Solar convection is a fundamental concept in solar physics that investigates the turbulent bulk motion of plasma within specific layers of the Sun, primarily the convection zone, as a mechanism for energy transport. This research area focuses on understanding how thermal energy generated in the Sun's core is transported outward through the rise of hot, less dense plasma and the descent of cooler, denser plasma, significantly influencing the Sun's internal structure, surface phenomena like granulation and supergranulation, and driving solar activity such as the solar dynamo and magnetic field generation.