Question

The chart above shows the relative abundances of the elements in the solar system. We know that the elements were formed by nuclear reactions within stars. The elements hydrogen to iron were formed by nuclear fusion, while elements larger than iron were most likely formed by nuclear fission. A trend can be found on the graph, with a few exceptions, showing that elements with an even atomic number tend to be more abundant than elements with an odd atomic number. What is the most viable reason for explaining why this phenomenon exists? A) It is just coincidental that the even atomic numbers are more abundant than the odd atomic numbers, therefore, no logical reason exists. B) An even atomic number gives an element more stability due to the equal pairing of protons inside the nucleus resulting in somewhat of an equilibrium to the nuclear forces. C)Nuclear fission results in most of the element formations, and during this process, only elements with an even atomic number can be formed due the equal splitting of the nucleus by the neutron collision D)The element with the greatest abundances were formed by way of nuclear fusion, and the energy release from the nuclear fusion of two elements will cause an equal distribution of nucleons to balance the nuclear forces Inside the nuclei

Answer 1

Elements with even atomic numbers are more abundant due to the process of nucleosynthesis in stars, where tightly bound nuclei with even numbers of protons and neutrons form more readily. Heavier elements beyond iron are created in supernova explosions through rapid neutron capture.

Step-by-step explanation:

The phenomenon in which elements with an even atomic number tend to be more abundant than those with an odd atomic number can be explained by the process of nucleosynthesis in stars. During nuclear fusion, which predominates in stars and creates elements up to iron, there is a preference for the formation of nuclides with even numbers of protons and neutrons because these combinations form more tightly bound nuclei.

Nuclides with even numbers of protons Z and neutrons N, especially when Z = N, are exceptionally tightly bound, yielding more stable configurations that are likely to form during stellar nucleosynthesis. Since elements heavier than iron cannot be formed by fusion due to their endothermic nature, they are typically synthesized in the supernova explosions of massive stars where additional neutrons are available and rapid neutron capture r-process can occur, leading to the formation of even heavier elements.