| 英文摘要
| The rapid development of space detection technology provides technical support for our study of dark energy, dark matter and other cosmological issues. In the process of exploring dark energy, all hypothetical models must be tested by experimental observations. The general step is to theorize the behavior of cosmological evolution and then test whether the observed data agrees with the model. The Sandage-Loeb (S-L) test serves as an experiment to measure the redshift of a distant object, which reflects the change in the expansion rate of the universe. Although the principle of this experiment is simple, it is capable of providing independent evidence on the existence of dark energy without making assumptions on space-time curvature, any cosmological approximations, or astrophysical postulations from unique observations.
In this publication, we first used the Sandage-Loeb method to detect the non-gravitational interactions between the three types of dark matter and dark energy to expand the dark energy model of holographic Ricci. The phenomenological is proportional to Hubble’s expansion rate and energy density of the dark component ( , , and respectively), yielding the analytical solutions of the three interactions. We found out that the interacting holographic dark energy model with Hubble parameters can be distinguished from the holographic dark energy model. In addition, the S-L test is not sensitive to the change of Ωm0 in the model. The size of Ωm0 represents the quantity of the entire component. Since its change has little effect on the test results, it is not the main reason for the accelerated expansion of the universe. Next, we examined the change of the cosmic component in the Quintessence dark energy model. When the state equation is transformed from w = -1 into a discrete function, we observed a gradual increase or decrease of cosmic component based on the value of w. Hence, we identified that when wu003e0.4, the change is significant. Finally, we obtained the analytical results of the dark energy model in the range of redshift 2 ≤ z ≤ 5. Applying the redshift range and the discrete function to the S-L test, we concluded that the sensitivity of different models regarding universe expansion varies and that w has a greater impact on the model under high redshift. The initial value of the best fit range is Ω_m0＝〖0.287〗_(-0.027-0.036)^(+0.029+0.039). |
