Nucleosynthesis is the process by which

It came from Energy. To do that we need carbon and oxygen and nitrogen and silicon and chlorine and every other naturally occurring element. Nuclear species can be transformed into other nuclear species by reactions that add or remove protons or neutrons or both.

Because technetium is radioactive, with halflife much less than the age of the star, its abundance must reflect its creation within that star during its lifetime. The four major types of nucleosynthesis Big Bang nucleosynthesis Big Bang nucleosynthesis occurred within the first three minutes of the universe and is responsible for much of the abundance ratios of 1H protium2H deuterium3He helium-3and 4He helium-4in the universe.

In a way, this means that the energy present in a system is spread out among particles in such a way that the population of molecules at different energies doesn't change, even though the molecules themselves are constantly changing energy levels. Less dramatic, but equally convincing evidence is of large overabundances of specific stable elements in a stellar atmosphere.

The 10 Lagrangian points on the 3p subshell, are formed with six harmonically manifested Lagrangian points from the 3p subshell, which are labeled as 3d-8 L13d-3 L23d-6 L43d L53d-1 L43d-5 L5and two pairs of two L4 and L5 Lagrangian points of 3dL1 and 3d3-L2 manifested on the 3d subshell, which are labeled as 3d-7 L43d-9 L53d-2 L4and 3d-4 L5.

The problem that we run into is that with Atoms that are lighter weight than Iron. The outer major planets Saturn, Uranus, and Neptune, can be perceived as the nested positrons coalesced spheroidal bodies of stellar materials formed with the cyclonic spinor field of the L1 Lagrangian points within the outer shell walls of the L, M, and N shells respectively.

These include 44Ti48Cr52Feand 56Niall of which decay after the explosion to create abundant stable isobars at each atomic weight. So, then the most common Element in the entire Universe is Hydrogen.

This started to tip the balance in favor of the proton-forming reactions. This only happens with binary systems. Every now and then a Proton is being squished together with an Electron to create a Neutron. By the time the universe was three minutes old the process had basically stopped and the relative abundances of the elements was fixed at ratios that didn't change for a very long time: In the cores of lower-mass main-sequence stars such as the Sunthe dominant energy production process is the proton—proton chain reaction.

This is where the Weak Force gets involved and switches the identity of a Neutron into a Proton while emitting bits of other stuff like an Electron and the anti-Electron Neutrino.

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In order to form atomic nuclei, the nucleons the scientific word for protons and neutrons must be able to collide and stick together. This was a result of the high energy density. Reaction rate[ edit ] The reaction rate per volume between species A and B, having number densities nA,B is given by: When nucleosynthesis began, all the neutrons present were incorporated into He nuclei.

To do that you need stars, which means waiting around for at least billion years. It is apparent with the UVS atomic model that as a result of the 2nd sphere and the 3rd sphere are rendering four additional Lagrangian points outwardly to the next outermost subshell of an electron shell, which are rendered by the two pairs of L4 and L5 Lagrangian points manifested with the two primary L1 and L2 Lagrangian points, or with its harmonics resonated in the outer electron shells.

Isotope abundances are typically calculated by calculating the transition rates between isotopes in a network.

As illustrated in the diagram of the UVS atomic model, it is perceivable that the two primary L1 and L2 Lagrangian points spawned in the 1s subshell, are resonated as harmonics at the L1 and L2 angular phases in all the outer subshells.

Category:Nucleosynthesis

The nice thing about Deuterium is when it collides with another Hydrogen you start to get Helium. In this case you take two Hydrogen Atoms, squish them together and you get what is called the Deuterium. The pretty pair will be on display from twilight until Jup You take a Star like the Sun and initially it will just burn through all the Hydrogen-producing Helium.

The abundance ratio was about seven protons for every neutron. Before one neutron half-life passed nearly every neutron had paired up with a proton, and nearly every one of these pairs had paired up to form helium. So, then what happened? As a result, the core region becomes a convection zonewhich stirs the hydrogen fusion region and keeps it well mixed with the surrounding proton-rich region.

The successive nuclear fusion processes which occur inside stars are known as hydrogen burning via the proton-proton chain or the CNO cyclehelium burningcarbon burningneon burningoxygen burning and silicon burning.

Explosive nucleosynthesis occurs too rapidly for radioactive decay to increase the number of neutrons, so that many abundant isotopes having equal even numbers of protons and neutrons are synthesized. Then the Oxygen probably came from a Star bigger than our Sun. The matter present was in the form of electrons, positrons, and a very small concentration of protons and neutrons about 1 part per billion.

They were continually changing back and forth by means of the following two reactions: Heavier elements can be assembled within stars by a neutron capture process known as the s process or in explosive environments, such as supernova e, by a number of processes.

How is it that other Stars keep going?

Big Bang Nucleosynthesis

The difference in energy production of this cycle, compared to the proton—proton chain reaction, is accounted for by the energy lost through neutrino emission.the name r-process nucleosynthesis, have remained obscure.

Initial efforts focused on supernovae being the best possible candidates then known for the production of the large neutron fluxes necessary for the r-process to occur, but most mod-ern work has found that the conditions in numerical simula.

Nucleosynthesis and the Origin of the Elements Stellar Nucleosynthesis - The Origin of the Elements Name of Process Fuel Products Temperature (K) Lifetime Remaining 1.

H-burning H 6He 60 x 10 10, years 2.

Nucleosynthesis

The theory of this building of elements is called nucleosynthesis. For the successful computer modeling of any kind of star, a library of nuclear physics information is needed. Such a library contains all of the nuclear processes that may occur in the hot and dense stellar plasma: nuclear reactions, beta-decays, photodisintegrations, and so on.

Stellar nucleosynthesis is the collective term for the nucleosynthesis, or nuclear reactions, taking place in stars to build the nuclei of the elements heavier than hydrogen. Some small quantity of these reactions also occur on the stellar surface under various circumstances.

Almost all of the hydrogen and helium in the cosmos, along with some of the lithium, was created in the first three minutes after the Big Bang.

Two more light ele-ments, beryllium and boron, are synthesized in. Nov 18,  · Supernova nucleosynthesis is a theory of the nucleosynthesis of the natural abundances of the chemical elements in supernova explosions, advanced as the nucleosynthesis of elements from carbon to.

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Nucleosynthesis is the process by which
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