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To help clarify the nomenclature of celestial bodies, Gibor Basri proposed to the IAU that any "object that achieves core fusion during its lifetime" be called a fusor. [ 1 ] This definition includes any form of nuclear fusion , so the lowest possible mass of a fusor was set at roughly 13 M J ( Jupiter masses ) at which point deuterium fusion ...
As a result, there is little mixing of fresh hydrogen into the core or fusion products outward. In higher-mass stars, the dominant energy production process is the CNO cycle , which is a catalytic cycle that uses nuclei of carbon, nitrogen and oxygen as intermediaries and in the end produces a helium nucleus as with the proton–proton chain ...
The Corefusion Mark was released on March 12, 2003. The processor core is based on the VIA C3 'Nehemiah', and includes the VIA ProSavage CLE266 Northbridge and the S3 Graphics ProSavage4 graphics processing unit. It supports 133 MHz SDRAM. Specifications (C3 Core) L1-Cache: 64 + 64 kB (Data + Instructions) L2-Cache: 64 kB; MMX, 3DNow!, SSE
In fusion power research, the Z-pinch (zeta pinch) is a type of plasma confinement system that uses an electric current in the plasma to generate a magnetic field that compresses it (see pinch). These systems were originally referred to simply as pinch or Bennett pinch (after Willard Harrison Bennett ), but the introduction of the θ-pinch ...
The horizontal branch (HB) is a stage of stellar evolution that immediately follows the red-giant branch in stars whose masses are similar to the Sun's. Horizontal-branch stars are powered by helium fusion in the core (via the triple-alpha process) and by hydrogen fusion (via the CNO cycle) in a shell surrounding the core.
The core never reaches high enough temperature for further fusion burning of heavier elements than carbon. [13] Stars of more than 12 solar masses start carbon burning in a non-degenerate core, [14] and after carbon exhaustion proceed with the neon-burning process once contraction of the inert (O, Ne, Na, Mg) core raises the temperature ...
A stellar core is the extremely hot, dense region at the center of a star. For an ordinary main sequence star, the core region is the volume where the temperature and pressure conditions allow for energy production through thermonuclear fusion of hydrogen into helium.
Silicon burning begins when gravitational contraction raises the star's core temperature to 2.7–3.5 billion kelvins . The exact temperature depends on mass. When a star has completed the silicon-burning phase, no further fusion is possible. The star catastrophically collapses and may explode in what is known as a Type II supernova.