Structure of neutron stars in massive scalar-tensor gravity. (arXiv:2007.14429v3 [gr-qc] UPDATED)
<a href="http://arxiv.org/find/gr-qc/1/au:+Rosca_Mead_R/0/1/0/all/0/1">Roxana Rosca-Mead</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Moore_C/0/1/0/all/0/1">Christopher J. Moore</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Sperhake_U/0/1/0/all/0/1">Ulrich Sperhake</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Agathos_M/0/1/0/all/0/1">Michalis Agathos</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Gerosa_D/0/1/0/all/0/1">Davide Gerosa</a>
We compute families of spherically symmetric neutron-star models in
two-derivative scalar-tensor theories of gravity with a massive scalar field.
The numerical approach we present allows us to compute the resulting spacetimes
out to infinite radius using a relaxation algorithm on a compactified grid. We
discuss the structure of the weakly and strongly scalarized branches of
neutron-star models thus obtained and their dependence on the linear and
quadratic coupling parameters $alpha_0$, $beta_0$ between the scalar and
tensor sectors of the theory, as well as the scalar mass $mu$. For highly
negative values of $beta_0$, we encounter configurations resembling a
“gravitational atom”, consisting of a highly compact baryon star surrounded by
a scalar cloud. A stability analysis based on binding-energ calculations
suggests that these configurations are unstable and we expect them to migrate
to models with radially decreasing baryon density {it and} scalar field
strength.
We compute families of spherically symmetric neutron-star models in
two-derivative scalar-tensor theories of gravity with a massive scalar field.
The numerical approach we present allows us to compute the resulting spacetimes
out to infinite radius using a relaxation algorithm on a compactified grid. We
discuss the structure of the weakly and strongly scalarized branches of
neutron-star models thus obtained and their dependence on the linear and
quadratic coupling parameters $alpha_0$, $beta_0$ between the scalar and
tensor sectors of the theory, as well as the scalar mass $mu$. For highly
negative values of $beta_0$, we encounter configurations resembling a
“gravitational atom”, consisting of a highly compact baryon star surrounded by
a scalar cloud. A stability analysis based on binding-energ calculations
suggests that these configurations are unstable and we expect them to migrate
to models with radially decreasing baryon density {it and} scalar field
strength.
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