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Astrophysical Bulletin

, Volume 70, Issue 4, pp 474–493 | Cite as

Hydrodynamic model of a self-gravitating optically thick gas and dust cloud

  • E. V. Zhukova
  • A. M. Zankovich
  • I. G. Kovalenko
  • K. M. Firsov
Article

Abstract

We propose an original mechanism of sustained turbulence generation in gas and dust clouds, the essence of which is the consistent provision of conditions for the emergence and maintenance of convective instability in the cloud. We considered a quasi-stationary one-dimensional model of a selfgravitating flat cloud with stellar radiation sources in its center. The material of the cloud is considered a two-component two-speed continuous medium, the first component of which, gas, is transparent for stellar radiation and is supposed to rest being in hydrostatic equilibrium, and the second one, dust, is optically dense and is swept out by the pressure of stellar radiation to the periphery of the cloud. The dust is specified as a set of spherical grains of a similar size (we made calculations for dust particles with radii of 0.05, 0.1, and 0.15 μm). The processes of scattering and absorption of UV radiation by dust particles followed by IR reradiation, with respect to which the medium is considered to be transparent, are taken into account. Dust-driven stellar wind sweeps gas outwards from the center of the cloud, forming a cocoon-like structure in the gas and dust. For the radiation flux corresponding to a concentration of one star with a luminosity of about 5 ×104 L per square parsec on the plane of sources, sizes of the gas cocoon are equal to 0.2–0.4 pc, and for the dust one they vary from tenths of a parsec to six parsecs. Gas and dust in the center of the cavity are heated to temperatures of about 50–60 K in the model with graphite particles and up to 40 K in the model with silicate dust, while the background equilibrium temperature outside the cavity is set equal to 10 K. The characteristic dust expansion velocity is about 1–7 kms−1. Three structural elements define the hierarchy of scales in the dust cocoon. The sizes of the central rarefied cavity, the dense shell surrounding the cavity, and the thin layer inside the shell in which dust is settling provide the proportions 1 : {1–30} : {10−7–10−6}. The density differentials in the dust cocoon (cavity–shell) are much steeper than in the gas one, dust forms multiple flows in the shell so that the dust caustics in the turning points and in the accumulation layer have infinite dust concentration. We give arguments in favor of unstable character of the inverse gas density distribution in the settled dust flow that can power turbulence constantly sustained in the cloud. If this hypothesis is true, the proposed mechanism can explain turbulence in gas and dust clouds on a scale of parsecs and subparsecs.

Keywords

interstellar medium: clouds convection instabilities turbulence 

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Copyright information

© Pleiades Publishing, Ltd. 2015

Authors and Affiliations

  • E. V. Zhukova
    • 1
  • A. M. Zankovich
    • 1
  • I. G. Kovalenko
    • 1
  • K. M. Firsov
    • 1
  1. 1.Institute of Physics and TelecommunicationVolgograd State UniversityVolgogradRussia

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