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The thermal history of the intergalactic medium is full of extremely usefuldata in the field of astrophysics and cosmology. In other words, by examiningthis environment in different redshifts, the effects of cosmology andastrophysics can be observed side by side. Therefore, simulation is our verypowerful tool to reach a suitable model for the intergalactic medium, both interms of cosmology and astrophysics. In this work, we have simulated theintergalactic medium with the help of the 21cmFAST code and compared theevolution of the neutral hydrogen fraction in different initial conditions.Considerable works arbitrarily determine many important effective parameters inthe thermal history of the intergalactic medium without any constraints, andusually, there is a lot of flexibility for modeling. Nonetheless, in this work,by focusing on the evolution of the neutral hydrogen fraction in differentmodels and comparing it with observational data, we have eliminated many modelsand introduced only limited simulation models that could confirm theobservations with sufficient accuracy. This issue becomes thoroughly vital fromthe point that, in addition to restricting the models through the neutralhydrogen fraction, it can also impose restrictions on the parameters affectingits changes. However, we hope that in future works, by enhancing theobservational data and increasing their accuracy, more compatible models withthe history of the intergalactic medium can be achieved.

A New Constraint on the Simulation of the Intergalactic Medium through the Evolution of the Neutral Hydrogen Fraction in the Epoch of Reionization