Fig5_1 Nuclear tunneling in the Sun's core

Fig5_1 Nuclear tunneling in the Sun

Fig. 5.1 . The high-speed tail (left) of the Maxwellian distribution of nuclear particle speeds plotted as a function of kinetic energy, E, for protons near the center of the Sun. The P(E) function (right) describes the quantum mechanical probability of two protons overcoming the electrical repulsion between them; it depends on the Gamow energy EG and the relative energy E of the two colliding protons. The function f(E) is the product of the speed and penetration function (center), and it determines the nuclear reaction rate in the core of the Sun.

Copyright 2010, Professor Kenneth R. Lang, Tufts University