A mathematical description of the Sun’s structure that gives the variation of pressure, temperature, and other quantities with radius from the Sun’s centre. It is obtained by considering how a mass of gas simulating the Sun at its birth evolves to its present state, with radius and luminosity matching measured values. The most recent models give a core temperature of 15.6 million K and a density of 148 000 kg/m3. Many models of stellar evolution are calibrated with respect to this standard solar model.