Some Studies On The Orbital Dynamics Of Black Holes And Properties Of Quark Stars In The Ho(?)ava-Lifshitz Theory Of Gravity

The detection of gravitational waves and event horizon telescopes has stimulated a strong interest in the exploration of dense stars.The recent observation of dense stars with masses of about 2.50-2.67 M⊙ by the GW 190814 gravitational wave event has led researchers to investigate the modified gravitational theory and the structure of microscopic matter.Based on this,in the framework of Ho(?)avaLifshitz(HL)gravitational theory,the study of the structure of the black hole spacetime geodesic and the matter structure of quark stars is carried out in this paper,and the main works are as follows:1.In the second chapter,the geodesic structure of HL black hole spacetime is analyzed by using the effective potential method.For time-like geodesics,the unstable circular orbit radius ru,the innermost circular orbit radius rms and the minimum radius bound orbit rmb all increase with the increase of the parameterω in HL black hole space-time.The orbit radius rs decreases with the increase of ω.For optical geodesics:unstable circular orbit radius ru and HL black hole shadow radius RS increase with the increase of ω.As ω approaches infinity,all characteristic orbitals return to their corresponding solutions in the Schwarzschild black hole.2.In the third chapter,the properties of quark stars under HL gravitational theory are studied by numerical simulation.Firstly,quark stars with ColorFlavor-Locked(CFL)phases are studied.The effects of the parameter ω in HL gravity and the bag constant B in quark star state equation on the mass-radius relationship and density of quark stars are analyzed.Secondly,the material structure of isotropic quark stars is studied by using the equation of state of interacting quark matter,and the effects of the parameters ω in HL gravity and a4 in the equation of state on the mass-radius relationship and density of quark stars are analyzed.Thirdly,The effects of a4⊥,B⊥,ω on the properties of anisotropic quark stars with interacting quark matter are analyzed,and the numerical results obtained are compared with the isotropic case.The numerical results of these three types of quark stars show that the maximum mass decreases with the increase of the bag constant B,and increases with the decrease of ω.The maximum mass can all reach above 2 M⊙.This is consistent with observations of pulsars PSR J0348+0432,PSR J0751+1807,and gravitational wave GW 190814.Finally,anisotropic quark stars with large masses and high densities are of great significance for the study of revised gravity theory and the structure of matter.