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Self-gravity driven instabilities at accelerated interfaces
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DOI：10.1196/annals.1350.021.png)
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Abstract
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Nonlinear hydrodynamic flows are ubiquitous in the interstellar medium (ISM). Such flows play an important role in shaping atomic and molecular clouds and determining the initial conditions for star formation. One mechanism by which nonlinear flows arise is the onset and growth of interfacial instabilities. Any interface of discontinuous density is subject to a host of instabilities, including Rayleigh-Taylor, Kelvin-Helmholtz, and Richtmyer-Meshkov. As part of an ongoing study of structure formation in the ISM, Hunter, Whitaker, and Lovelace discovered an additional density interface instability. This instability is driven by self-gravity and termed the self-gravity interfacial instability (SGI). The SGI causes any displacement of the interface to grow on roughly a free-fall time scale, even when the perturbation wavelength is much less than the Jeans length. Numerical simulations have confirmed the expectations of linear theory, including the near scale invariance of the growth rate. Here, we build upon previous work by considering an initial condition in which the acceleration due to self-gravity is non-zero at the interface.
Keywords:
hydrodynamics
instabilities
ISM
evolution
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