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Finding the best interacting dark energy model with observed data

  • Original Paper - Geophysics and Astrophysics
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Abstract

Dark energy and dark matter problem is one of the most important issues in modern cosmology. There are many candidate models explaining the current observed dark matter and dark energy density parameters. One of the promising models is the interacting dark energy model with holographic principle applied. It was shown that interacting holographic dark energy model in non-flat universe cannot accommodate a transition from the dark energy to the phantom regime and its background cosmological evolution is compatible to current observational data of energy fractions between dark matter and dark energy. However, only a few selected parameters yielded compatible cosmological background evolution. In this article, we want to extend this model to incorporate the current observed Hubble data as red shift. It was shown that the physical parameter most compatible to observed data are \(H_0 \sim 68\) and interaction parameter \(b^2 \sim 0.009\). We have applied a simple numerical regression technique to find out the best interacting model parameters to fit the current observational data. We have shown that the background cosmological evolution is insensitive to interaction strength but the evolution of Hubble constant.

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Acknowledgements

H.W. Lee and J.C. Kim were supported by the National Research Foundation of Korea (NRF) (No. NRF-2018R1D1A1B05049338). K.Y. Kim was supported by “Regional Innovation Strategy (RIS)” through the National Research Foundation of Korea(NRF) funded by the Ministry of Education (MOE).

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  1. Institute of Basic Science & College of AI Convergence, Inje University, 197 Inje-ro, Gimhae, 50834, Korea

    JeongCho Kim, Hyung Won Lee & Kyoung Yee Kim

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  1. JeongCho Kim
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Correspondence to Kyoung Yee Kim.

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Kim, J., Lee, H.W. & Kim, K.Y. Finding the best interacting dark energy model with observed data. J. Korean Phys. Soc. 81, 191–197 (2022). https://doi.org/10.1007/s40042-022-00517-8

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  • DOI: https://doi.org/10.1007/s40042-022-00517-8

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