Static spherically symmetric three-form stars

Abstract

We consider interior static and spherically symmetric solutions in a gravity theory that extends the standard Hilbert-Einstein action with a Lagrangian constructed from a three-form field $A_{\alpha \beta \gamma }$, which generates, via the field strength and a potential term, a new component in the total energy-momentum tensor of the gravitational system. We formulate the field equations in Schwarzschild coordinates and investigate their solutions numerically for different equations of state of neutron and quark matter, by assuming that the three field potential is either a constant or possesses a Higgs-like form. Moreover, stellar models, described by the stiff fluid, radiation-like, bag model and the Bose-Einstein condensate equations of state are explicitly obtained in both general relativity and three-form gravity, thus allowing an in-depth comparison between the astrophysical predictions of these two gravitational theories. As a general result we find that for all the considered equations of state, three-form field stars are more massive than their general relativistic counterparts. As a possible astrophysical application of the obtained results, we suggest that the 2.5$M_{\odot }$ mass compact object, associated with the GW190814 gravitational wave event, could be in fact a neutron or a quark star described by the three-form field gravity theory.

23 pages, 24 figures; minor modifications, accepted for publication in EPJC

References in corpus (16)

• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• f(R,T) gravity
• Cosmology of hybrid metric-Palatini f(X)-gravity
• Can accretion disk properties distinguish gravastars from black holes?
• Testing Hořava-Lifshitz gravity using thin accretion disk properties
• Inflation from N-Forms and its stability
• Thin accretion disk signatures of slowly rotating black holes in Hořava gravity
• Hybrid metric-Palatini stars
• Interacting 3-form dark energy models: distinguishing interactions and avoiding the Little Sibling of the Big Rip
• Relativistic stars with a linear equation of state: analogy with classical isothermal spheres and black holes
• Testing Bose-Einstein Condensate dark matter models with the SPARC galactic rotation curves data
• Cosmic infinity: A dynamical system approach
• Thin accretion disks around cold Bose-Einstein Condensate stars
• Inflation in a two 3-form fields scenario
• Radiation Fluid Stars in the Non-minimally Coupled $Y(R)F^2$ Gravity