CNO cycle Totally Explained

Everything about The Cno Cycle totally explained

The CNO cycle (for carbon-nitrogen-oxygen), or sometimes Bethe-Weizsäcker-cycle, is one of two sets of fusion reactions by which stars convert hydrogen to helium, the other being the proton-proton chain. Theoretical models show that the CNO cycle is the dominant source of energy in stars heavier than the sun. The proton-proton chain is more important in stars the mass of the sun or less. This difference stems from temperature dependency differences between the two reactions; pp-chain reactions start occurring at temperatures around ~4 K, making it the dominant force in smaller stars. The CNO chain starts occurring at ~13 K, but its energy output rises much faster with increasing temperatures. At ~17 K, the CNO cycle start becoming the dominant source of energy. The sun has a temperature of around ~15.7 K and only 1.7% of ⁴He nuclei being produced in the Sun are born in the CNO cycle. The CNO process was proposed by Carl von Weizsäcker and Hans Bethe independently in 1938 and 1939, respectively.
In the CNO cycle, four protons fuse using carbon, nitrogen and oxygen isotopes as a catalysist to produce one alpha particle, two positrons and two electron neutrinos . The positrons will almost instantly annihilate with electrons, releasing energy in the form of gamma rays. The neutrinos escape from the star carrying away some energy. The carbon, nitrogen, and oxygen isotopes are in effect one nucleus that goes through a number of transformations in an endless loop.

CNO-I

The main reactions of the CNO cycle are :

Note that all CNO cycles have the same net result: ť 4 → + 2 + 2 + + 26.8 MeV

Use in astronomy

While the total number of "catalytic" CNO nuclei is conserved in the cycle, in stellar evolution the relative proportions of the nuclei are altered. When the cycle is run to equilibrium, the ratio of the carbon-12/carbon-13 nuclei is driven to 3.5, and nitrogen-14 becomes the most numerous nucleus, regardless of initial composition. During a star's evolution, convective mixing episodes bring material in which the CNO cycle has operated from the star's interior to the surface, altering the observed composition of the star. Red giant stars are observed to have lower carbon-12/carbon-13 and carbon-12/nitrogen-14 ratios than main sequence stars, which is considered to be proof of nuclear energy generation in stars by hydrogen fusion.
The presence of the heavier elements carbon, nitrogen and oxygen places an upward bound on the maximum size of massive stars to approximately 150 solar masses. It is thought that the "metal-poor" early universe could have had stars up to 250 solar masses without interference from the CNO cycle.

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