Helium Flash - Core Helium Flash

For a star with a mass less than 2.25 solar masses, the core helium flash occurs when the core runs out of hydrogen, and the thermal pressure is no longer sufficient to counter the gravitational collapse. This causes the star to start contracting. During the contraction the core becomes hotter and hotter until it causes the outer layers to begin fusing hydrogen and expand outwards, initiating the red giant stage. As the star continues contracting due to gravity, it eventually becomes compressed enough that it becomes degenerate matter. This degeneracy pressure is finally sufficient to stop further collapse of the most central material. As the rest of the core continues to contract and the temperature continues to rise, a temperature (≈1×108 K) is reached at which the helium can start to fuse, and so helium ignition occurs.

The explosive nature of the helium flash arises from its taking place in degenerate matter. Once the temperature reaches 100 million–200 million kelvins and helium fusion begins using the triple-alpha process, the temperature rapidly increases, further raising the helium fusion rate and, because degenerate matter is a good conductor of heat, widening the reaction region.

However, since degeneracy pressure (which is purely a function of density) is dominating thermal pressure (proportional to the product of density and temperature), the total pressure is only weakly dependent on temperature. Thus, the dramatic increase in temperature only causes a slight increase in pressure, so there is no stabilizing cooling expansion of the core.

This runaway reaction quickly climbs to about 100 billion times the star's normal energy production (for a few seconds) until the temperature increases to the point that thermal pressure again becomes dominant, eliminating the degeneracy. The core can then expand and cool down and a stable burning of helium will continue.

A star with mass greater than about 2.25 solar masses starts to burn helium without its core, becoming degenerate, and so does not exhibit this type of helium flash. In a very low-mass star (less than about 0.5 solar mass), the core is never hot enough to ignite helium. The degenerate helium core will keep on contracting, and finally becomes a helium white dwarf.

The helium flash is not directly observable on the surface by electromagnetic radiation. The flash occurs in the core deep inside the star, and the net effect will be that all released energy is absorbed by the entire core, leaving the degenerate state to become nondegenerate. Earlier computations indicated that a nondisruptive mass loss would be possible in some cases, but later star modeling taking neutrino energy loss into account indicates no such mass loss.