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See for example this table which contains the excess energy for each nuclide. You can take this table to compute the number you are interested in. The answer depends not only on the atomic number, but on the number of neutrons as well. This is why you need to think about how you want to represent this. I recommend you study that table and then figure out ...

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The sun's core has a density of of 150 g/cm³ (150 times the density of liquid water) at the center, and a temperature of close to 15,700,000 kelvin, or about 15,700,000 degrees Celsius; 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, at a pressure estimated at 265 billion bar (26.5 ...

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You should just think of Deuterium burning as a short-lived counterpart of main sequence hydrogen burning. As the pre-main-sequence star (PMS star, or protostar if you like) contracts, its core reaches around $6\times 10^{5}$ K and D burning is smoothly initiated. The star is then held at roughly constant luminosity and radius, because if it contracted, the ...

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