Abstract
Gravitational decoupled compact polytropic hybrid stars are here addressed in generalized Horndeski scalar-tensor gravity. Additional physical properties of hybrid stars are scrutinized and discussed in the gravitational decoupling setup. The asymptotic value of the mass function, the compactness, and the effective radius of gravitational decoupled hybrid stars are studied for both cases of a bosonic and a fermionic prevalent core. These quantities are presented and discussed as functions of Horndeski parameters, the decoupling parameter, the adiabatic index, and the polytropic constant. Important corrections to general relativity and generalized Horndeski scalar-tensor gravity, induced by the gravitational decoupling, comply with available observational data. Particular cases involving white dwarfs, boson stellar configurations, neutron stars, and Einstein–Klein–Gordon solutions, formulated in the gravitational decoupling context, are also scrutinized.
Highlights
The direct observation of gravitational waves emitted from mergers consisting of neutron stellar configurations has nowadays comprised one of the most important stages of investigation in physics
Anisotropic stellar configurations are naturally addressed by several gravitational decoupling procedures, which is a sharp apparatus that can be used in a wide range to derive new analytical solutions to Einstein’s coupled system of field equations [3–5]
Gravitational decoupled hybrid stars were scrutinized and described by anisotropic polytropic stellar configurations, that are self-gravitating bound regular stellar structures constituted by scalar bosons and fermionic matter
Summary
The direct observation of gravitational waves emitted from mergers consisting of neutron stellar configurations has nowadays comprised one of the most important stages of investigation in physics. When gravity is investigated in the strong regime, general relativity and generalizations can be experimentally probed by current observations gleaned mainly at LIGO, eLISA, and the Chandra X-ray Observatory Such experiments can precisely approach extended models that describe gravity when the remnant coalescent binary black hole system does emit gravitational waves pulses while entering into its final state. Employing the gravitational decoupling of kernel solutions of Einstein’s field equations, gravitational field sources can be split into a solution in general relativity and an associate source, which encodes any additional interaction in the theory, including gauge and tidal charges, hairy physical fields, and extended models of gravity This approach has been generating new solutions that describe a comprehensive list of stellar configurations and include particular cases of coalescing binary neutron stars and black holes [22–27], whose acoustic analogs were scrutinized [28,29].
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