Filament Evolution Process

The Herschel Gould Belt Survey showed that stars form in dense filaments in nearby molecular clouds. Recent studies suggest that massive filaments are bound by the slow-shocks caused by inflows onto the filaments. The slow-shocks are known to be unstable to corrugation deformation of the shock front. Corrugation instability could convert the inflow’s ram pressure into turbulent pressure that influences the width of the filament, which, according to theory, determines the self-gravitational fragmentation scale and core mass. In spite of its importance, the effect of slow-shock instability on star-forming filaments has not been investigated. In addition, the linear dispersion relation obtained from ideal MHD analysis shows that the most unstable wavelength of shock corrugation is infinitesimally small. In the scale of dense filaments, the effect of ambipolar diffusion can suppress the instability at small scales. In this chapter, we show the influence of ambipolar diffusion on the instability of the slow-shock. We perform two-dimensional MHD simulations to examine the linear growth of the slow-shock instability, considering the effect of ambipolar diffusion. The results demonstrate that the most unstable scale of slow-shock instability is approximately 5 times the length scale of ambipolar diffusion \(l_\text {AD}\) calculated using post-shock variables, where \(l_\text {AD}\) corresponds to the scale where the magnetic Reynolds number for ambipolar diffusivity is unity.