Locally Varying Hubble Parameter in Terms of Reduced Friedmann Equation  

作　　者：Ayman Kassem Ayman Kassem(Egyptair, Cairo, Egypt)

机构地区：[1]Egyptair, Cairo, Egypt

出　　处：《International Journal of Astronomy and Astrophysics》2021年第2期175-189,共15页天文学与天体物理学国际期刊（英文）

摘　　要：Assessment of the Hubble parameter as an indicator of the expansion rate of the universe holds a central position in the field of astronomy. From its initial estimate of about 500 km<span style="white-space:nowrap;">&sdot;</span>sec^-1<span style="white-space:nowrap;">&sdot;</span>parsc^-1, this value had been steadily amended as the observational tools became more accurate and precise. Despite this, a gap remains between the value of observations relating to local and nonlocal estimations of the Hubble parameter that gave rise to what became known as the Hubble tension. This tension is addressed here while dealing with space fabric as a cosmological fluid that undergoes transition.Assessment of the Hubble parameter as an indicator of the expansion rate of the universe holds a central position in the field of astronomy. From its initial estimate of about 500 km<span style="white-space:nowrap;">&sdot;</span>sec^-1<span style="white-space:nowrap;">&sdot;</span>parsc^-1, this value had been steadily amended as the observational tools became more accurate and precise. Despite this, a gap remains between the value of observations relating to local and nonlocal estimations of the Hubble parameter that gave rise to what became known as the Hubble tension. This tension is addressed here while dealing with space fabric as a cosmological fluid that undergoes transition.

关 键 词：Cosmic Fluid Transition Locally Varying Hubble Parameter Energy Degrees of Freedom 

分 类 号：P15[天文地球—天文学]