Cooling flows in galaxy clusters involve gas cooling in the central regions, where radiative cooling times are much shorter than in outer regions. Observations with XMM and Chandra suggest that gas cooling below 1–2 keV is not evident, despite the short cooling times. Chandra images reveal complex structures like cold fronts and radio lobes, indicating that the core regions are not simply cooling but are instead dynamically active. The cooling flow picture is challenged by the lack of observed mass cooling rates and the presence of cold gas and dust in cluster cores. The cooling of gas in the central regions may be balanced by heating mechanisms, such as energy from radio sources or infalling subclusters. However, the exact nature and efficiency of this heating remain unclear. Numerical simulations suggest that cooling flows are common in galaxy clusters, and recent observations support this. Chandra data show that the cores of clusters are complex, with structures like cold fronts and filaments. The temperature drops significantly in the central regions, but the cooling process is not straightforward. Some gas may cool and mix with surrounding gas, leading to the observed cold gas and dust. This process may contribute to star formation and further cooling. XMM-Newton data indicate that the cooling of gas below 1–2 keV is not evident, possibly due to absorption or mixing with hotter gas. The presence of cold gas and dust in cluster cores suggests that more star formation may occur than previously thought. The cooling flow phenomenon is an important aspect of galaxy evolution, as it influences the mass and luminosity of galaxies. The balance between cooling and heating is crucial for understanding the dynamics of galaxy clusters. Observational and theoretical studies continue to explore the mechanisms behind this complex process.Cooling flows in galaxy clusters involve gas cooling in the central regions, where radiative cooling times are much shorter than in outer regions. Observations with XMM and Chandra suggest that gas cooling below 1–2 keV is not evident, despite the short cooling times. Chandra images reveal complex structures like cold fronts and radio lobes, indicating that the core regions are not simply cooling but are instead dynamically active. The cooling flow picture is challenged by the lack of observed mass cooling rates and the presence of cold gas and dust in cluster cores. The cooling of gas in the central regions may be balanced by heating mechanisms, such as energy from radio sources or infalling subclusters. However, the exact nature and efficiency of this heating remain unclear. Numerical simulations suggest that cooling flows are common in galaxy clusters, and recent observations support this. Chandra data show that the cores of clusters are complex, with structures like cold fronts and filaments. The temperature drops significantly in the central regions, but the cooling process is not straightforward. Some gas may cool and mix with surrounding gas, leading to the observed cold gas and dust. This process may contribute to star formation and further cooling. XMM-Newton data indicate that the cooling of gas below 1–2 keV is not evident, possibly due to absorption or mixing with hotter gas. The presence of cold gas and dust in cluster cores suggests that more star formation may occur than previously thought. The cooling flow phenomenon is an important aspect of galaxy evolution, as it influences the mass and luminosity of galaxies. The balance between cooling and heating is crucial for understanding the dynamics of galaxy clusters. Observational and theoretical studies continue to explore the mechanisms behind this complex process.