The core of the Sun is considered to extend from the center to about 0.2 to 0.25 solar radius. It is the hottest part of the Sun and of the Solar System. It has a density of up to 150 g/cm³ (150 times the density of liquid water) and a temperature of close to 15,000,000 kelvin, or about 27,000,000 Fahrenheit; by contrast, the surface of the Sun is close to 6,000 kelvin. The core is made of hot, dense gas in the plasmic state. The core, inside 0.24 solar radius, generates 99% of the fusion power of the Sun.
Energy production 
About 3.6×1038 protons (hydrogen nuclei) are converted into helium nuclei every second, releasing mass and energy at the mass-energy equivalence rate of 4.3 million tonnes per second, 380 yottawatts (3.8×1026 watts), equivalent to 9.1 ×1010 megatons of TNT per second.
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 energy 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 kinetic energy of particles.
The energy production per unit time (power) of fusion in the core varies with distance from the solar center. At the center of the Sun, fusion power is estimated by models to be about 276.5 watts/m3.
The power production density of the core overall is similar to the metabolic production density of a reptile. The peak power production in the Sun's center, per volume, has been compared to the volumetric heat generated in an active compost heap. The tremendous power output of the Sun is due not to its high power per volume, but rather to its gigantic size.
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 degrees kelvin. However, layers of the Sun are radiating to outer layers only slightly lower in temperature, and it is this difference in radiation powers between layers which determines net power production and transfer in the solar core.
At 19% of the solar radius, near the edge of the core, temperatures are about 10 million degrees kelvin and fusion power density is 6.9 watts/m3, which is about 2.5% of the maximum value at the solar center. Some 91% of the solar energy is produced within this radius. Within 24% of the radius (the outer "core" by some definitions), 99% of the Sun's power is produced. At 30% of the solar radius, the rate of fusion is almost nil.
The rate of nuclear fusion depends strongly on density, so 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, reducing the fusion rate and correcting 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 present level.
Energy transfer 
The high-energy photons (gamma rays and x-rays) released in fusion reactions take a long time to reach the Sun's surface, slowed down by the indirect path taken, as well as by constant absorption and reemission at lower energies in the solar mantle. Estimates of the "photon travel time" range from as much as 50 million years to as little as 17,000 years. However, the concept of photon travel is not a well-defined one, since photons are not conserved, and one photon at a high temperature normally turns into many photons at a lower temperature, during passage of heat out of the solar core to the Sun's photosphere. The long periods of time (tens of millions of years) refer to the characteristic time for the entire solar temperature distribution to change, as a result of changing heat generation rate in the core. This is far longer than the average time for transport of heat through the Sun because most of the Sun's heat capacity is in the kinetic energy of the particles in its plasma, not in the electromagnetic radiation present within it. The shorter estimates of photon travel time (tens of thousands of years) refer to the relatively rapid mean time needed for radiation to travel from the center of the Sun to the photosphere, even though the Sun's heat cannot pass from core to surface at this rate, due to the large heat capacity needed to be heated or cooled in the process, as mentioned above.
After a final trip through the convective outer layer to the transparent surface of the photosphere, the photons escape as visible light. Each gamma ray in the Sun's core is converted into several million visible light photons before escaping into space. Neutrinos are also released by the fusion reactions in the core, but unlike photons they very rarely interact with matter, so almost all are able to escape the Sun immediately. For many years measurements of the number of neutrinos produced in the Sun were much lower than theories predicted, a problem which was recently resolved through a better understanding of the effects of neutrino oscillation.
- García, Ra; Turck-Chièze, S; Jiménez-Reyes, Sj; Ballot, J; Pallé, Pl; Eff-Darwich, A; Mathur, S; Provost, J (Jun 2007). "Tracking solar gravity modes: the dynamics of the solar core.". Science 316 (5831): 1591–3. Bibcode:2007Sci...316.1591G. doi:10.1126/science.1140598. ISSN 0036-8075. PMID 17478682.
- Table of temperatures, power densities, luminosities by radius in the sun
- A 50 kg adult human has a volume of about 0.05 m3, which would correspond to 13.8 watts at the volumetric power of the solar center. This is 285 Kcal = Cal/day, about 10% of the actual average caloric intake and output for humans in non-stressful conditions.
- Lewis, Richard (1983). The Illustrated Encyclopedia of the Universe. Harmony Books, New York. p. 65.
- Plait, Phil (1997). "Bitesize Tour of the Solar System: The Long Climb from the Sun's Core". Bad Astronomy. Retrieved 2006-03-22.
- Animated explanation of the core of the Sun (University of South Wales).
- Animated explanation of the temperature and density of the core of the Sun (University of South Wales).