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The core is made of hot, dse plasma (ions and electrons), at a pressure estimated at 265 billion bar (3.84 trillion psi or 26.5 petapascals (PPa)) at the cter.
Due to fusion, the composition of the solar plasma drops from 68 to 70% hydrog by mass at the outer core, to 34% hydrog at the core/Sun cter.
The core inside 20% of the solar radius contains 34% of the Sun's mass, but only 0.8% of the Sun's volume. Inside 24% of the solar radius is the core which gerates 99% of the fusion power of the Sun. There are two distinct reactions in which four hydrog nuclei may evtually result in one helium nucleus: the proton–proton chain reaction – which is responsible for most of the Sun's released ergy – and the CNO cycle.
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The Sun at the photosphere is about 73–74% by mass hydrog, which is the same composition as the atmosphere of Jupiter, and the primordial composition of hydrog and helium
At the earliest star formation after the Big Bang. However, as depth into the Sun increases, fusion decreases the fraction of hydrog. Traveling inward, hydrog mass fraction starts to decrease rapidly after the core radius has be reached (it is still about 70% at a radius equal to 25% of the Sun's radius) and inside this, the hydrog fraction drops rapidly as the core is traversed, until it reaches a low of about 33% hydrog, at the Sun's cter (radius zero). All but 2% of the remaining plasma mass (i.e., 65%) is helium.
, or roughly 600 million tonnes of hydrog, are converted into helium nuclei every second releasing ergy at a rate of 3.86×10
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The core produces almost all of the Sun's heat via fusion: the rest of the star is heated by the outward transfer of heat from the core. The ergy produced by fusion in the core, except a small part carried out by neutrinos, must travel through many successive layers to the solar photosphere before it escapes into space as sunlight, or else as kinetic or thermal ergy of massive particles. The ergy conversion per unit time (power) of fusion in the core varies with distance from the solar cter. At the cter of the Sun, fusion power is estimated by models to be about 276.5 watts/m
Despite its intse temperature, the peak power gerating dsity of the core overall is similar to an active compost heap, and is lower than the power dsity produced by the metabolism of an adult human. The Sun is much hotter than a compost heap due to the Sun's ormous volume and limited thermal conductivity.
The low power outputs occurring inside the fusion core of the Sun may also be surprising, considering the large power which might be predicted by a simple application of the Stefan–Boltzmann law for temperatures of 10 to 15 million kelvins. However, layers of the Sun are radiating to outer layers only slightly lower in temperature, and it is this differce in radiation powers betwe layers which determines net power geration and transfer in the solar core.
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At 19% of the solar radius, near the edge of the core, temperatures are about 10 million kelvins and fusion power dsity is 6.9 W/m
Some 91% of the solar ergy is produced within this radius. Within 24% of the radius (the outer core by some definitions), 99% of the Sun's power is produced. Beyond 30% of the solar radius, where temperature is 7 million K and dsity has fall to 10 g/cm
There are two distinct reactions in which 4 H nuclei may evtually result in one He nucleus: proton–proton chain reaction and the CNO cycle (see below).
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The first reaction in which 4 H nuclei may evtually result in one He nucleus, known as the proton–proton chain reaction, is:
This reaction sequce is thought to be the most important one in the solar core. The characteristic time for the first reaction is about one billion years ev at the high dsities and temperatures of the core, due to the necessity for the weak force to cause beta decay before the nucleons can adhere (which rarely happs in the time they tunnel toward each other, to be close ough to do so). The time that deuterium and helium-3 in the next reactions last, by contrast, are only about 4 seconds and 400 years. These later reactions proceed via the nuclear force and are thus much faster.
The second reaction sequce, in which 4 H nuclei may evtually result in one He nucleus, is called the CNO cycle and gerates less than 10% of the total solar ergy. This involves carbon atoms which are not consumed in the overall process. The details of this CNO cycle are as follows:
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Therefore, the fusion rate in the core is in a self-correcting equilibrium: a slightly higher rate of fusion would cause the core to heat up more and expand slightly against the weight of the outer layers.
This would reduce the fusion rate and correct the perturbation; and a slightly lower rate would cause the core to cool and shrink slightly, increasing the fusion rate and again reverting it to its prest level.
However the Sun gradually becomes hotter during its time on the main sequce, because the helium atoms in the core are dser than the hydrog atoms they were fused from. This increases the gravitational pressure on the core which is resisted by a gradual increase in the rate at which fusion occurs. This process speeds up over time as the core gradually becomes dser. It is estimated that the Sun has become 30% brighter in the last four and a half billion years
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The high-ergy photons (gamma rays) released in fusion reactions take indirect paths to the Sun's surface. According to currt models, random
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