an alternative to the quasi-spherical wind solutions where a major part of the current flow is in a current sheet which is unstable to magnetic field annihilation.

ar X iv : a st ro - p h / 06 10 24 6 v 1 9 O ct 2 00 6 Special Features of Galactic Dynamics

ar X iv : a st ro - p h / 06 10 44 9 v 1 1 6 O ct 2 00 6 A Multicoloured View of 2 S 0114 + 650

We report the results of radio and X-ray observations of the high mass X-ray binary 2S 0114+650, made with the Giant Meterwave Radio Telescope and the Rossi X-ray Timing Explorer respectively. No emission was detected at radio wavelengths. The neutral hydrogen column density was found to vary over the orbital period, while no variability over the the super-orbital period was observed. We discus...