Abstract
In order to model the Fermi bubbles we apply the theory of the superbubble (SB). A thermal model and a self-gravitating model are reviewed. We introduce a third model based on the momentum conservation of a thin layer which propagates in a medium with an inverse square dependence for the density. A comparison have been made between the sections of the three models and the section of an observed map of the Fermi bubbles. An analytical law for the SB expansion as function of the time and polar angle is deduced. We derive a new analytical result for the image formation of the Fermi bubbles in an elliptical framework.
Highlights
The term super-shell was observationally defined by [1] as holes in the H I-column density distribution of our Galaxy
This section introduces a test for the reliability of the model, analyzes the observational details of the Fermi bubbles, reviews the results for the two models of reference and reports the results of the inverse square model
We have compared two existing models for the temporal evolution of the Fermi bubbles, a thermal model, see Section 3.1, and an autogravitating model, see Section 3.2, with a new model which conserves the momentum in presence of an inverse square law for the density of the ISM
Summary
The term super-shell was observationally defined by [1] as holes in the H I-column density distribution of our Galaxy. The dimensions of these objects span from 100 pc to 1700 pc and present elliptical shapes. These structures are commonly explained through introducing theoretical objects named bubbles or Superbubbles (SB); these are created by mechanical energy input from stars (see for example [2] [3]).
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