Abstract
Let us summarize what we have learned about compact stars and dense matter, having in mind the two questions we have formulated in the preface. In addition, let us also list a few things which would in principle have fitted into these lectures topic-wise. We haven’t discussed them in the main part because either I found them not suitable for a concise, and yet pedagogical, introduction or because they are simply beyond the scope of these lectures, such as some of the theoretical approaches to dense matter listed at the end of Sect. 6.2. And, well, some selection has to be made, so for some of the following points there is no good reason why they appear here and not in the main part. The volume of the main part is chosen such that it should conveniently fit into a one-semester course, maybe dropping one or two of the more specialized subsections. In Sect. 6.2 I will give some selected references where interested readers can find more information about the questions we haven’t addressed in the main part.
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Notes
- 1.
Oscillatory modes of compact stars are classified according to their restoring force. In the case of r-modes, this is the Coriolis force.
- 2.
In the case of a superfluid, there are in fact several bulk viscosities.
- 3.
It is instructive to view this phenomenon in analogy to a type-II superconductor. There, a magnetic field (if sufficiently large but not too large) penetrates the superconductor through flux tubes. It partially destroys superconductivity, i.e., in the center of the flux tubes the order parameter is zero. Hence the analogy is superfluid – superconductor; angular momentum – magnetic field; vortices – flux tubes.
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Schmitt, A. (2010). Discussion. In: Dense Matter in Compact Stars. Lecture Notes in Physics, vol 811. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-12866-0_6
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