The same force also pulls the neutrons together, or neutrons and protons together because the nuclear force is stronger than the coulomb force for atomic nuclei smaller than iron and nickel, building up these nuclei from lighter nuclei by fusion releases the extra energy from the net attraction of these particles a substantial energy barrier. The reason for this is simple: there isn't enough energy for these nuclei to fuse together into heavier combinations, but there's too much energy for electrons to bind to them and form atoms. Production of neutrons can lead to s-process (neutron capture slower than beta decay) this produces primarily stable elements where the number of protons and neutrons are very similar. Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons the first nuclei were formed about three minutes after the big bang.
At early times, neutrons and protons (l) interconvert freely, owing to the energetic electrons, positrons, neutrinos and antineutrinos, and exist in equal numbers (top middle. Nuclei with the same number of protons but different numbers of neutrons are called isotopes only some combinations of protons and neutrons are stable nucleosynthesis is the process by which heavier elements are created. Big bang nucleosynthesis begins with the individual baryons—the protons and neutrons the neutrons are unstable as free particles, but due to the shortness of time during the nucleosynthesis era of the big bang, their abundance is only slightly reduced by this decay.
Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons the first nuclei were formed about three minutes after the big bang , through the process called big bang nucleosynthesis. The leftover matter is in the form of electrons, protons and neutrons as the temperature continues to drop, protons and neutrons can undergo fusion to form heavier atomic nuclei this process is called nucleosynthesis. Nucleosynthesis, production on a cosmic scale of all the species of chemical elements from perhaps one or two simple types of atomic nuclei, a process that entails large-scale nuclear reactions including those in progress in the sun and other stars chemical elements differ from one another on the basis of the number of protons (fundamental. Neutrons and z gives the number of protons bound in the nucleus as heavier nuclei just exist in the outer shells around as heavier nuclei just exist in the outer shells around the neutron stars these interactions can happen there.
Nucleosynthesis or nucleogenesis, in astronomy, production of all the chemical elements  from the simplest element, hydrogen, by thermonuclear reactions within stars, supernovas, and in the big bang at the beginning of the universe (see nucleus  nuclear energy . Nucleosynthesis in the early universe the term nucleosynthesis refers to the formation of heavy elements, atomic nuclei with many protons and neutrons, from the collision of light elements the big bang theory predicts that the early universe was a very hot place. Along with protons, neutrons form the nuclei of atoms neutron capture the primary mechanism by which very massive nuclei are formed in the violent aftermath of a supernova instead of fusion of like nuclei, heavy elements are created by the addition of more and more neutrons to existing nuclei. Terms nuclear fusiona reaction in which two or more atomic nuclei collide at very high speed and join to form a new type of atomic nucleus nuclear forcethe force that acts between nucleons and binds protons and neutrons into atomic nuclei the residual strong force. At this time there were about six protons for every neutron, but a small fraction of the neutrons decay before fusing in the next few hundred seconds, so at the end of nucleosynthesis there are about seven protons to every neutron, and almost all the neutrons are in helium-4 nuclei.
In physical cosmology, big bang nucleosynthesis (abbreviated bbn, free neutrons are less stable than helium nuclei, and the protons and neutrons have a strong tendency to form helium-4 however, forming helium-4 requires the intermediate step of forming deuterium. Evolution and nucleosynthesis calculation of gamow peak assumes that the process is far from a resonances since any reaction branch that completes this must turn 2 protons in 2 neutrons, two neutrinos are also emitted, which carry energy away from the reaction site interaction between nuclei and free neutrons (neutron capture) – the. The period of baryionic matter formation: protons, neutrons and some of the lighter elements – the epoch of big bang nucleosynthesis – lasted from 10 seconds to about 20 minutes from the beginning itself. Deuterons are the nuclei of deuterium and are made when protons and neutrons fuse and emit photons deuterons and neutrons can fuse to create a tritium nucleus with one proton and two neutrons.
After two minutes, deuterium formed by the fusion of protons and neutrons after three minutes, helium formed by the fusion of deuterium, protons, and neutrons (1) during the first four seconds of the universe, matter formed by pair production. In order to form atomic nuclei, the nucleons (the scientific word for protons and neutrons) must be able to collide and stick together in the early universe the key reaction was the collision of a proton and a neutron to form a deuterium nucleus (an isotope of hydrogen. By the end of big bang nucleosynthesis, essentially all neutrons available end up in helium nuclei (with traces of deuterons and lithium nuclei) and thus the h/he ratio ends up at 12 protons for every he nucleus (2 protons, 2 neutrons. More neutrons are needed as atomic number increases in order to keep the balance, and neutron-proton ratio can reach 15:1 for largest atoms, have more neutrons than protons band of stability the area on a proton (x)-neutron(y) graph within which all stable nuclei are found.