Planck E PressCenter Articles
How Does the Sun Work?
Date published: 2023-04-14
Date modified: 2023-04-14
Reading time: 00:01:04
“Sunshine is my quest.”
Winston Churchill
There is a direct relationship between the kinetic energy and the shock it causes in the incident particle.
For fluxes of kinetic energy inferior to 10,000 electron-volts, the cross-section is very small because the Coulomb barrier is broken.
In the interior of the Sun, reactions of this type occur all the time, and even though they occur at extremely low productivity rates, solar nuclear fusions are extremely efficient given the immense mass of the star.
And this is one of the most difficult problems to solve when we think about nuclear fusion reactors for energy production on Earth: the penetration of the Coulomb barrier would have to be much more expressive, and in this case, the temperature inside the reactor would have to be -at least- 10,000,000K, which is the average temperature of the Sun.
The mass of our star is so large that its gravitational field naturally produces this container.
The efficient thermal fusion observed in stars is the result of the balance between protons, neutrons, positrons, antineutrinos, and gamma rays immediately after the Big Bang.
The fusion of two hydrogens produces the noble and stable gas helium, which today occupies about 10% of interstellar space, and the increase in density of this gas leads to an ever greater accumulation of matter until there is the sufficient gravitational attraction to guarantee the stability of the mass. When the core temperature exceeds 100,000K, complete ionization of the hydrogen atoms occurs, forming a plasma of protons and neutrons. At 10,000,000K, the movement of the protons is such that the kinetic energy allows the Coulomb barrier to be breached, albeit at a low rate.
And the sun rises.
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