Instruct: Identify the main and secondary category of Arxiv papers based on the titles and abstracts
Query: Spontaneous scalarisation of charged black holes: coupling dependence
  and dynamical features   Spontaneous scalarisation of electrically charged, asymptotically flat
Reissner-Nordstr\"om black holes (BHs) has been recently demonstrated to occur
in Einstein-Maxwell-Scalar (EMS) models. EMS BH scalarisation presents a
technical simplification over the BH scalarisation that has been conjectured to
occur in extended Scalar-Tensor Gauss-Bonnet (eSTGB) models. It is then natural
to ask: 1) how universal are the conclusions extracted from the EMS model? And
2) how much do these conclusions depend on the choice of the non-minimal
coupling function? Here we perform a comparative analysis of different forms
for the coupling function including: exponential, hyperbolic, power-law and a
rational function (fraction) couplings. In all of them we obtain and study the
domain of existence of fundamental, spherically symmetric, scalarised BHs and
compute, in particular, their entropy. The latter shows that scalarised EMS BHs
are always entropically preferred over the RN BHs with the same total charge to
mass ratio $q$. This contrasts with the case of eSTGB, where for the same
power-law coupling the spherical, fundamental scalarised BHs are not
entropically preferred over Schwarzschild. Also, while the scalarised solutions
in the EMS model for the exponential, hyperbolic and power-law coupling are
very similar, the rational function coupling leads to a transition in the
domain of existence. Furthermore, fully non-linear dynamical evolutions of
unstable RN BHs with different values of $q$ are presented. These show: 1) for
sufficiently small $q$, scalarised solutions with (approximately) the same $q$
form dynamically; 2) for large $q$, spontaneous scalarisation visibly decreases
$q$; thus evolutions are non-conservative; 3) despite the existence of
non-spherical, static scalarised solutions, the evolution of unstable RN BHs
under non-spherical perturbations leads to a spherical scalarised BH.

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The categories of this paper are: cmp-lg
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The categories of this paper are: cond-mat
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The categories of this paper are: mtrl-th
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The categories of this paper are: eess
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The categories of this paper are: math-ph
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The categories of this paper are: comp-gas
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The categories of this paper are: ao-sci
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The categories of this paper are: q-alg
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The categories of this paper are: bayes-an
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The categories of this paper are: chao-dyn
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The categories of this paper are: math
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The categories of this paper are: alg-geom
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The categories of this paper are: nlin
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The categories of this paper are: astro-ph
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The categories of this paper are: supr-con
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The categories of this paper are: q-fin