Update index.md

index.md

@@ -101,7 +101,7 @@ The study revealed several important trends in the evolution of cosmic filaments
 
 The most important results have been shown in Figure 3. Temperature profiles showed a clear increase as a function of decreasing redshift, highlighting the progressive heating of the IGM by ionizing sources. High-density filaments developed distinct thermal envelopes, with peak temperatures observed at increasing distances from their central axes over time. Interestingly, while lower-density filaments also experienced heating, they lacked the pronounced temperature peaks seen in their higher-density counterparts.
 
-The analysis of neutral fraction profiles revealed a shift in the ionization pattern as reionization progressed. At early redshifts, dense regions of the filamentary network were the first to become ionized, driven by their proximity to radiation sources. By later stages of the EoR, the ionization process transitioned to an outside-in pattern, with less dense regions becoming the most ionized. What it means is that at redshift 9, the denser regions being nautrally closer to the ionizing sources receive the effect of the ionizing bubbles first, but as time progresses, the expanding bubbles reach the emptier regions of the IGM, which are less shielded from the background radiation, and ionise them even more than the denser regions. # Evolution of the IGM Neutral Fraction During Reionization. By **z=7**, the intergalactic medium (IGM) reaches a nearly uniformly ionized state, with ionizing photons forming a pervasive background. At this stage, gas density becomes the dominant factor influencing the neutral fraction:
+The analysis of neutral fraction profiles revealed a shift in the ionization pattern as reionization progressed. At early redshifts, dense regions of the filamentary network were the first to become ionized, driven by their proximity to radiation sources. By later stages of the EoR, the ionization process transitioned to an outside-in pattern, with less dense regions becoming the most ionized. By **z=7**, the intergalactic medium (IGM) reaches a nearly uniformly ionized state, with ionizing photons forming a pervasive background. At this stage, gas density becomes the dominant factor influencing the neutral fraction:
 
 $x_\mathrm{HI} \propto \frac{\rho_\mathrm{gas}}{\rho_\mathrm{radiation}}$