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The Solar Neutrino Problem

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The Solar Neutrino Problem
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In his first three neutrino lectures at the Lindau Meetings, Rudolf Mößbauer described his experimental project to detect a possible non-zero neutrino mass through the observation of neutrino oscillations. As a source for neutrinos, he used nuclear fission reactors in France and Switzerland. At the time of the present lecture, these experiments were finsihed and Mößbauers interest had moved to using a much larger source of neutrinos, the sun. In the first part of the lecture, which gives the background to his involvement in a new experimental collaboration, Mößbauer describes what is called the standard solar model and how the neutrinos are created in nuclear fusion reactions in the interior of the sun. He also gives a very nice short history of the concept of neutrino particles, which derives from Wolfgang Pauli’s attempts to understand the continous energy spectrum of electrons emitted in radioactive decay and in which, among others, Lise Meitner was involved. Mößbauer also puts forward the hypothesis that the universe is filled with very low energy neutrinos, much like the cosmic background radiation discovered by Arno Penziaz and Robert Wilson. Since the detection of very low energy neutrinos is extremely difficult, he tells his audience of students and young researchers that finding a method to detect a cosmic neutrino background surely would lead to a Nobel Prize. As far as I know, this background radiation has so far (2012) not been detected, so there is still lots to do! Mößbauer then describes the so-called solar neutrino puzzle, by which was meant the fact that only one third of the expected neutrinos from the sun were ever detected during many years of experiments in the Homestake mine in the US. Finally, he describes a new project which would complement the Homestake measurements by looking for neutrinos of a lower energy. This new project, planned to start taking data in the beginning of the 1990’s, had been given the name GALLEX and was to be constructed in the Gran Sasso tunnel north of Rome. Mößbauer gives an inspired account of the problems in starting this new project, acquiring funding of about 20 million US dollars (too much for the low-energy committees, too little for the high-energy committees!), and buying about 100 tons of gallium chloride. In this amount of gallium chloride, about one gallium atom per day would be hit by a solar neutrino and thus transmuted into a radioactive germanium atom. Since the radioactive germanium atom would have a half-life of about 10 days, the 100 ton detector fluid would have to be washed trough every fortnight in order to find the radioactivity! Mößbauer shows pictures of the laboratory and the planned experiment and also explains what information could be gained from the measurements. Having listened to several lectures by Mößbauer, both recorded and in real life, I have seldom heard him be so enthusiastic! Anders Bárány
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Transcript: English(auto-generated)
Ladies and Gentlemen, our good old son and the most objective of your life is physical.
Our good old son stayed normal in his home and the rest of his life changed. In the last few days, in the media, we have seen that his son is a protoboransian, and that he also works in communication.
But that is not good. Today we will see that his son is a protoboransian. Then we will see that his son is a protoboransian. I must say that today his son is a protoboransian, and not only that, but the overflow of his son. We have seen that. We have seen that his life is different,
we have seen that his energy is different, the luminosity of his son is very small. But this is not what I am saying, because the son that he made is very small. It took hundreds of thousands of years to make his own son, and the overflow of his son is very small.
I must say that today, not only that overflow of his son, but the overflow of his inner son. And the overflow of his son is relatively small. We have seen that today, we have seen that today his son is the standard son model, but we have seen that he is relatively small.
What do we mean by that? We have two experimental models, one of which is called the Androsian Elta, one of which is called the Heliosysmography, and the last one is called Doppler Effect,
and it is a local model, the son of the son is very small. The Doppler Effect, the biolum and the chemical, are very similar. We saw the Doppler Effect as a function, when it is in the air and in the air, that is what I demonstrated. I showed you a sequence,
and you can see that the chemical and the biolum are similar. You can see that when you start with an auto, the road is very small, and the policy is very small, then the policy is clear, and you can see that, for example, your car is very small. You can see that in Germany,
we don't have very small cars. In America, people in the region are very small, they have very small cars, they have very small cars, and when they are very small, they have very small cars. You can see that in Germany, the car is very small. So, I don't want to say that you are not saying that
you are not saying that you are not saying that the interpretation of this state is very small, and a large amount of this state exists. I think that was said about the reaction that the son of the son has made, and about the future process that the state has made.
The son is the only son that, from the younger generation, the son of the son has made, is that we have to experiment with him. We have to work with him, to understand what the inner son is doing. This is the prototype of a son,
and all that we have to understand is that, with the car's reaction, with the production of the son, we have to understand that all that can be experimented with in our son's test. And therefore, I think that was said. So, the medium with which we are testing is that we have to understand the inner son of the son,
and that it is a fertile son, and that the son's brain can still function. We have to understand the inner son of the son of the son, who is the son of the son, and who is the son of the son of the son. The son of the son of the son
is what is known as the first experimental experimental study. It is quite simple, but today we are talking about the relative values of this study. In the case of the son, the experiment is not too interesting, and it is what the inner son is doing,
and it is also what the new son is doing. When I talk about the new son, it is interesting to understand that it is the first experimental study of the new son. I don't mean gravitation, there are a lot of changes. I mean the electron magnetization of the new son, and the new son.
These are the changes of the study. And yet, no one knows that the new son is not an experimental study. You can see here, the new son, the new son of the son, in a culture study, and that was a big change from the family labs, which was also made. I read here about the relative values of the new son,
MFAO, or the typical physical energy. These are the changes of the new son. I can also explain to you that there are a lot of changes in the study. For example, the new son, the electron magnetization of the new son, can also be used as an electron magnetization of the new son.
When these changes of the new son, the new son,
can also be used as an electron magnetization of the new son, which comes up in the study of MFAO and again,
and also tells us what the new son's impact is. I was just saying that in the new son, the new son, is a very important part of the study. And I also wanted to say that these new son may be a bit more important in the early 1990s and early 2000s. And I don't know if this is the early 1990s. And still, this small,
micro planet can be as big a part of the study as the new son, the new son, which comes up in the study of the new son when he comes up in the study and also tells us that the son's impact on the new son is very important in the study of the new son. So, we came up with a new study with the restoration of the experiment with which
the detector of a cubic meter of voluminous light can be used to measure the impact of the new son. You can see that the new son is a very important part in the study of the new son,
and the new son can be used the impact of the new son on the new son. So, we came up with when we did the experiment the experiment was to the impact of the new son on the new son. And we practiced two different types of changes in the study of the new son
so that the new son can be used and the son can be used for the son. Thank you. In the study of we have this situation that we can do in two to three to four to three to three to three to four of this unalienable thing. They were able to speak in their own reactor and make them
the same. They can see neutrons in the same way and make them speak in a similar way. They have so many neutrons and they must be able to speak in a different way. And this is a better example. The neutrons are in protons, in electrons, and in electrons
an anti-neutrinos, that's why I call them anti-neutrinos. An analog beta-cervals process is in the sun, so it's important that you don't use protons, you use neutrons, positrons, and electron neutrons. This way, when you're in the sun, a fusion process is made,
so that you can use four protons, one in helium, four at the same time. That's the last thing, that's what's in the sun, which you'll find out later. That's why, when I use four protons, one in helium, four at the same time, two protons and two neutrons, it's important that you use two protons and two neutrons
in order to make a decent process. Then, the reactant produced electrons, anti-neutrinos, in large quantities, because there were a lot of reactions, and the sun made a lot of neutrinos, because there were a lot of processes, and in the sun, it's a lot bigger.
This is the reaction here, that we've already demonstrated. We've already demonstrated a lot with this thing, and we'll show you how it works here. Experimented here, and this is the whole process. We'll show you the theory of Bethe, Weizsäcker, and so on. However, you can see that this experiment is very difficult.
This neutrino is also involved in this experiment, and you can see the next step, where the process is completely completed. This is where the situation is going. We don't need the neutrinos for gas, you can see that the Bethe is involved in this experiment, so you can see how it works here. This is Chika Nöss,
from the nature of this experiment. You can see that Chika Nöss is not involved in this experiment, so you can see how it works, and it's very important that you use two neutrinos. I can hear the next song, and you can see that this experiment is very important, and in the end, Pauli has a very strong voice.
So now you can see that in the end, this is a very difficult process, this is over, and this is very difficult. When it's over, you must have the world-definite energy, which is very important, the kinetic energy for all of us, so that we can manifest that this experiment is also a world-definite energy,
as a monochromatic line. You can see it here. This is why you don't see in the 20 years that the beta spectrum is a continuous spectrum. As Pauli said earlier, when the energy is already under the interface, you must know what's going to happen. And what's going to happen is that
the photons are going to be released. So you can see that this is a three-circles file, and not a two-circles file, this beta process, is going to be a three-circles file and a three-circles file and a three-circles file. Many people have been saying that this is a three-circles file, and it's not a one-circles file.
And Wolfgang Pauli, who was a theoretical physicist, was the only scientific experiment in the 20th century. As I said earlier, this is a very difficult process, and Wolfgang Pauli is a very new person, and he's a great scientist. So, let me tell you what it is that
the experimental physicists don't know. What is so difficult to understand is that it's very difficult to understand. And so comes the difficult to understand in the physical world. And this is what we today call neutrinos. You see, that's when neutrons and neutrons were not detected, and so on and so forth.
All of this is difficult. So why are neutrinos so difficult for us? Why are they not so difficult for us? This is difficult for us because this process is the swag-waxed-werkung. If we don't understand this, then we can't understand the electromagnetic or the state-waxed-werkung process. But this is a process of swag-waxed-werkung.
The waste is not long. I've already told you what swag-waxed-werkung is. And waste is not long. The waste is a very difficult process to understand in our lives. We cannot understand the state-waxed-werkung process.
It's a very difficult process. But it is difficult to understand the state-waxed-werkung process in a very long time. I'd like to remind you that we in the cosmos have the opportunity to understand the state-waxed-werkung process. I'd like to remind you that in the last year, a supernova explosion happened, and so a big explosion happened.
So a big explosion happened. And if we understand the state-waxed-werkung process in a very long time, the state-waxed-werkung process is not long. The fact that our planet has been living for four and a half years and has been living for so long means that we are able to understand the state-waxed-werkung process,
the state-waxed-werkung process, the state-waxed-werkung process, the existence of these new things. This is a very difficult process. It's not a gigantic thing, but it's a very difficult one. So that's why we are able to understand the state-waxed-werkung process. This is a very difficult one. I'd like to remind you that the sun is shining.
And here we see this proton-proton fusion. I'd like to remind you that this proton-proton fusion is not only the reaction of the meteorites but also the reaction of the waves and the nuclear bombs. It's not just the sun. It's also the spring. What we can do next.
We are able to understand this process the same as the sun for the energy upgrade. We are able to understand the state-waxed-werkung process, the control of the fusion, the control of the proton, the helium in the spring. We are able to understand the energy that our planet is living for.
The energy is lost, but it is not. We are able to understand the state-waxed-werkung process. We are able to understand the state-waxed-werkung process. What we are able to understand in the next 10 years. Then we are able to understand the energy that our planet is living for. This practice of energy is a long and long way to go.
In the sun it was also known that it was 4,5 million years ago that a sun-stance was created and the temperature was reduced and the radius was reduced. So 4,5 million years ago the sun-stance was a constant constant
and it was also known for a long time. What is happening now is that there is a lot of stuff here in the road. In Germany, you can see the site of the sun. The helium is still there. The planet is here in Germany. This is the inner sun. The inner sun is right here. In Germany, there is a lot of helium here in the sun.
The sun is still there. There is a lot of stuff here in the road. But there is also a lot of stuff there. We don't know much about that. We are able to understand the sun and see how it works. Then we are able to understand what is the new spectrum.
The sun is still here. And we are able to understand the sun. We can see the sun. Then we can see the sun. Then we can see the energy that is emitted by the sun. I don't think it is a practical thing here. The sun is here. We have seen a lot of things.
We saw a lot of things. The solar energy and also the energy that is emitted by the sun is the flux of the new energy that is produced by the centimeter-quadratic energy that is emitted by the sun. I would like to talk about the new spectrum 2. This is the new spectrum 3. This is the green spectrum
and this is the blue spectrum. The blue spectrum is the only important part of the process. The same logarithm is here. They are dominated by absolutely everything. Almost 80% of the energy is generated by the blue spectrum. But the green spectrum is also important. It is a very small
and uninteresting new process. However, this is something that is important for the experimental physics because it is the only source of energy that is emitted by the sun. It is not only the blue spectrum that is emitted by the sun. The green spectrum is here. The blue spectrum is the only source of energy that is emitted by the sun. And the whole energy is very small
because the reaction of the sun is very small and it is in the light of light that is emitted by the sun. The energy is very small and what is important is the work of the energy that is our whole aperture before the whole energy. It is important that we have the most energy. The reaction
that is generated by the sun is here plus plus plus plus plus plus plus plus
plus I am going to show you a close up of this. This is the result of a new 3N2 target,
which I have manifested in this detector. I have the reaction of the swelling word, the swelling word is used for this reaction, and we can see what happens when the swelling word is used in this green swig. The swelling word is used in this swelling word.
I am going to show you this experiment. I am going to show you an example here. This is the swelling word. I am going to show you the result of the swelling word. The swelling word is used in this red swig. This is Ray Davies, and he is in the home state of South Dakota. The reaction is here. I am going to show you that the detector is so big.
It is not interesting to say that this swelling word, the swelling word is used in this red swig. It is a swelling word,
and it is a very important model.
It is a relatively small parameter, and if you have a small drain in the parameter, then you get the whole sun independent. You don't have the radius, the temperature, and you know what the energy is. The standard sun model is shown to be a model of a lot of people. There are a lot of theoretical theories that I am going to talk about today,
and that is why the standard sun model is so important. However, it is not so much a theory, and it is not really that important. However, this factor 3 is the state of the sun quality. You can see that 10% of the sun is clear, but a factor 3 is not so important.
We don't have a whole lot of physics that you can talk about today. Therefore, the swelling word is, and this factor 3 is clear, that you can see that the standard sun model is not so important. The problem is that this green swig, this little green swig, is not so important.
It is not only because of the temperature in the inner sun, that you can see the potential of the sun, but also because it is not more important when the blue swig is not important. The blue swig is directly connected to the luminosity of the sun, which is important. That is why the blue swig is not important
and you cannot find the light spectrum, when the sun is important. If you cannot find the light spectrum, then you cannot find the sun. Then you must find the neutrinos, which are the waves of the sun, of the earth, of the inner sun, which are so far away, then you cannot find the light spectrum.
Therefore, you must find a chance, when you are actually finding the neutrinos, to learn something about the mass of the neutrinos, then you cannot find the mass of the neutrinos. We all know that the neutrinos are a mass. We cannot find them. We do not know that they are a mass,
but if we cannot find them, we must find a symmetry principle, what this mass represents. We can also find the photons, which are the waves of the sun, where the photon mass is null. We can also find symmetry principles, we must find the neutrinos, but no one has ever seen them, and it is a little unusual, this way, that the mass is null.
Therefore, the mass of the neutrinos is a mass. We cannot find the mass. Therefore, the theoretical theory of the electron neutrinos is given by the electron neutrinos by 100 electron volts and 100 grand volts by 10-6 electron volts, so that you can find the theoretical theory
of the neutrinos. However, it is so that you cannot find the mass which is only open or out of the spectrum, when the neutrinos are only null. With other words, one can predict that experimental physics can be found, which is not the mass of the neutrinos, and also that it is not fantastic, but it is a big thing when it is in stability.
Also, we have also, when we are in the blue, we must find a chance, one of the very features is that the standard sun model is right, or is that what is wrong? And that cannot be good, when the photon flux is right, and when we don't find the photon flux, then we must find the neutrinos. It is a lie.
Now, what is the problem? We must find the blue, because we can't find the mass and we cannot find a reaction which is also possible. We must find the reaction of gallium-1-6 plus sun-neutrino plus gallium-1-6 plus electron, and this reaction has a lot of nitrogen in it.
We have the electron here, and the same thing here, and the same thing here. and we have to find the reaction of the spectrum, when we are in this state. The other thing is that there is no long-term commitment. There have been attempts to indicate that this is the most stable substance, this substance is also only true. This was a surprise.
And in the past, for example, for 10 years, there was an American-German society, the German-German group of the Max Planck Institute of Physics in Heidelberg, of the German society and the Blue Cave National Laboratory of the German National Laboratory of the U.S. side. This is the second time we have done this experiment. It was a very important experiment in this decade.
However, the German society was in the last three decades trying to bring together almost 50,000 gallons of gas, which was in the space of about $20 million. The Americans were not able to come here. The fact is that $20 million was not only
a relative of $500 million. However, the third time is so important. There was a huge increase in comity. The third time is for the non-energy. This is too much, and for the whole energy, this is too much. And you have to remember the frustration. This is the second time we have done this. And we have done a study in Europe
about the scale of gas. And this is in the third time, in the third time. This is a European study. The European Galax Project, Galax for Gallium Experiment, and this is the same, but it is still in the middle of it. This is a large group, the Max Planck Institute for Cancer Physics in Heidelberg.
This group is the first time I have done this experiment. Then I took a look at this experiment, and this time I found the car in Karlsruhe, the group in Rehoboth, the Weizmann Institute in Israel, and then came here to the Brookhaven National Laboratory.
We were in Milan and then in Rome. And then the French group here in Grenoble, in Paris, and in NHTSA, they did the same experiment for Antwoord.
I thought that I wouldn't be able to see it. Then we did this Galax Experiment. The reaction is very similar. This is the same, but it is still in the middle of it. This is an experiment. The reaction is still in the middle. The reaction is still in the middle of it.
This reaction is still in the middle. We have a form of gallium chloride. We have a hole in the middle of it. The reaction is still in the middle of it. And the idea is that in this tank of gallium-3, we are going to move it. The neutrinos are going to move it. We have in this tank, in this substance here,
about 29.25 gallons of gallium. And this 29.25 gallons of gallium will take, when all is good, one ounce of water in one can of germanium-1.50. And the problem is that this 29.25 gallons of this one can be sufficient.
If the tank is sufficient, then I can move it to the other side and then I can move it to the other side and in this side I can move it to the other side and in this side I can move it to the other side. And this is a very important step that is why this process
of looking at the state of the atom is not only an absorption, it is a neutrino state of the atom. And the reason why this is germanium-1 is that this is a large target. You can see that for every large target, this is a small target, but it must be a relatively small target. And that is why this is a large target.
And the reason why this is a large target is that it must be a relatively small target. You can see that for every large target, it must be a proportionally large target. And why is it that you can't move one ounce of water in one can of germanium-1 and one ounce of water in two can of germanium-2? That is not the reason why this is a target. You can't do that with efficiency,
with work-time. It is 80 to 90 percent, and that is why this is a small target. The gallium chloride is the only way that it can be a neutrino absorption in germanium-1-6 chloride. You can see that this is about three, and this is four. This is four, and it is not the only way
in which it can be a relatively small target. But you can see that it is a germanium carrier in this substance, and it is possible that with gas or helium gas, it is possible. If you take gas from this gas with germanium chloride,
you must have it running, and that can cause a lot of damage. You must have it running, and that can cause a lot of damage. You must have a large target of germanium in the process, which is not possible at all. You can't do that. This is why it is here. And, of course, it is possible that germanium chloride
can be used in germanium. This substance is here, german, and we think it is very important that for all of these experiments, a French group of gallium-1-6 and a German group of germanium-1-6 are able to do this. This is a good example of this experiment. This experiment is done
with xenon in a cell that is also called a cell gas. And the cell gas that we saw, it has an active volume of about a half a centimeter, and the site of Max Planck in 2016 is called Zeller und Wickelt. This is in the case of an interesting example. You must have it here,
where you can activate it. You must have it here, so that you cannot have it at all, without having to work on it, without having to deal with any problem. You must have it here, without having to work on it. However, that is not right. You must have a refining of the electronics this is the most important thing and the most important thing in the pulse system.
I believe that this is the most important thing. This is a concurrence mechanism for this galaxy experiment. And an erosive group is doing this experiment in Caucasus, in the valley of Waksan. I don't know if you can see the situation now.
The virus is the most important thing. It is the most important thing. We are in the sixth century in the gallium, which is a huge tank of gas. We will see the gallium in the next years, in the next few years. We will see the growth of a wealth production rate, in a year, in the gallium.
This is the experiment. This is the most important thing. The gallium production will be a lot of work between all of the gallium companies. The gallium does not have a significant substance in the oil industry. The financial side is very interested in this.
For the third time in the gallium, from BMFT, from Max Planck, a company of 22 million in Denmark. This is a huge amount of money. However, the gallium will not be produced by this experiment, as we will see it in the next few years. We can't come to a better place,
as we are going to see it in the next few years. So when the experiment ends, we will begin in two years, so in the next few years, and then we will have to wait for the next four years, to see what we will do extra-poly. So we will make the next six years,
this gallium will be in the market. We can't do it. We are not going to be able to do it. We are going to invest in it. This will be a good investment for the experiment, as we will see it in the next few years. The gallium will be produced in the next two years, but we will have the detector, and the detector will not be produced.
And it is not very clear why that will happen. This is very interesting, that in our Brookhaven National Laboratory, with its largest chemical company, which we are going to see in the next few years, what is going to happen is that the Russian Group of Los Alamos National Laboratory is going to happen. And we are going to see in the next few years, the interesting situation, that in the first two years,
the American National Laboratory is going to have the opportunity to do something new, and that will happen in the next few years. We will see in the next few years. It is also very good, that this experiment, which is not going to happen, because the Russian Group of Los Alamos National Laboratory is not going to have gallium chlorate,
gallium, gallium metal. It is very good, that this experiment is going to happen in the next two years. You will see that, because that is not going to happen, that the result will happen. Then, when we are in full control of this experiment, then everything is in order. There is a standard zone model, which is going to happen in no time.
But what is not going to happen? When we are in full control, then we will see new neutrinos, new neutrinos, new neutrinos, new neutrinos, new neutrinos, and that will happen in no time, when it is not going to happen in the next few years. We will see that. Of course, we will also see that this is going to happen in the next few years.
We will see that in the next few years. We will see that in the next few years. I also want to mention, because it is very good, that this experiment will happen in the next few years. We will see that here, with a large tank, in which the gallium chlorate is actually being used,
and that a large acid is not going to happen. It is not so trivial. We have the big committee here. We also have a lot of knowledge as to what is going on. We are not going to leave. We are going to get the gas. The gas is going to be very early. And we will also see,
that we are not going to get a gold mine. We will see that in the next few years, and that the gas is going to be very high. And the gas is going to be very low. We also have a lot of knowledge as to what is going on in the next few years. And I am very happy to talk to a doctor who is here today. We have a lot of fun with this. We will see that in Italy,
in the big sassos, the new laboratory in which the gas is going to happen, and I also want to say that my American colleague is also here, Italian. And for the European patients, I also want to say that this is the middle Italian in Greece.
Here is Rome. And at 150 km east of Rome, we find the big massive approach, with the big sassos. And during this big sassos, the Italian has a motorway and an autobahn. And in the center, this autobahn, where the big massive is going to happen,
is going to happen in the big sassos and the big ones, the largest ones, and the largest ones are going to happen in Greece. And this is the Italian new laboratory. The next step is to take the big sassos and to find out what is going to happen after our experiment in Greece.
There are a lot of other experiments to be done. When he is here, he is going to do an other experiment in Greece. This laboratory is also a good example. This is the home of the big sassos. Here is the one side
of the autobahn. The other side of the other side of the autobahn. This is the part of the autobahn. So, if you are in Ruhr, this laboratory can happen. If you are in Germany, it is not possible. So, if you are in an autobahn, it is not possible. I am going to show you the two of them. I am going to show you in principle.
We are going to show you the main part of the autobahn. Our lab is here. This is a small cavity. This is not exactly a building or a robot. There are several large cavities for other experiments. The first one is for laser experiments. It is a small one.
We are going to show you this small hole here in the vertical side. This is also here. We are going to show you one of our physics that we are going to show you in this hole. This hole is the base of gold mine.
We are going to show you the large part of the autobahn. We are going to show you one tank under the bridge. This is a very big one.
These are the detectors. Here is the tank.
We are going to show you two of these experiments. One is the Neutrino-Kwelle and the other one is the Sonic-Conquerian. We are going to show you the calibration of these experiments. We can show you a little bit of information and a little bit of information about a gallium atom
that is in germanium. We are going to show you the chemical reaction of the solar atom and show you that the solution is not going to be possible. We can show you all the results. We are going to show you that we are going to show you three things.
However, we are not going to show you that we are not going to be able to do that. This is a big problem. We are going to show you that we are not going to be able to do it. If this is solved, then we will have to do it. Then I am going to show you the experiments.
This is a big problem. We are going to show you that our French and American colleagues are going to be able to do it. The French colleagues are also going to do the reactor. This is a mega-curie in the background in the 19th century. Atome Pro Secunde 1 we are going to show you that the Americans are going to do
the isotope analysis for this californium. We are going to show you 120 kilograms of chrome. We are going to show you that as neutral as chrome as the alpha-alpha- alpha-vend. We are going to show you that it is 40 kilograms. And that is a big problem. We are going to show you that this is a $5 million dollar price for the Americans.
This is the price for the Earth and this is the isotope for this experiment. We are going to show you a big problem. We are going to show you what we are going to do in the 19th century when we are going to show you the standard zone model and what we are going to learn.
I am going to show you a simple example of two parameters. The simplest model. The simplest is what I am talking about. We are going to show you a three-dimensional model. We are going to show you the quarks. We are going to show you the leptonian model. In logarithm,
we are going to show you the quadratic mass difference. We are going to show you m1 squared minus m2 squared because m1 and m2 are the mass of two neutrinos of one of the six. What I am going to show you in the next part of this is that the neutrinos,
the electron neutrinos produced, are connected in muon neutrinos, so they come in electron neutrinos or in the tower neutrinos or in the other ones that we as electron neutrinos are forming. And that was the reason why we were able to meet with them to learn about one sort of technology.
This is a long and long time ago. You wouldn't be able to see in a vacuum or in a quasi-vacuum and in the air state, in the inner sun, the idea that electron neutrinos are a complex thing, but all neutrinos with an electron in the sun can be used, or can be used. And that's why
we decided that we need to use the electron neutrinos for this experiment. This is the mission, which is that the electron neutrinos are a complex thing, and we need the neutrino mass, because in nature, we need quantum mechanics, we need energy, and we don't need to use the electron neutrinos.
Now, I'm here in the experiment of this parameter, in Blau. She says that what we need to do is to find out the mass of 10 minus 4 in the atmosphere, and to find out the mass of 10 minus 4 in the atmosphere, so that we can find out the mass
of 10 minus 4 in the atmosphere. I've been looking for a route for another experiment, which we've been doing for a year, and there's an experiment here, called the Gaussian Reactor Experiment, where the electron neutrinos are a complex thing, and we need to find out the mass of 10 minus 4 in the atmosphere,
and to find out the mass of 10 minus 4 in the atmosphere, so that we can find out what this parameter is and what this route is and what this experiment is. This was the most dramatic experiment that I've ever seen. Not only the logarithmic scale, but also a linear one, and then you can see that the most important thing is this and you see that neutrinos
are a complex thing, and you can see that this parameter is different. However, we have the upstream- the upstream-detector and reactor that we've already done for our 60 meters, so that the upstream- the air and the sun's are the same, so we need to find out the mass of 10 minus 4 in the atmosphere,
and find out the mass of 10 minus 4 in the atmosphere, and then you see that this experiment is the answer to our galaxy experiment. Also, if there is a difference in this in the atmosphere, then we're going to see, but we can't really see it. We can't really see that the neutrino mass is going to be different. And that is why this experiment,
which is a big experiment, nor this experiment, which is a small experiment, is too big. Therefore, we need to find out what this experiment is, and find out that there are a lot of groups that are in this experiment. So, in a way, I think that this experiment was a great one, because I find that, for example, this experiment was a great one, because I find that,
we need to find out when a positive result is that when the mass is is not so big, then this experiment is less, when the mass is not so big, then it comes into the atmosphere. The big experiment in this experiment is a big one, because we can see the relative light of one of the potentials of the two
that were so big, the big one, is also a very financial one, and that's why we need to find the best physical and biological results in this experiment. And if we need to find this result, then we can find out how much better it is. So, that's it for today. We'll see you in the next two weeks.
We'll see you in the next four months, in the first day, where you will see the following results from the other day. And we'll see you in the next two weeks. Bye.