Qualitative analysis of dynamic equations on time scales

In this article, we establish the Picard-Lindelof theorem and approximating results for dynamic equations on time scale. We present a simple proof for the existence and uniqueness of the solution. The proof is produced by using convergence and Weierstrass M-test. Furthermore, we show that the Lispchitz condition is not necessary for uniqueness. The existence of epsilon-approximate solution is established under suitable assumptions. Moreover, we study the approximate solution of the dynamic equation with delay by studying the solution of the corresponding dynamic equation with piecewise constant argument. We show that the exponential stability is preserved in such approximations.Comment: 13 page

Thermally induced flow instabilities in two-phase mixtures in thermal equilibrium

Ph.D.Novak Zube

On the Formation of Planetesimals via Secular Gravitational Instabilities with Turbulent Stirring

We study the gravitational instability (GI) of small solids in a gas disk as a mechanism to form planetesimals. Dissipation from gas drag introduces secular GI, which proceeds even when standard GI criteria for a critical density or Toomre's $Q$ predict stability. We include the stabilizing effects of turbulent diffusion, which suppresses small scale GI. The radially wide rings that do collapse contain up to $\sim 0.1$ Earth masses of solids. Subsequent fragmentation of the ring (not modeled here) would produce a clan of chemically homogenous planetesimals. Particle radial drift time scales (and, to a lesser extent, disk lifetimes and sizes) restrict the viability of secular GI to disks with weak turbulent diffusion, characterized by $\alpha \lesssim 10^{-4}$. Thus midplane dead zones are a preferred environment. Large solids with radii $\gtrsim 10$ cm collapse most rapidly because they partially decouple from the gas disk. Smaller solids, even below $\sim$ mm-sizes could collapse if particle-driven turbulence is weakened by either localized pressure maxima or super-Solar metallicity. Comparison with simulations that include particle clumping by the streaming instability shows that our linear model underpredicts rapid, small scale gravitational collapse. Thus the inclusion of more detailed gas dynamics promotes the formation of planetesimals. We discuss relevant constraints from Solar System and accretion disk observations.Comment: Accepted for publication in the Astrophysical Journal; 20 pages, 10 figure