Listing the statements I kind of understand:
1)
The higher temperatures (for DT fuel, my note) are needed to counter the lower pressure in the reactor, with a higher required power density [mfb], 3 (power density, not understood)
Relevant pressure is plasma pressure (p=nkT) and not gravitational pressure so this part I understand.
Plasma pressure has the unit J/m
3 and thus N/m
2 so yes, it may be called pressure.
J/m
3 may also be written Ws/m
3 which may be interprated as power times time devided by m
3.
Looking at a single second this leads to W/m
3 which may be interprated as "power density".
But it tells me nothing
2) Because the power output of a single cubic meter of solar core material (i.e. ordinary hydrogen, proton-proton fusion) is roughly on par with a toaster oven [mheslep], 1 (is it really that bad?)
With regard to the huge size of the Sun I kind of understand this.
3) Pressure is limited by the magnetic fields (in a Tokamak, my note)-
a higher temperature does not allow to increase pressure, so the volume density will go down. As the interaction probability rises quickly with temperature, this still leads to a higher fusion rate [mfb], 1 (why not higher pressure? And fusion rate, how is that defined?)
Why?
4) The sun, including the core, is electrically neutral. Both ions and electrons exist under very height pressures at the core.[Drakkith], 4 (electrically neutral sounds convenient, though)
Roger that.
7) Also remember that the Sun has electrons and is not charged overall. The atoms in the gas cloud that initially collapsed to form the Sun didn't repel each other because they were not ionized.[Drakkith], 4 (the post Big Bang soup should have been be more elementary, I believe)
Roger that.
8) By the time you need to worry about proton repulsion (in the Sun, my note), you already have the 250 billion kg/cm^2 pressure of neutral matter above to overcome it.[PAllen], 3 (why suddenly not neutral? What happens under high pressure?)
This sounds reasonable.
9) Correct in that the starting point (for the Sun, my note) is Hydrogen gas. However, the fusion reaction is not to Helium 2, which would not release energy. It is to Deuterium when the proton-proton interaction is accompanied by emission of a positron and a neutrino. This process releases energy but is very rare.[PAllen], 1 (but very interesting).
So p + p somehow yields "p + n" (+ positron + neutrino)?
Recalling what you so kindly have said before, a neutron may decay to a proton but a proton, being slightly lighter, may not unless accompanied by some energy, right?
So first we have p + energy -> neutron + neutrino + positron
Then we have p + p -> D + positron + neutrino.
As I've said before, this is very interesting and I must study this further.
12) as it (the neutral Hydrogen, my note) collpased and heated (you can think of this simply as conversion of gravitational potential energy to heat), the center became ionized, but still neutral on average. You than have a neutral plasma at high temperature and pressure (= high density), such that the rare p + p -> deuterium + neutrino + positron can occur (at a low rate per volume). [PAllen], 2 (why ionized?)
Already acknowledged.
13) p + p -> deuterium + neutrino + positron [PAllen], 0 (but extremely interesting)
Already acknowledged.
14) The g (in a .1 lightyears wide cube of Hydrogen, my note) is varying during the collapse, but it should be easy to imagine that you have an enormous amount of energy per unit compressed volume of hydrogen. [PAllen], 2 (no, it's not easy)
If energy is kT and could be related to gravitational pressure (and thus density increasement) pressure is indeed high.
Looking at pressure as J/m
3 I now finally understand what you mean!
Pressure
is simply "Energy per Volume"!
But it is still an enigma how T is changed.
15) Normally, a neutron decays via weak interaction (in about 10 minutes if outside of a nucleus) into proton, an electron, and an anti-neutrino [PAllen], 0 (but extremely interesting)
This I would very much like to understand!
Repeating for convenience: p + energy->neutron + positron + neutrino
16) Since a proton is slightly lighter than a neutron, it does not decay (by any standard model processes). However, a proton plus energy, can, with low probability, undergo the 'decay' p -> neutron + neutrino + positron, mediated by the same weak interaction [PAllen], 0 (but extremely interesting)
Already acknowledged.
17) In the core of the sun, where the high temperature give each proton plenty of KE, and the high density makes collisions likely, once in a blue moon this reaction occurs along with with a collision. When it does, the formation of deuterium releases net energy (not much, but enough to keep things going). [PAllen], 1
So p + p not only gives D + neutrino + positron
it also gives energy?
18) You are ignoring pressure, density, and temperature, and you are also ignoring the fact that the Sun is electrically neutral. [D H], 4 (electrically neutral sounds as convenient as the useful law of conservation of energy)
I now understand this.
19) While the gravitational force between two protons is exceedingly small, the mutual gravitational interaction amongst the ~10^57 protons and neutrons in the Sun is extremely large. This is what is responsible for the extremely high pressure at the center of the Sun [D H], 1 (what mutual gravitational interaction? And how can this give a high pressure?)
High density gives high pressure.
25) You need to think when you see a very large number such as 250 billion atmospheres. Think about what it means in terms of pressure and temperature [D H], 3 (still just a huge number )
Roger that.
28) Terrestrial fusion plasmas use d+t fusion, because it is easier, but has the disadvantage that most of the energy is released to the 14.1 MeV neutron, which means it has to slow down and be captured in some blanket, which is heated and the heat is then passed to a working fluid, which is then used in some thermodynamic [Astronuc], 3 (please explain "easier")
Still interested in why.
Roger
PS
The thoughts of building a Tokamak of my own has been renewed.
Today my colleague (holding a Master's degree in Physics while being a technical oracle) explained to me how a luminance tube (LT) works.
He told me that the LT has a lightly pressurized Mercury vapor inside. And wrote the actual electrical configuration of it all down on an paper sheet in about two minutes.
It obviously consists of two heaters/filaments at either end, an inductor in series with the AC and a glimm lighter that is shorted at power up but releases after a short while which makes the inductor spike the voltage so high that the Mercury vapor ignites. This in turn makes the luminant coating of the inside of the tube shine, which is what we see.
Obviously still not understanding Saha and thus what a plasma really is, I would insist on calling this a plasma.
This is because we here have both "free" electrons and Mercury ions, right?
In my stupid electron "plasma" we did however not have any ions, only Nitrogen and Oxygen atoms.
So I am rethinking like this:
Let's build a
proton cannon (or perhaps more generally, an ion cannon).
Let's build it like a CRT, accelerating the ions with a high voltage.
The velocity of the ions may then be determined by:
\frac{mv^2}{2}=qU
Considerations:
1) I wish to chose the gas
2) Hydrogen is dangerous
3) A pressurized cannister of Hydrogen might be heated by a Bunsen burner for even more ions
4) The system needs to have several valves
5) Gas diffusable membranes might be used to confine the gas/ions to be accelerated.
6) Evacuating the tube would give a negative pressure, sucking the gas thru the membrane.
7) Turning on the toroidal B.
8) Opening the main valve and turning on the ion cannon.
9) Turning on Ohmic heating (i.e running electrons thru the ions/plasma)
10) Adjusting B and watching the plasma glow more and more (or even change color)
The main interest with this is to be able to see the color of the plasma change somewhat with regard to me changing B and the Ohmic heating and thus the temperature of the plasma.
This is my number one joy with this project.
Now, what gas should I use?
I have obviously thougt of Hydrogen but it sounds dangerous to say the least and it really is not that important to mimmic a fusion reactor that closely.
So I'm thinking of other gases. Pure Nitrogen, perhaps.
I don't think Nitrogen ions are that dangerous. And Nitrogen obviously gives nice colors (Aurora).
So perhaps I should try to get me some pressurized Nitrogen in a cannister. Should not be that difficult because both racing cars and hospitals use it(?)
Ionizing the Nitrogen could perhaps be done by heating it up with a Bunsen burner.
The question is how much I have to heat it up to be able to inject ions into my tube Tokamak.
Considering the Saha equation, it strikes me that the high pressure (and thus density) itself makes ions being available without heating it up.
But this depends on how much it is actually pressurized.
But really, going from 10^{-122} to some 10^{-10} is a huge step. To say the least
