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Session 20 - Molecular Clouds, Dense Cores, and Protostars.
Display session, Monday, January 15
North Banquet Hall, Convention Center
We study the linear evolution of small perturbations in self-gravitating, magnetized fluid systems in two spatial dimensions. The analysis is general, but the application of primary interest is molecular clouds. We consider a class of equations of state which heuristically take into account the presence of turbulence; in particular, we consider equations of state which are softer than isothermal. We take the unperturbed cloud configuration to be in magnetohydrostatic equilibrium with the magnetic field parallel to the direction of translational symmetry. We find wave solutions which propagate along the cylinder or slab supported by kinetic and magnetic pressure. We determine the form of the perturbations and the dispersion relations for a wide range of wavelengths. Finally, we discuss the implications of our results for star formation and molecular clouds.
