Evolution of overdense regions in cluster cooling flows

Details Evolution of overdense regions in cluster cooling flows Evolution of overdense regions in cluster cooling flows

May 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.238...15l&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 238, May 1, 1989, p. 15-41. Research supported by the R

Astronomy and Astrophysics

Astronomy

32

Cooling, Density Distribution, Galactic Clusters, Galactic Evolution, Mass Transfer, Astronomical Models, Equations Of Motion, Flow Equations, Long Term Effects, Perturbation Theory

Scientific paper

The evolution of regions of finite overdensity in cooling flows is investigated by solving the equations of motion and energy, assuming the regions to be spherical and uniform, and by performing hydrodynamical calculations specifically designed to treat perturbations to a steady background flow. Results differ in detail from the linear analysis, but the basic behavior remains - overdense regions exhibit thermal-convective oscillations and do not cool out. It is concluded that a satisfactory explanation for the origin of optically emitting gas and the evidence from X-ray observations for mass deposition does not presently exist, and that a detailed understanding of the central parts of cooling flows is still lacking.

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