CNO cycle

Their models were similar to the later CNO cycle.

This is the case because it is a part of the CNO cycle.

The core became convective and utilized the CNO cycle for energy generation.

By contrast, stars with 1.8 solar masses or above generate almost their entire energy output through the CNO cycle.

Unlike the latter, the CNO cycle is a catalytic cycle.

Stars in the upper main sequence have sufficiently high core temperatures to efficiently use the CNO cycle.

The CNO cycle is very temperature sensitive, so it is strongly concentrated at the core.

This core convection occurs in stars where the CNO cycle contributes more than 20% of the total energy.

Nitrogen-13 plays a significant role in the CNO cycle, which is the dominant source of energy in stars heavier than the sun.

When helium fusion comes to an end at the core, convection mixes the products of the CNO cycle.

This explosive stellar nucleosynthesis begins with the hot CNO cycle which quickly yields to the rp-process.

As a main sequence star ages, the core temperature will rise, resulting in a steadily increasing contribution from its CNO cycle.

The seed nuclei needed for this process to occur are thought to be formed during breakout reactions from the hot CNO cycle.

These processes are a simple result of the star's size and temperature, with only quite large stars using the carbon cycle (the CNO cycle).

Neutrinos are also produced by the CNO cycle, but that process is considerably less important in the Sun than in other stars.

Hydrogen plays a vital role in powering stars through proton-proton reaction and CNO cycle nuclear fusion.

The energy generation in main-sequence B-type stars comes from the CNO cycle of thermonuclear fusion.

Another of the fusion mechanisms powering stars is the CNO cycle, in which carbon acts as a catalyst to allow the reaction to proceed.

The proton-proton chain reaction is one of several fusion reactions by which stars convert hydrogen to helium, the primary alternative being the CNO cycle.

Theoretical models show that the CNO cycle is the dominant source of energy in stars more massive than about 1.3 times the mass of the Sun.

Although there are various paths and catalysts involved in the CNO cycles, simply speaking all these cycles have the same net result:

A nova results from runaway hydrogen fusion (via the CNO cycle) in the outer layer of a carbon-oxygen white dwarf star.

In most stars the fuel is provided by hydrogen, which can combine together to form helium through the proton-proton chain reaction or by the CNO cycle.

Under typical conditions found in stellar plasmas, catalytic hydrogen burning by the CNO cycles is limited by proton captures.

Because of the long timescales involved, the cold CNO cycles convert hydrogen to helium slowly, allowing them to power stars in quiescent equilibrium for many years.