Abstract
The gravitational decoupling is applied to studying minimal geometric deformed (MGD) compact superfluid stars, in covariant logarithmic scalar gravity on fluid branes. The brane finite tension is shown to provide more realistic values for the asymptotic value of the mass function of MGD superfluid stars, besides constraining the range of the self-interacting scalar field, minimally coupled to gravity. Several other physical features of MGD superfluid stars, regulated by the finite brane tension and a decoupling parameter, are derived and discussed, with important corrections to the general-relativistic limit that corroborate to current observational data.
Highlights
Brane is rigid, or equivalently, when the brane tension attains an infinite value [6,7]
Some results regarding superfluid stars in the general relativity (GR) limit [91] are qualitatively similar to the ones obtained in this work, scrutinizing minimal geometric deformed (MGD) superfluid stars
Most of our results show that the finite fluid brane tension and the MGD parameter bring new results that comply with a more realistic and physically feasible model, whose eventual gravitationalwave observations can be more reliable in a finite brane tension setup
Summary
MGD-decoupling methods represent a realistic algorithm to derive and scrutinize compact stars. Since inflationary universe models driven by scalar fields with logarithmic potential shed new light on cosmology [75,76,77], it is natural to argue how the setup of the Klein–Gordon equation with logarithmic potential, coupled to GR, can be used to study MGD-decoupled superfluid stars. It is natural to ascertain, in a realistic model that complies with recent observational data, how the finite tension of the brane can drive new gravitational MGDdecoupled solutions of the Einstein–Klein–Gordon coupled system with logarithmic scalar potential, that encodes compact strongly-interacting and extremely dense superfluids. The finite brane tension setup, complying with current observational data, is shown to improve the Schwarzschild GR analysis, paving new ways to describe realistic models for superfluid stars.
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