2008/06/30 by Noam Soker
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1086/591962
Accepted by ApJ Letters
arxiv created 2008/07/17 · openalex publication_date 2008/08/11 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/04
I propose an explanation for the finding that star formation and visible filaments strong in Hα emission in cooling flow clusters occur only if the minimum specific entropy and the radiative cooling time of the intracluster medium (ICM) are below a specific threshold. The explanation is based on the cold feedback mechanism. In this mechanism, the mass accreted by the central black hole originates in nonlinear overdense blobs of gas residing in an extended region of the cooling flow region. I use the criterion that the feedback cycle period must be longer than the radiative cooling time of dense blobs, for large quantities of gas to cool to low temperatures. The falling time of the dense blobs is parameterized by the ratio of the infall velocity to the sound speed. Another parameter is the ratio of the blobs' density to that of the surrounding ICM. By taking the values of the parameters as in previous papers on the cold feedback model, I derive an expression that gives the right value of the entropy threshold. Future studies will have to examine in more detail the role these parameters play, and will have to show that the observed sharp change in the behavior of clusters across the entropy, or radiative cooling time, threshold can be reproduced by the model.