1994A&A...287...55J

We present a 2D computer code for stochastic self-propagating star formation (SSPSF) in differentially rotating galaxies. The isotropic probability distribution, used in previous models of Seiden, Gerola and Schulman (Seiden & Schulman, 1990, and references therein), is replaced by an anisotropic one. The motivation is provided by models of expanding large-scale supernova remnants (SNR) in disks with shear (Palous et al. 1990): the distortion of the SNR leads to uneven density distribution along its periphery and, consequently, to uneven distribution of new star forming sites. To model anisotropic SSPSF we proceed in two steps: first, we eliminate artificial anisotropies inherent to the technique used by Seiden, Gerola and Schulman and, second, we define the probability ellipse on each star forming site. The anisotropy is characterized by its axes ratio and inclination with respect to the galactic center. We show that anisotropic SSPSF is able to produce highly organized spiral structures. Depending on the character of the probability ellipse, we can obtain continuous spiral arms of different length, thickness and pitch angle. The relation of the probability ellipse to rotation curves, ISM density and metallicity is discussed as well as its variation along the Hubble sequence and van den Bergh's luminosity classification of galaxies. To demonstrate applications, we compare our results with two different classes of galaxies: M 101-type grand-design spirals with open and robust arms and NGC 2841-type flocculent galaxies with thin and tightly wound arms.