English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Dynamical behavior and future singularities of $f(R, T,R_{\mu\nu}T^{\mu\nu})$gravitational theory are investigated. This gravitational model is a morecomplete form of the $f(R,T)$ gravity which can offer new dynamics for theuniverse. We investigate this gravitational theory for the case $f = R + \alphaR_{\mu\nu}T^{\mu\nu}$ using the method of autonomous dynamical systems and byassuming an interaction between matter and dark energy. The fixed points areidentified and the results are consistent with standard cosmology and show thatfor small $\alpha$, the radiation dominated era is an unstable fixed point ofthe theory and the universe will continue its procedure toward matter era whichis a saddle point of the theory and allows the evolution to dark energydominated universe. Finally the dark energy dominated epoch is a stable fixedpoint and will be the late time attractor for the universe. We also considerfuture singularities for the two $f = R + \alpha R_{\mu\nu}T^{\mu\nu}$ and $f =R +\alpha RR_{\mu\nu}T^{\mu\nu}$ cases and for $w = 0,\dfrac{1}{3},1$ and $-1$.Our results show that for the case of $f = R + \alpha R_{\mu\nu}T^{\mu\nu}$,the future singularities of the universe will happen in the same condition asdo for the Einstein-Hilbert FRW universe. However, a new type of singularity isobtained for $f = R +\alpha RR_{\mu\nu}T^{\mu\nu}$ that is captured by$t\rightarrow t_s;\ a \rightarrow a_s;\ \rho\rightarrow \infty;$ and $\ |p|\rightarrow 0$.

Late time dynamics of $f(R, T, R_{\mu\nu}T^{\mu\nu})$ gravity