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Line 22e6 Carbon Fusion Cycle Helium Nucleus Nitrogen 15 UFO 5g WOW SETI

July 23, 2012

Line 22e6 Carbon Fusion Cycle Helium Nucleus Nitrogen 15 UFO 5g WOW SETI

5g force ufo engine acceleration plasma formulas

part 247 of 100 videos there are more videos after this one i’ll post all then update the #.
Math Equation Wow Seti 1977 radio signal alien

Wow SETI 1977 radio signal alien

11/111/1/1/14=0.0071

Google 0.0071

Google 11 111 1 1 14

research notes quotes links

13 June 2012 12 22 am edt]

Comments on video:

Line 18a4e Helium 3 Alpha Particle Decay Tritium U238 PU239 Nuclear Fusion Engine 5g WOW SETI

http://www.youtube.com/all_comments?v=WfDot7VEV6o>

Comment received about carbon nitrogen 15 fusion

I’ve googled it to see what comes up.

carbon fusion cycle diagram

 The main theme of the carbon cycle is the adding of protons, but after a carbon-12 nucleus fuses with a proton to form nitrogen-13, one of the protons decays with the emission of a positron and a neutrino to form carbon -13.

Two more proton captures produce nitrogen-14 and then oxygen-15. Another neutron decay leaves nitrogen-15.

Another proton capture produces oxygen-16 which emits an energetic alpha particle to return to carbon-12 to repeat the cycle. This last reaction is the main source of energy in the cycle for the fueling of the star.

While this process is not a significant part of the sun’s fuel cycle, a star like Sirius with somewhat more than twice the mass of the sun derives almost all of its power from the carbon cycle. The carbon cycle yields 26.72 MeV per helium nucleus.

http://hyperphysics.phy-astr.gsu.edu/hbase/astro/carbcyc.html

13 June 2012 12 24 am edt

My thoughts

Formula idea from data

Carbon + cycle + protons + carbon-12 + nucleus +fuses+ nitrogen -13 + proton decay + emission + positron + neutrino + forms carbon -13 + 2 proton captures + nitrogen -14 + oxygen -15 + neutron decay + nitrogen -15 + proton capture + oxygen -16 + emits + energetic + alpha particle + return+ carbon -12 + repeat cycle + last reaction + source +
energy + fuel + star power + carbon cycle + 26.72 MeV per helium nucleus

Google
helium nucleus nitrogen 15

1. Atoms – the inside story. Isotopes and decay.
resources.schoolscience.co.uk/stfc/16plus/partich2pg1.html
The nucleus of an atom contains protons and neutrons and it accounts for nearly all … Some nitrogen atoms have 15nucleons in the nucleus and therefore have an atomic … We now know that the nucleus of helium is 1.9 x 10–15 m across.
2. CNO cycle (nuclear fusion) — Britannica Online Encyclopedia
http://www.britannica.com/EBchecked/topic/94896/CNO-cycle
Eventually, the nitrogen-15 nucleus captures a fast-moving proton and breaks down into a carbon-12 nucleus plus ahelium nucleus (alpha particle) of mass 4 …

https://www.google.ca/webhp?sourceid=chrome-instant&ie=UTF-8&ion=1#hl=en&sclient=psy-ab&q=helium+nucleus+nitrogen+15&oq=helium+nucleus+nitrogen+15&aq=f&aqi=&aql=&gs_l=hp.3…50.5076.0.5497.13.13.0.0.0.0.196.1397.7j6.13.0…0.0.SEd-vpbf984&pbx=1&bav=on.2,or.r_gc.r_pw.r_cp.r_qf.,cf.osb&fp=d435548b4fe14b69&ion=1&biw=1600&bih=732>

Quotes

Stellar Processes and Evolution

Nucleosynthesis

Nuclear fusion, where nuclei combine to make a nucleus with a larger number of protons and neutrons, occurs in main sequence stars once they reach a critical temperature.

As the core temperature rises, due to ongoing core contractions and resulting increase in pressure, the atomic nuclei move faster thereby increasing the probability of two nuclei colliding with each other and fusing into heavier elements.

Proton-Proton Chain

The simplest reaction that occurs in stars is the conversion of hydrogen into helium – a process known as the proton-proton chain and requires a core temperature of at least 10 million K. In this process six hydrogen atoms are needed to create one helium nucleus of two protons and two neutrons.

Process Result Extras
1 proton + proton deuterium positron, neutrino
2 proton + deuterium helium-3 gamma-ray
3 helium-3 + helium-3 helium-4 2 protons

Table 5.1: Proton-Proton Chain Reactions
In Step 1 two protons come together to form deuterium (a nucleus of one proton and one neutron).  This interaction also involves the liberation of a positron (a positively charged electron) and a neutrino.  This process occurs 1038 times per second in the Sun.
In Step 2 the resulting deuterium nucleus combines with a proton to make the rare isotope helium-3 consisiting of one neutron and two protons.  This reaction also produces a gamma-ray.

In Step 3 the helium-3 nucleus becomes a helium-4 nucleus by the addition of a neutron.  This step can occur in several ways, but the combination of two helium-3 nuclei is the most common way.
Steps 1 and 2 must occur twice before step 3 can occur.  Six protons go into the cycle, but two come back out.  The overall process results in 4 protons (hydrogen nuclei) becoming a helium-4 nucleus, two positrons, two neutrinos and two gamma-rays.

CNO Cycle
In more massive stars (at least 4 solar masses) the Carbon-Nitrogen-Oxygen cycle dominates as the main process for proton burning proton.  The heavier elements are already present in the star, therefore largely restriciting this process to younger Population I stars.
The CNO cycle occurs only in more massive stars due to the necessity of a convective core with a temperature of at least 20 million K. In the process a 12C nucleus and four protons combine in various stages ultimately resulting in the creation of another 12C nucleus, a helium nucleus and the liberation of a significant amount of energy. The carbon is acting as a catalyst in the process of converting hydrogen into helium. There is no net creation of the heavier elements through this process.

Figure 5.2: CNO Cycle

Process Result Extras
1 carbon-12 + proton nitrogen-13 gamma-ray
2 nitrogen-13 decay carbon-13 neutrino, positron
3 carbon-13 + proton nitrogen-14 gamma-ray
4 nitrogen-14 + proton oxygen-15 gamma-ray
5 oxygen-15 decay nitrogen-15 neutrino, positron
6 nitrogen-15 + proton carbon-12 helium nucleus
Table 5.2: CNO Cycle Reactions
The Future?
Once the stellar core has used up the majority of its hydrogen source the core region is dominated by helium. The future evolution of the star now depends very firmly on its mass and whether there is sufficient gravitational pressure to induce helium burning and the burning of successively heavier elements.

http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=36828&fbodylongid=1736>

gamma ray electron neutrino positron neutron proton total reaction diagram

In more massive stars (at least 4 solar masses) the Carbon-Nitrogen-Oxygen cycle

13 June 2012

Based on the keywords from the data

Formula ideas:

Nucleus + atom + protons + neutrons + nitrogen atoms + nucleus helium + nucleus captures fast moving proton + breaks down + carbon -12 + helium nucleus + alpha particle + mass 4

Nuclear fusion + nuclei + large number + protons + neutrons + critical temperature

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