I will present a variety of extragalactic science projects from two of the leading submillimeter telescopes, with a special focus on continuum studies. First, I will discuss a recent 350 micron follow-up survey of submillimeter-selected galaxies (SMGs) from the CSO. The new data give the first firm far-infrared characterization of this elusive population of distant galaxies, confirming the radio to far-infrared correlation out to high-z. In the second part, I will give a brief summary of the various extragalactic science efforts we are presently pursuing at the APEX telescope in Chile. I will focus on bolometer studies of deep fields and nearby galaxies, but will also mention the ongoing Sunyayev-Zel'dovich cluster survey, and molecular (CO) line studies.

Attilio Ferrari - Accretion disks and astrophysical jets are used to model many active astrophysical ob jects, viz., young stars, relativistic stars, and active galactic nuclei. However, extant proposals on how these structures may transfer angular momentum and energy from disks to jets through viscous or magnetic torques do not yet provide a full understanding of the physical mechanisms involved. Global stationary solutions do not permit understanding the stability of these structures; and global
numerical simulations that include both the disk and jet physics are often limited to relatively short time scales and small (and possibly astrophysically unlikely) ranges of viscosity and resistivity parameters that are instead crucial to define the coupling of the inflow/outflow dynamics. Along these lines we discuss existing self-consistent time-dependent simulations of supersonic jets launched from magnetized accretion disks, using high resolution numerical techniques. I shall concentrate on the effects of the disk physical parameters, and discuss under which conditions steady state solutions of the type proposed in the self-similar models of Blandford & Payne can be reached and maintained in a self-consistent nonlinear stage. In addition I shall discuss how the interaction between an accretion disk and a magnetosphere of a star can modify the outflow solutions.

We consider Alfvenic MHD turbulence which is imbalanced, i.e. when waves propagating in one direction along magnetic field have higher amplitudes than counter-propagating waves. Contrary to the straightforward interpretation of the Goldreich-Sridhar critical balance, the anisotropy of the strong component is smaller than the anisotropy of the weak component. I will explain why this actually makes sense and how you replace critical balance to make a consistent theory. I will also show the results of direct numerical simulations of imbalanced turbulence.