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3D Hydrodynamical Simulations of a Galactic Fountain

Published online by Cambridge University Press:  12 April 2016

M.A. de Avillez ,
D.L. Berry  and
F.D. Kahn
M.A. de Avillez
Affiliation:
Departamento de Física, Universidade de Évora, R. Romão Ramalho 59, 7000 Évora, Portugal
D.L. Berry
Affiliation:
Departamento de Física, Universidade de Évora, R. Romão Ramalho 59, 7000 Évora, Portugal
F.D. Kahn
Affiliation:
Department of Physics and Astronomy, University of Manchester, Schuster Laboratory, Manchester M13 9PL, England

Abstract

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Galactic fountains are thought to be responsible for the formation of the observed intermediate and high velocity clouds in the Galactic halo. Threedimensional simulations have been carried out to determine the evolution of the disk gas as it enters the fountain, cools and returns to the Galactic disk. The descending cold gas, headed by a shock, sweeps up the ascending flow, triggering the formation of an unstable layer where Rayleigh-Taylor instabilities grow, which may provoke the formation of the observed clouds.

Type
Part VIII High-Velocity Clouds, Galactic Halo Models, Observations of the LMC
Information
International Astronomical Union Colloquium , Volume 166: The Local Bubble and Beyond , 1997 , pp. 495 - 498
Copyright
Copyright © Springer-Verlag 1998

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