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A dark matter compact star in the framework of the pseudo‐complex general relativity
Author(s) -
Hadjimichef D.,
Machado M.V.T.,
Köpp F.,
Volkmer G.L.,
Razeira M.,
Vasconcellos C.A.Z.
Publication year - 2017
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.201713439
Subject(s) - physics , dark energy , general relativity , dark matter , gravitational collapse , equation of state , astrophysics , compact star , dark fluid , gravitation , hydrostatic equilibrium , cosmology , stars , classical mechanics , astronomy , quantum mechanics
In the theory of pseudo‐complex general relativity (pc‐GR), the field equations have an extra term, associated with the nature of space‐time, of repulsive character, which may halt the gravitational attractive collapse of matter distributions in the evolution process of compact stars. This additional term arises from microscale phenomena due to vacuum fluctuations, which simulate the presence of dark energy in the Universe. In this paper, we explore the presence of this additional term and propose a toy model consisting of dark matter, represented by standard model Fermi gauge singlets having their origin in the Higgs portal model , held together by the presence of the gravitational interaction and superimposed on the repulsive background of dark energy forming a type of unconventional and nonluminous star, composed only of dark matter and dark energy, a rare compact object formed solely by exotic content. The combination of these two ingredients, namely gravitational attraction and dark energy repulsion, allows the hydrostatic equilibrium condition of the star to hold. Solving the corresponding field equations and the Tolman‐Oppenheimer‐Volkoff (TOV) equations, and assuming that the fluid components interact only gravitationally, we determine the hydrostatic equilibrium equations of the star. We then analyze the corresponding results obtained for the equation of state and for the mass–radius relations and then determine the maximum mass of the exotic star for different parameter configurations.