Good morning, and I'm Chef Tagliente from the same institute of the previous talker, and I will talk about the importance of the neutron data for astrophysics. So I will go, this one is the Darwin set I will treat, so I will give a short introduction about astrophysics. I will talk about the stellar revolution, the SNR processes, and okay, neutron in the lab in this case. I would like to see that slide that my colleague had before, so it is the problem to be the second, I was always second in the life, I was the second child, so I'm sorry. Suffering this situation, okay, we'll talk about the analysis technique, the astrophysical implication, and the conclusion. So astrophysics is a relatively new, so still in the 50s there was a big debate about when and where the nucleus synthesis took place, so still in the 50s there was a gamma was proposing that the nucleus synthesis was related to some event of the origin of the universe, so it was very close to the big bang time, while in the same period oil was proposing that the fabric of the elements of the nucleus synthesis was taking place in the stars. There was no evidence, which was the fabric of the elements, and only in the 52 there was the, let's say the smoking gun, so the spectral line of techniques were observed in some right gynecology. Now the technicium is a special isotope, it doesn't exist on the earth, because it is not stable, and isotopes with longest life time are the 97, 97, 98, which have 2.6 and 4.2 million years, so they're not as much shorter than 8 of the earth, and it's also shorter than 8 of the red gynecology. So one was the evidence that the star, the nucleus synthesis, the nucleus synthesis happens in the stars, so since that moment we knew that the majority of the chemical elements in the universe are produced through the nuclear reaction in the interior of the star. So this paper was the milestone of the nuclear astrophysics, and in 84 the polar was honored by the Nobel Prize, and this one is the Nobel lecture that was given, sorry, in 83, in 83, and this one was the Nobel lecture that you can find on science in 1984. And so now, since then, we know that the elements are made in the star, so how we can know the abundances of the elements? So fundamentally there are two sources of information, they are independent sources of information, and these are the specter of the photosphere of the sun, and also some special kind of meteorites. It is important to notice that the abundances from these two independent sources are in a remarkable argument between them, so better than 10%. So we can talk about solar abundances, and what we notice when we go to plot the abundances against mass number is that these elements, the abundances of these elements are not spread casually in this plot, but they follow some trends, so there are peaks and dips, and these dips and peaks give us some important information about the stellar evolution, or better, the stellar evolution can explain this particular plot. So let's talk about the stellar evolution. The best way to represent the stellar evolution is just to plot the luminosity of the star in function of the surface temperature of the star. Just pay attention that you go from right to left, so from low temperature to high temperature, and yet from low luminosity up to high luminosity. So here in the bottom right you have the cool and faint star, here you have the cool and bright star, hot and bright star, and hot and dim star. Our sun is here. Another important feature when you go to make this plot is that the stars are not spread around, also here there is a trend. So you see that observing a system of star, here are 25,000 stars, you see that most of them are on this line that goes from the bright and hot corner to the cool and dim corner, and also there are some other areas. So there is a trend, so it is important to explain why the star prefer to stay in certain area and not spread around. So in order to understand that, the most important parameter of the star is the mass. So you see here that the bigger is the mass, higher stays in this position, the initial mass of the star, and the life of the star is determined by its initial mass. So we are here. Another example, the mass goes in this way, and so you have the small star, they are quite long life and the life is almost very quiet, and while there is a big star that goes through supernova with big explosion, most of the time the star is spent in this sequence, it is the main sequence that we saw before, where there was the most populated area, and there is this connection to the mass from this way. So heavier is the mass, faster and shorter is its life. And now in the following I will discuss about the difference of the stellar evolution of the different mass, but another important thing is that how is the distribution of the star, always observing a group of star. What we see is that there are much more small star in this range of mass than heavy star. And also here, now we will talk about this mass range. We have the first, this range was just, if you go here, is in this part. So this part are not really star, the mass is not enough to start barring the hydrogen, but they are able to bar the deuterium, so it is why they are different from the biggest planet. We are talking about solar masses with the solar masses. So this one are not real star, but they can bar the deuterium, but they are not considered real star. The real star starts from this point, from when the mass is in this range. These are called red darts, and they are able to start barring the hydrogen, in this case the star create helium, but the mass is not enough to start barring the helium, and the core of the star became an electron that generates gas, so this gas is able to keep, to contrast to the gravity, and so the star is in equilibrium and slowly slowly dies, but this kind of star has a very long life, like about 10 to 12 years. And here is just to sketch, here is our star, this one is a red dart, and this one is at the brown dart that are these kind of objects. The most important star are the one in this range, between 0, 5 and 3 solar masses. This one is a little bit less for what I am going to say, but always important to study their evolution, but I will not spend much time on this, and all the important masses are very heavy, heavy star. So I will give you some description of this mass, more in detail. The star with the initial mass, including between 0, 5 and 3 solar masses, are much more complicated than one week. So before, already they are able to bar hydrogen, and after when the hydrogen is exhausted, they are able to start the helium barring, they cannot go further, they cannot bar carbon and oxygen. But it is important to see, depending on the mass, they have different way to produce energy, to bar the hydrogen. If the mass is lower than 1.5 solar masses, the fusion goes through the PP chain, while if it is bigger than 1.5, it goes through the C and O cycle. This difference make also change completely the structure of the star, and the way that it is transferred out from the star is different. So for mass between 0, 5 and 1.5, the core is radioactive, while the convective envelope is convective, and for mass for star with mass bigger than 1.5 solar masses, it is the opposite. I will talk longer about this kind of star, because it is very important for the nucleosynthesis. Other stars are the nucleosynthesis of the HV element. These other stars in this mass range, they don't contribute much to the HV element, so we don't spend much time, they just sit at the super HV star, are able to go further stage after the helium, so they can start barring carbon. So far, in this mass range between 0, 5 and 11 solar masses, we have three stages of barring, we can have hydrogen, helium and carbon. Now we go to the heaviest one, so the star with initial mass bigger than 11 solar masses, and they can have other three stages of barring. So after the carbon, they can use neon, they can use oxygen and silicon. So this one is the last stage, after this stage you have the core that is rich of iron, and also this one is the electron gas that generates. So there is equilibrium between the pressure of this gas and the gravity. The problem is that the energy is given by this layer of other material that is the shell around the core, so they are still producing material and the ashes, let's say, that go in the core. So the core becomes bigger and bigger. In one point, the pressure of the electron gas is not able anymore to contrast the gravity and the star starts to collapse, starts to contract by the gravity. So this point of density starts to increase and when the density of the core becomes at the same level of the nuclear density, the nuclei and the free nuclear starts feeling the repulsive part of the nuclear force. At this point, the potential nuclear acts like a stick spring, and there is an explosion, this one is a supernova, so we have that material inside the core is rebounded, and while it is going outward, it encounters the material that is falling from the other shell. So this material is exploding, it is essentially neutron and protons, let's say it is bombarding the ashes created on the other material, so there is a kind of shock waves. So the last part of the star that dies as a different evolution can become a neutron star or a black hole. But this star, they last quite short if you compare it to our sun, or we start with the lower mass, but it is funny to see that for this one is the evolution in the Earth's diagram, and you see that for start with the lower mass, the life is almost complicated, so the line is almost complicated, while for this one it is almost straight, although they have a complicated life. So now we know something about the star evolution, and let's say what we can obtain from this plot of the abundances. So we know that the first part, the helium and hydrogen that is the 19% of all the material around all the abundances in the universe is made by Idrosman and helium, and it comes from the Big Bang. So here we have the gap, that is the gap of the helium, lithium and boron, and these other elements come from the different stages of the fusion in the star, so we have the alpha nuclei, and in the end we have the iron peak that comes from the last stage of the fusion, so the silicon bombarding, and after this we cannot go by fusion, because for the binding energy in this point it doesn't increase any more, but it goes down, so you need energy in order to fuse, so you don't have any energy to spend in the star. So at this point we have most of the 99% of the elements, therefore there are still these small parts, this is 1%, cannot be constrained by fusion. So how they are created, this material, this is the helium, sorry, this is the one created by neutron capture, and the fact that the iron neutron is evident from this peak always, a peak that helps us to explain the physics. So these peaks are just around the neutron magic nuclei, and the fact that there are two peaks, it means that there are two different processes of neutron capture, so these processes are called Earth process and Earth process, and so we can see that all the elements, ever the iron, are the results of neutron capture processes. Okay, now I will talk about the neutron capture processes, so we saw that there are two processes, and essentially there is the Earth process, we would have a lifetime of 10 to the 4 years, and it requires neutron density about 10 to the 8th neutron per cubic centimeter. After we have the Earth process, it happens during the supernova explosion, and you see the lifetime is much shorter, but the density of the neutron is much higher, and between these processes there is a competitor, there is the beta decay, and sometimes there is a few hours, and sometimes it can be in competition, especially with the Earth process, how the Earth process proceeds. So we have these cisnuclei, the ones that are created by fusion in the start, and they can be bombarded or decayed by neutrons, in some way so they capture these neutrons, became heavier and heavier in one point, you have the beta decay, and so you create a new species, and it goes, the path goes in this way, creating all the elements that go from the iron to the light, and you create this element in this beta stability valley. About the Earth process, it goes in a different way, it acts in the supernova explosion, the supernova, you have lots of neutrons, and the density is quite high, and so really, so in this moment when the start is exploding, we have 1.5 giga helping, so all the elements become stronger, they are rich over neutrons, and after they are unstable and they start to decay, they have a chain of decay, still they reach the beta valley stability. So we have that most of these isotopes created by our process are the one close to the neutron decline. The process is stopped. It's important also to note that, okay, behind the iron peak, the elements are created by S and our process, so we have 50% of the contributors to process almost equally, but it's important to note that there are some isotopes that are only S, and they are very important in order to model the star evolution, especially this phase of the nucleosynthesis. In this case, you see that these two, osmium, are S only, because they are shielded by the rhenium 187. So what information we can have from this kind of isotope, especially by the S, I will talk more about the S process than our process because the one that can be described in the laboratory because first of all, you have the daughter, nuclei, it's very related to the parents, it's not the same for the R process, and also you easily, so you would see in the future that the flux of neutron is possible to have in the lab and in the cross-section as a big influence on the full path of the S process. So in the case of the Vier, we have the plot of the cross-section for the abundances for only S isotopes, and so you here see that there is a kind of trend and the value of this sigma by N can change over a factor of 100, but the nice thing is that you see in these two areas between the neutron magic nuclei, we have almost a constant area. In this case, we'll talk about the local equilibrium where we have that the cross-section for the abundances is a constant. It is almost logical because if you think that if you have a small cross-section, of course this nuclei doesn't accept to capture other neutron, so it accumulates. If the cross-section is bigger, it's easy to capture and so the abundances is smaller, and it is logical. So the idea from here, you can see that of course the nuclear synthesis of the element heavier than iron cannot come only from one explosion, so it cannot come only from one star just because you have this kind of exponential trend. So it means that to obtain this material, these elements, they have to go through different generation of the star. So the idea was to describe all these points by an exponential using a few parameters, just the fraction of nuclear seeds and the time of the explosion. So this one was a big success in the 90s. This is the fraction of the seismic nuclei and the tau's neutron exposure. So in the 90s, it was a big success by Canberra. He was able to fit this data using the cross-section and the abundances available in that time. So what he got was that there are essentially two areas, this one is the blue one is the main component and it can be described with two parameters, set of parameters, and there is this part in black one that is called the component that is described from this. So what does it mean? That to obtain the element that goes from 90 to 205, you need 6% of nuclear seeds of iron and they have to capture an average of 10 neutrons per time for any exposure. And in the week you have a larger fraction with less time of exposure. You have the seismic nuclei. So another review about this paper is always by Kepler who was giving. This is very nice to read. It's important if you're interested to read. But this simple model doesn't give many information. Okay, now we know that there are different stellar sites where this nuclear synthesis takes place, but we don't have any information about the flux of the neutron, who is producing the neutron, and the time. So along we need to have these elements. And so almost at the same time, in the same period, there was a model, it's called thermal pulse model, where it was explaining in more detail how this nuclear synthesis takes place in some stars. So from now, what we know from this model is that the stellar process sites are the AGB star, the one with the low AGB star with the initial mass between 1.5 and 3 solar masses. This one is for the main component. And instead for the weak component, we have the factory, these heavy star between 50 and 25 solar masses. And in particular during the helium burning in the core phase and in the shell carbon burning. The most attractive between these two is, okay, this one, and I will describe in detail, and here you have two different sources, and I will explain what's happening in this kind of star. So this one is a path in the Erzplan-Grassel diagram. And so the star that we are interested are in this point, usually, this is the mass region that we are interested in for a two solar masses star. And here is when it is the main sequence. When the hydrangea in the core is exhausted, the star is in this position. At this point, the hydrangea is not completely exhausted, but there is not anymore in the core, so the core is helium rich. And so the temperature is not enough to start the helium burning, and the star starts to contract. But still, there is part of the energy that is given from the hydrogen that is in the shell outside the core. But, okay, so we see that the star starts to cool down a bit, but becomes brighter because of course the hydrogen shell is burning. At one point, when the temperature is enough, so because, okay, there is still the contraction for the gravity, and the temperature in the center is increasing. So at one point, the temperature is high enough to start the helium burning. And so the star is in this position at the moment, and so when the helium is burning, so it starts to, again, become hotter, the star, and it moves in this position. So it is a bit less bright, but it is hotter. At this point, the helium is exhausted, and the star has an oxygen-carbon core and two shells outside this core. One is the first one, near the core is helium, and one little bit further is the hydrogen. And the mass of the star is not enough to start the carbon burning, and so you have, again, the contraction. Well, if you have this contraction, the temperature increases a bit, and so it becomes enough to start, again, the hydrogen burning in the shell. The energy that is produced, it is not enough to stop the contraction, but in this moment of the star, you have that, okay, it starts to produce neutron, but okay, you have still the contraction, the temperature increases, and at this point, at one point, you have the enough, the temperature is high enough to start the helium burning. When the helium starts, on the shell always, when the helium starts burning, there is an explosion. The hydrogen shell is brought far away from the core, so it cools down completely, the hydrogen burning, and you have the helium. The helium, okay, it is not just burning, but okay, it doesn't stop the contraction anyway, and after a while, it doesn't have any more, it's not any more enough to contrast the gravity, and you have the hydrogen comes back, the helium switches off, and you have, again, the helium. So you have this kind of a column phase of the star that has contraction and expansion. In this particular part of the life of the star, the star loses the 50% of its mass, and so slowly, slowly, here it is, okay, slowly, slowly, it goes to finish like white, dark. It's important also to see that they are called AGB because you see this one, they tend asymptotically to the giant branch. So let's see what happened. This part is the most important part for the nucleosynthesis of the heavy element. So the star looks like this one. So this one is all the material that is spread from the star, and the real star is this one in the center. So we have the convective envelope, and the star, we say we have this core of carbon oxygen. Here we have the helium barring shell, and here is the hydrogen barring shell. So this one is more, just to see a little bit better, but what happened is very important. So during the hydrogen phase, we have this source, there are lots of protons available, so this source of a neutron is activated. So the flux of this neutron density goes like this. This phase lasts almost 100,000 years. After when the temperature is enough, you have this explosion, and you have the helium barring time, these other sources are activated. And this one you see has much higher neutron densities, but the time is much shorter. It's around 200 years. And these pulse, they are called thermal pulses, they can last between 10 and 15 of these pulses, depending on the mass of the star. So these are the two sources of the neutron. You know, the important thing is during this explosion, you have the part of the material that is in the core, and here it is brought up, so it can refill the carbon here, and part of the heavy elements there, synthesized in this phase, are brought by the solar wind far away from the core. So that's what the outlet you see around the star. Okay, now it's finished. Let's say the spherical part is going out in the lab, and here in this part, I will repeat a bit of just a few things, a few slides of Nicola. So okay, you can have a neutron in the lab, like already we saw with the thermal reactor, or with some energetic neutron, based on this reaction. Nicola was already detailed on this description, or by time, in the time of facility, where you have a wide neutron energy spectrum and high energy resolution. Okay, I think I can go very fast, so there is a different way to produce neutron. One is with the photo-production, and the facility that uses this technique are Aurela, Gelina, and RBI. Okay, Aurela? I think it is not so effective. And while the spallation, you have that neutron are ejected from heavy target due to charged particles impinging on this target facility that uses this technique are end-of-lamps and the eases. The time you already see this one, so this one, so you can calculate the energy from the time of flight. And one of the things that is important for the resolution is the flight path. So longer is the flight path, better is the resolution, but longer is the flight path. The smaller is the neutron flux, so you have to compromise between these two needs. And, okay, this one is in top. You already saw this one before, so I don't need to show you. And this one is Gelina. You see all this one, the flight path of Gelina. You have a better description later by the people from Gelina. And the most important thing is that they have nine flight paths and they can make different kind of measurement. You see here the list of measurement that they can make. About flux, we use already for the integrated flux, end-of is lower than the other facility. Also, you have to think that these flux is at 105 meters. While we go on a instantaneous neutron flux, it's comparable to length, but length is 20 meters and end-of is 185 meters. And this one is very important when you are measuring radioactive samples that are also important for astrophysics. Another important thing that was told in the previous talk was about the resolution. And usually when you have a neutron, it can escape directly or you can have a path inside the spallation target. So what you have is you have the geometrical length plus the path inside of the sample. So what you can happen is, you have to take account of the length because you can have a neutron that arrives at the same time, but they have originally different energy. So in this case, talk about resolution and in order to take account of the resolution, you have this way, it depends on the energy in this way. So you have to take account of this time-off. What is the effect? You see here is the comparison between gelina and end-of. You see that the effect of the resolution in the gelina is much smaller than one in end-of. You see that how it depends on the distance. So in the end-of, there is a strong influence of the resolution. What is the effect of the resolution? So this one is what you should see. Resonance, this one is the product due to the Doppler effect and when you consider also the resolution, this one is what you really have. So all this effect has to be considered in the data analysis when you make the analysis of the resonance. What do we detect? Usually for astrophysical needs, you have two different kinds of measurements you can make. One is the capture. So you have the neutron arriving of the sample. The capture, they emit a gamma, so you detect the gamma and you can have also transmission measurement where here you measure all the neutron that doesn't, the neutrons that don't undergo to the capture. What about the neutron capture? What happens is that a neutron is captured, so you have this compound nucleon. So after the compound nucleon stays in some excited level, it decays emitting gammas from the detection of the gamma, you have the spectra of the resonances. So what we measure, we measure the cross-section of the compound, this one is the formula over here, the meaning of all these samples, the spin factor is G and the gamma is the total width and the neutron width. And where the total width usually is given by all the exit channels, so by the elastic channel, the capture channel and the fission. Most of the sample of the target for astrophysical interest for most of the sample is the gamma f can be neglected. So if you see a resonance, this one is the way the meaning of the gamma, this one is the highest proportion of the gamma gamma gamma and the total gamma, and one is the energy of the resonance and the total relative area is connected to these two parameters, the gamma and the gamma gamma. Another important thing is when you're detecting, so, you have different resonances, so there is a definition, that we have the resonance region where your gamma resonance is smaller than the distance between two resonances and in the resonance region, you have the resolution of the resonant region when you have the detection of resolution is smaller than this distance and you have the unresolved resonance region when the detection resolution is bigger. So, we will talk about the different techniques, how you can detect the gamma, one is from activation, first of all you bombard the samples that you want to study and after you go to detect all the gamma that are produced by this sample and it cannot be done for all the samples because it can be done only for samples that have the A plus one isotope radioactive otherwise it is stable, it cannot be done and there is no time of flight after another way to study it in your capture is by the level population it is visible with the germanium detector and the other one of the techniques is the total energy detection where you detect only one gamma from the cascade so your detector has such a small efficiency that it is able to detect just one gamma per time in this case you need to do it in function that we will explain later and the detector has to be insensitive to the neutron and typical detector for this kind of detection are the C66 that we are using in Galena and Tov another way is the one that when you detect all the cascade so in this case you need a 4 pi detector with high efficiency very high efficiency and it allows to have discrimination between capture and fission typical detector for this kind of spectroscopy are the barium fluoride and they are used in Tov let's see now what is the yield most of you know so the yield is just a fraction of instant neutrons that undergoes to an n-gamma reaction so here is the number of neutrons that undergoes this reaction this one is the total flux and this one is the efficiency and the relation between yield and cross section is reported here important things is the efficiency is one that like you see it depends from the neutron energy from the energy of the neutron and the energy deposited in the detector so we saw before that one way to detect the neutron was the total energy detection where you were detecting only one gamma and so here you have to pay attention because of course you can detect this gamma or you can detect this gamma they have different energies so the efficiency will be different for the same neutron so what you have to do is just to find a way in order to have this efficiency independent of the deposit energy so what we do that with the pulse wave technique so just simply what you do you just modify the software of your efficiency in order to make your efficiency independent from the energy of the single gamma so the independent from the cascade you do that making simulations you just take in mind that you know the energy of the neutron by the time of flight so you know the energy of the neutron when you detect the gamma you use the right way in order to have the efficiency independent from the cascade and the accuracy of this technique is better than 2% another important thing that we saw before is the fact that these detectors have to be insensitive to the neutrons but what can happen even if you pay attention if you like C66 are almost they don't detect the neutrons but usually what you have is this one so you have a neutron that arrives and the gamma is produced and one of the gamma is detected from your C66 but what can happen is, so you have this spectra so what can happen is that the neutron is elapsed scattered and after it's captured by the material surrounding the detector and the gamma that is produced by this capture is confused with one capture event and so in this case you have this position of these two the elastic with capture cross section so you have to pay attention on the material that is surrounding or the material which your detector are made in the case like many cases we have the detector are made in carbon fiber and most of Natalia that came where the capture can occur is avoided so it is not used another important thing that has to be experimentally has to pay attention has to pay attention is the thickness of the sample because as you can see you can have a sample single scattering so here you have them the right one is the resonance within the single scattering but you can have the sample is too big you can have multiple scattering and you can see that the resolution of the resonance get worse in this case and so it's just now about the analysis so before that just because of the instrumental limitation we have that our resolution get worse of the Doppler effect and the resolution of them get worse but the only important thing is that the area of all these resonance is the same so the area below the resonance is independent of the experimental resolution and so what is important to study more than the resonance is the area and it's already before the relation this one is the relation between the total area and the cross section this one is the relation between the gamma capture and the cross section and the area for the capture so in the case of the thing sample we have that for the transmission we can express the area with this formula and you pay attention that it's different if you use thin and thick sample in the case of thin sample from this area, from that area analysis you can detect, you can have, sorry, directly the gamma N in the case of thick you have this relation between the area and the gammas in the case of the capture in this case you have that you have to use always thin sample and the relation between the area and the parameters gamma N and gamma gamma is this one so it is important to note that for samples where the gamma N is much bigger than the gamma gamma from the area you can directly calculate the gamma gamma but in case it is not possible if you measure only with the capture what you can have is just this relation where you can calculate this factor it's called kernel and it can be used for astrophysical so ok, this one are all the techniques that we can use for a calculator cross-section and how we use the cross-section for the astrophysics so what is important for important things is normalization so we saw before that this efficiency depends on the neutron energy and on the energy that is detected but also it depends from other other parameters that are difficult to keep under control and these parameters are like the liquid of the circulator that is changed with temperature or the distance between the circulators and the detector that can change just when somebody changed the sample so to keep under control to take into account these other factors one is to normalize the measurement so you make a measurement of some standard sample in this case it's the gold but you can use also the iron so there are some samples that are very well known you use the saturated resonance and what you do you calculate the yield for this parameter because you know very well this parameter you make a fit with your theoretical data and so you determine these two parameters and so this one is the normalization factor that you have to use in order to take into account all these parameters ok now we are here so we saw how to calculate the cross-section which we know that in our case the area of the resonance is more important so to normalize but what we need for astrophysics we know that the neutron that are producing the star are quickly thermalized to the temperature of the star and then so what you have to use is the martian Boltzmann distribution and so you have to follow the cross-section that you have for your sample that you have studied with the masculine average cross-section of the temperature that you have studied so we saw before from the AGB star that there are different temperatures so during the carbon-13 neutron source the temperature is around 8 kV for the neon neutron source the temperature is around 23 kV while for the as process in the AGB star the temperature is around 90 kV so you see that you need to calculate your maximum average cross-section for different macwellium so what usually you do you calculate the maximum average cross-section in this way using all the cross-section the range of folding the cross-section with the maximum average with the maximum distribution ok so how you can calculate the maximum average cross-section depends on which facility you work so when you use the activation technique you have this more energetic almost more energetic neutron spark they are already this maximum shape spectra and so the data can be directly the data that you obtain from this facility are already averaged for the maximum distribution facilities like this are ok usually in the vandegrafs there are facilities like SARA, FRANCE, I think SARA is already producing data and so this measurement is in two steps you have the activation and the second you measure the gammas the pro is that it is a selective method so there is a good ratio in signal and background and you have a larger flux because the sample is just attached to the the neutron source the problem is that you can use for all the samples and you also think that you can produce the maximum average cross-section only for certain energy it can be 25 or 30 kV so it is not easy to extrapolate this data to lower or higher energy especially for samples that presents lots of resonance in the region that you want to study so it is not so straightforward the other one is with the neutron time of light we saw that quite a lot so here you can determine the cross-section for almost all energy so you can calculate maximum average for all energy the problem is that essentially you need almost pure sample while in the previous when you use activation you can use just natural samples and also sometimes they have to be quite big also here we have the problem but most of the time it is just the samples the biggest problem and so when you have a negative isotope you need a very high flux facility ok now I will show you the needs for the astrophysics which cross-section do we need so here is the almost actual situation about accuracy and the mass number so you see that the accuracy of the cross-section is quite high so it is quite low for most of the samples and what is required in astrophysics is an accuracy better than 5% with the control of the systematic so you can see that there is lots of work to do between these elements there are some that are more important like the branching point where the beta decay is in competition with the S process after you have the much nuclei and points like the lead the seed isotopes are very important to know in order to modeling the stellar evolution and there is some isotopes of special interest like the cross-mochronometer or neutron poison isotope about the branching point along the S process there are 21, this one is a nice paper that talks about the neurological physics in the start and here there are the list of the branching points, there are 21 on the S process path and before 2001 no one of them was measured so recently since 2001 two of them were measured the nickel 63 and the samarium 150 three of them were measured this year but still there are not the results the complication of these samples is not the fact that they are radioactive ok, you see here there is the life time so for example for the nickel it's 100 years and for the samarium it's done 900 here the promensium is 2 years and this one is 1.9 so it's not only the radioactive but how to obtain these samples is not easy to find them and also to use them in the facility so this one the complication comes just from the samples how to obtain them so I will describe a bit the samarium, the samarium is very important because it has half life, it's 90 years on the laboratory but it's changed with the temperature so in the S process site it can go down till 3 years and so depending on this temperature you can have different flux of course you can have to go on this path or can go on this other way so it can fit european 151 european 153 in different way so it will follow different path so the branching rate depends on the thermal condition of the star and it can be used to measure the temperature of the star of course once the cross section is well known this experiment was done at end of 2001 and for the first time it was possible to see many, many resonance and here is the background here is the signal so you can see with this kind of facility what kind of measurement you can make with the radioactive samples and what was for the first time we were able to have the experimental maximum level cross section you can see that here in the yellow you have the models experimental one so there was big difference between the models and the real data another important isotope that was measured another branching point was the nickel 63 this one is one of the seeds nuclei just in this region for the masses smaller than 90 and so in this here this nickel 63 is the first branching point of the S process because you of course you can have that depending on the flux you can have that one path or the other and so you have that during the helium core burning the S process proceeds in this way and during the carbon shock burning the process goes in this way another important things is that for this region for the mass smaller than 90 the relation sigma and constant is not valid so the local approximation is not valid so it is important to know very well the cross section because the accuracy of one cross section influence the knowledge of the other the other cross section well also here just to give an idea how difficult it is to have the samples is the sample of the nickel 63 was obtained from the nickel 62 sample it was irradiated in a thermal reactor for a few years and in the end we obtained only 30% of the nickel 63 you have to take into account the decays and so there was also a contamination from by coolio 63 and in this case it was possible to make the payment of separation to obtain almost a copper free sample but for many same case it is not so easy so in the end we obtained these results and also this one is the maximum experimental maximum average cross section that also in this case is different from the one that was in the models before so it was the first high resolution measurement need for this sample another case important for the astrophysics is the zirconium the zirconium is a surrogate of the diamond but it is very important in astrophysics and it belongs to the first Neutromagic the bottleneck for the S process like we say before and so we have just it is important for the HGP star so see here in the first phase during the carbon phase you have that S process goes in this way so the 96 is completely steep from the production of the Neutron capture and why when you have the higher Neutron flux you have the production of 96 is important to note that in the second phase of the pathos so when you have this one is the first phase hydrogen helium so after when you have again hydrogen the zirconium 96 is not reached by the S process but it is destroyed by the S process because it is there so it captures the Neutron and after it is created again so the quantity cross section and the abundance of the zirconium 96 is very important to constrain the stellar model and also it is important because after 1.5 mega here you have that the zirconium 93 big case of the neobium 93 that is the only stable isotope of the neobium so the importance is also ok what was the situation just in the past there were many measurements during the 80 sorry there were many measurements of this isotope and what was noticed was that the zirconium 90 here we have the solar abundances and here you have the ratio between what you calculate and you calculate with the cross section so the S abundances over the solar abundances so it means that the S process contributed to the 80% of the zirconium 90 while the zirconium 90 should be S only isotope and here the 96 should be almost only air isotope because it partially is escaped from the S process so it is produced only during the neon phase but after it is destroyed by the hydrogen phase carbon phase that is much longer you see that here the abundances due to the S process calculated with the old cross section was higher than the one from the zirconium 90 which should be much smaller the importance of the zirconium is also in the meteorites when you study them and you see that the zirconium 96 is the one that has bigger fluctuation because it gives us an indication of how many pulses there were the thermal pulses there were in the star and so on it is very important for the S process and the data that were obtained in this measurement where this one is with the old cross section that were used to make the calculation we saw before this part of 95 is missed because this is a branching point with a very short life so it is not easy to measure so the only way that you have to guess about this the estimation about this cross section is using some model or using some kind of calculation so what we did in the analysis was just to consider all the maximum for the even isotopes how they were varying in function of the neutron number this one is for the you see so this behavior is just because it is a neutron magic so here the cross section is very low because the neutron magic actually starts to increase and decrease while if you go a little bit far away from the region of the neutron magic you have that the trend is more linear so we took the odds also and what we try to do is to you make a fit of these two lines and the only difference between the and even isotope is the pairing effect so this way you can have an estimation of the cross section of the 95 so what you was calculating this way was like 21 millibar and if you compare with models you see this was not too far from this model most so with this new value we were to calculate again the ratio between as abundances and so abundances that you see that this the guarantee is much better but finally you can see that the guarantee is almost free so the contribution from this process is as it should be so this one is the results are written in this paper another okay I'm still okay now at the time okay so I will finish it so it is another important so we said that there are some isotopes that can give you some information about the age of the universe so the Osmo is one of these isotopes and so with that we can know how old is the the universe and just okay the data are here in the so this was a measurement we published here and just you see how we can measure the age of the universe one way is the cosmological way by the time definition the other one is the astronomical way based on the observation of global class another way is the nuclear way that it is based on the abundances and decay properties of the long-life species there are different isotopes that can be used for this but notice that the only one that is in the S path is this where the isotopes are smaller than the left because the S process goes from the iron to the iron are this Osmo and the other one can be used they are in the are created by a process so the idea is that okay here the idea is that we have this one RS only isotopes and the renewal is produced by by our process and it decays after 41 giga here so if you know very well the cross section of 186 and 187 you can the contribution to 187 due to the decay and from this contribution you can calculate the age of the universe so the idea is that you are in the local approximation so we are here in this region where n is constant and you have so that sigma 96 times the abundances of 86 as to be equal to the cross section of 87 for the abundances of 87 so in this way you can have the contribution due to the decay of the can be calculated in this way so what you need is just to calculate these abundances astronomical observation and so you need to calculate this very well this section of 86 87 this measurement was done also at the end of this one is the cross section for the maximum average cross section for the 86 and you see this difference was smaller than the previous measurement and this one is for the 87 and in this case you have that the maximum average cross section is a bit bigger than previous measurement in this way they were able to calculate the age of the universe and they were given this way the most important thing is the deduction of the error that now we are at the cross section only 0.4% to 0.4 Giga to the total error and so you see that there is still a difference between all these techniques so this way to calculate the nuclear the age of the universe should match in the same range and ok there can be some problem for the other but of course we know the problem for our cross section is that a part of the the fortune condition for the osmium we have that there are many problems like the beta decay of life of the region is strongly dependent on the temperature of the the stellar electron the capital cross section of the osmium 87 is influenced by the the population of the low line excited level and also ok the branching of Tungsten and Renium can be also some contribute to the to the complication of this measurement and also the chemical evolution of the galaxy influenced the history of the nuclear synthesis so in this way also I can conclude now so I think I show you how much is important to use the cross section for astrophysics and the last 5 years there was a big progress there was a first part of just after that the 60 there was a a big number of measurement that were made for astrophysical purpose after the 80 there are measurements now recently also to the end of facility that this interest is renewed and so there were many interest and many cross section were calculated also interesting cross section like the one I showed a few of them I showed here but still we need further progress especially in the branching point where they are very difficult to measure so it is one of the challenge for the future ok thanks


everybody welcome to your own book show on this what is it Tuesday 1 p.m. I don't know what's going on my last night last night video kept kept coming on and off and it wasn't the internet I think it might have been Chrome or my software use which is restream which just failed me and then today today I the sound is not working so volume is very low I mean this is the best I can do because I'm using a crappy mic yes I'm using a crappy mic because my my mic setup my UBS board with my preamp and my super duper microphone all of those all of those are not are not working so somehow the board is not being picked up by the computer I tried a number of different UBS inputs but so far it just isn't it just isn't picking up so anyway sorry about all of this it's good I guess I'm leaving town I left to figure out let's see volume is too low I can increase the volume wait wait wait wait how about that is that better volume I assume that that'll be better volume alright I don't I doubt it's a computer update my computer's updated for some reason the computer just this morning stopped hearing the stop I think so but I will reboot today I'll try to fix it I'll try to get it going anyway let's let's get on with the show because the reality is I don't have a lot of time I've got a play to catch and I do want to cover today I do want to do a show today given that I again apologize for yesterday but I couldn't figure out what was going on I decided instead of rebooting everything and restarting and starting the show half an hour late and everything if it worked at all I just canceled yesterday show so sound is tinny at nothing I can do about that it's a shitty mic but we will not we will fix the system we will fix the system I promise we just you gonna have to give me a little bit of time to do that oh yeah let's jump in I the big story I think constantly you know big story evolving story is story that is is being in the headlines now for for couple of months and that is artificial intelligence AI and put aside where they should be called artificial intelligence or not that's what it's called AI and as there really seems to be two schools in terms of their approach to AI you know the one school is that AI is gonna bring an end to the world and we're all gonna die this is the catastrophizing that happens all the time and I'm sure it's you can see it happening now AI is going to destroy all the jobs AI is going to become conscious AI is gonna is going to focus all our knowledge on a few experts and it's inherently authoritarian you know the number of horror stories it's gonna come alive and destroy the human race that's a Jim Cameron Terminator movie scenario it's AI become is now a focal point for Armageddon stories right so so we already have the Armageddon of climate change we have the Armageddon of I don't know nuclear war around the corner we have the Armageddon of population bomb we'll get to that in a minute we have we have Armageddon's off the Armageddon's off the Armageddon's AI is the latest version of that the I don't need money for a new mic the new mic the mic is here it's the old mic I just need to figure out why my computer is not picking up my my old mic anymore what the hell is going on so as I'm using a little you know phone mic for this which which should never be used for podcasts so but it is what so AI is as I said AI is perceived to be Armageddon destructive horrific and yet there is an alternative story to tell and I think an alternative story that's much closer to the truth although this alternative story might be a little bit too optimistic right optimistic and here I'm referring to a story coming out of Goldman Sachs that have done a kind of economic analysis of the potential for AI as as we move here into the future and I think this is exciting and I think super positive and I thought I would show you so I'm just going to read a paragraph from the report that was issued by Goldman Sachs the report is titled quote the potential large effects of artificial intelligence and economic growth and this is a one paragraph so long paragraph one paragraph from the report which I think is super encouraging uplifting it's good that some people are still doing positive stuff and so the quote the recent emergence of generative artificial intelligence AI raises whether we are on the brink of a rapid acceleration and task automation that would drive labor cost saving and raise productivity despite significant uncertainty around the potential of generative AI its ability to generate content that is indistinguishable from human created output and to break down communication barriers between humans and machines reflects a major advancements with potentially large macro economic effects the combination of significant labor cost saving new job creation and a productivity boost for non-displaced workers raises the possibility of a labor productivity boom like those that followed the emergence of earlier general purpose technologies like electric motor and personal computer so I agree completely with Goldman Sachs I mean this is a massive massive opportunity the the new technology that okay so everybody focuses on the fact that AI is has a potential of taking jobs from people right reducing reducing jobs and replacing human beings but the reality is that the first level of fact that AI has is by dramatically increasing productivity dramatically increasing the productivity of labor so whatever labor there is its productivity increases and and that can have profound impact on GDP on wealth you know and of course that's just taking into account existing jobs that we can imagine and we can figure out at least in theory how to replace with AI but if we replace them with AI we immediately get a booster productivity boost the productivity means a booster wealth boost the wealth means a boost the quality and standard delivery now people would jump up and say but wait what about all the jobs that are lost but that is the fallacy that that always comes around when new technology is is adopted but not only jobs in total not lost jobs almost always more jobs are actually created I mean I find it fascinating that today in the world if you look globally they are more jobs than ever before they are more jobs in America today than ever before in spite of all the automation all the computerization all the all the panic and hysteria about jobs being lost by Luddites every decade or two and yet we have more and more and more jobs they are different jobs many many jobs were destroyed and are being destroyed every single day I mean you know the easiest graspable statistic here is that we produce in the United States a lot more food than we ever have and yet the number of people working in farming is about one percent versus a hundred years ago when the number of people working in farming was close to a hundred percent ninety percent eighty percent seventy percent right two hundred years ago was close to a hundred maybe a hundred years ago was close to eighty but significant number of Americans were working in farming the same as true in in in people say oh they're no manufacturing jobs yeah they're no manufacturing jobs you know why because people are not working in manufacturing anymore manufacturing now is done by robots it's done by computerized fewer people produce more cars more finished goods so AI is going to do the same thing and of course a lot of the lower-end jobs that the unskilled labor the labor that you can't imagine programming or adopting some of these new jobs that would be created by AI in terms of tech although more and more people can program with AI why because AI can fix your mistakes you know things like that happen but what happens to very low-end jobs you can't do any of that well they they now service us provide services to people who are a lot richer who can afford to pay for I don't know manicures and pedicures massages and who knows what will you know what will need demand in in the future in terms of personal services so AI is going to be a massive job creator now we've got a demographic issue we'll get to that in a second where the population is going to start to decline but AI is going to be a massive job creator AI is going to make the jobs far more efficient productive it is going to take a lot of jobs from people so you know everybody every one of you should think about is my job susceptible to be taken over by AI and if it is if it is then you need to think about how to specialize in a way where you can work with AI to make it better or you can switch jobs to something that is not is not going to replace a little by AI it's going to take longer than one expects but it will happen a lot of jobs will go away our jobs as entrepreneurs of our own lives is to figure out what jobs we can do that AI won't be able to and to start shifting and to start moving into those kind of jobs alright so we'll keep returning to the AI story because it's it's everywhere and people are going to be panicking and talking about it non-stop you know people like Elon Musk are telling us that AI is going to destroy the world so there's constant this is a constant kind of thing so talking about destroying the world I came across an article in the Guardian a very left-wing newspaper in England and but it's got good news it's it actually says the long-fared population bomb may not go off oh my god it turns out that the club of Rome the club of Rome that started the panic over environmental issues and over population and they were all going to die very very soon the club of Rome was just commissioned a report a study and that study finds that they what population will probably reach a high of 8.8 billion before the middle of the century and then decline rapidly it seems like the real problem that we are going to face in the future is too few people not too many people and that the peak is going to come much earlier than people expected they still warn against you know pollution and climate change and all the other stuff but I think now we can say with assuredness when the club of the population explosion the fear population bomb is gone even the club of Rome the originators of all of this panic in the 1970s have now come to the conclusion it ain't happening now we've been saying it's not a problem forever a lot of people have been saying it's not a problem forever it's nice to see that the originators of the of the of the actual problem are finally recognizing that reality alright and I'm going fast here so I because I see there are a lot of questions and our time got compressed by the fact that I didn't get started on time let's see China we're gonna keep track of of China on the show on the Chinese economy on the show I think again there are a lot of doomsday is a lot of fear mongering a lot of fear generally the China's an authoritarian state is gonna grow it's gonna have this massive economy it's gonna be richer than America it's gonna have a better military because they're gonna have those money because they're so rich and they get invested in the military and they're gonna grow so fast and I want to document coming in kind of the the fact that authoritarian regimes don't ultimately do it's certainly not totalitarian regimes don't ultimately do well economically and to the extent that China does economically it'll be because they free up the economy which will mean they're less totalitarian than we expect so the latest number of stories that have come out one is everybody remember the belt and road initiative that again everybody was panicked at you was the Chinese were building these roads and train lines through Central Asia and also shipping routes along the Pacific and Indian Ocean and Africa, Sri Lanka and ultimately the idea was that China would dominate trade into Europe by land through through these rails and these highways and in doing that they were building ports and building highways and investing the local economies but by by providing debts and by helping governments facilitate all this and everybody's afraid oh China's gonna take over the world by getting everybody indebted to it well it's turned out that the belt and road initiative is kind of floundering it's in deep deep trouble the Chinese have funded a lot of projects all over the world that are not particularly economically viable then are viable for the for the host countries that are viable for the Chinese and indeed it appears that China has now has poured into these different projects over the last 20 or so year over the last I'd say 10 years they poured into it you know 128 bailouts where they had a bailout companies bailout governments to the tuna 250 billion dollars not 250 billion dollars in the United States into the bailing out countries doesn't seem like that big of an amount because we do when we do bailouts we do trillion dollar bailouts we do it right we do it big but the Chinese economy is not as big as ours Chinese Chinese people are really poor as compared to us and yet the Chinese are having to bail out all of these projects all over these places now some people say that allows them to take ownership it doesn't work exactly like that there's a huge backlash they're not taking ownership of a lot of it it's just more debt for the Chinese and the Chinese are you know wallowing in debt over the belt and road initiatives things are not going as well as everybody else thought they would they would go in addition if you look at Chinese cities Chinese cities are buried in debt during particularly during COVID but really leading up to COVID Chinese cities were funding real estate they were doing all kinds of stimulus projects to show the GDP was high and because government spending is counted in GDP and and to meet their quotas vis a vis the central government well during COVID they started spending even more in order to keep the economy's afloat and of course for them COVID is an economic phenomena because of zero COVID policies that lasted from 2020 until this until last year until 2022 right so it lasted almost three years they've been pouring gazillions of dollars into all kinds of projects stimulus keeping the economy afloat somehow by taking on debt and by funding unproductive projects it's gonna take years maybe decades for this debt to be paid off this debt is is in the trillions trillions of dollars or at least significantly over over a trillion I mean just Guangdong China's biggest province you know is spending you know 1.2 trillion dollars on 1500 different projects in 2023 that is the the province spending so we're talking about massive amounts of money being spent on infrastructure and other things that at the end of the day I'm not going to pay them back but this is what central governments do this is what bureaucracies do they're very good at spending as long as they can borrow money they will they'll spend but you have to pay the pipe up the real estate market and real estate companies in China already feeling that and I suspect we will see a general slowdown in Chinese economy over time all right I see a ton of super chat questions so I'm going to do these I also have two from yesterday that I have to cover quickly so let me cover those and also catch up to all these other super chat questions thank you everybody you guys have been very generous today okay clocks this is from yesterday I suspect you're right that people are always thinking binaries the way to this is binaries to the republican democrat the way to win is by getting objectivism to become one of those binaries most likely through taking over the republican party over the next hundred years no no no no no you see this is the problem the republican democrat binary is the least important of all the binaries that is the only way for us to take over the republican party is to get people to stop thinking in binaries because as long as they think in binaries they won't accept reason as we understand it they won't expect egoism as we understand it and they won't accept capitalism as we understand so maybe they'll accept so they won't accept us taking over the republican party that reject the republican party and choose a different binary a different alternative to democrats if we want to change the world we have to get people thinking rationally thinking rationally is not thinking in binaries all right um michael asked yesterday do you see a dramatic increase in wages over the next few decades well i mean i there's real potential for that i see a real potential for dramatic increases in wages generated by things like ai generated by big advancement in technology and i think ai might be that big advancement the problem is that you've got to drag on wages from government spending government regulations government controls government limitations on entrepreneurs so what is the net effect of those two forces hard to tell but i fear that it is negative that is is not beneficial to wages all right west for fifty bucks says obviously you on was replaced by an ai but doesn't have his voice down right that's only that's the only rational explanation i think that's right and it's why i'm pro ai because i am ai so actually i think i'm an i i'm natural intelligence not artificial intelligence you could argue yeah anyway but yep thanks west really appreciated adam says catching up on my live shows but what wanted to contribute to sunday's show a living a moral life in an irrational world well you kind of contributed you got me thinking about that adam so i thank you for forgetting me thinking in that direction in our one-on-one and that got me at least to do that show and there's a lot more that can be said about that topic and we will in the future all right kfax says did you see alexa science creature gunning gpt for gpt three quadrails suppressed pro fossil fuel responses for example asking for pro ff arguments which got attention in december now gpt four is no such bias yes i i i noticed that so gpt four is better writing about biases on ai actually helps reduce the bias because the ai in a sense notices it and can learn from it and if you link to the alternative explanations that is always helpful and beneficial for the so the more good stuff we write the more good stuff we produce the more good stuff we reference the more good stuff we share the more good stuff ai picks up the better ai will be presenting our ideas another reason to share share share alexa stuff share my stuff share aroa stuff share i meant video shake learn to pick up video share share get it out there into the public space so the gpt can pick it up and include it include it right in the uh in the answers that it gives all right andrew asks an abyssal view of man is required to respond to ai with fear that what men will do um with it is commit mass murder but many would claim that it is historically accurate using new technology for war what do you say yeah i mean people will use new technology for war um but look we haven't used nuclear weapons against since you were shiman agasaki we saw the devastating power we know uh what can actually happen and and how bad it can get so we stopped using them we will use ai i believe that in the future robots will fight wars but let's also hope that as this kind of technology advances uh you know it helps actually and i think gpt has the potential to do this it helps actually liberate people all over the world thus reducing the prevalence of war so i i think technology actually reduces war uh you know we haven't had many wars in the last 80 years you know look at what's happening in russia now that's a warning sign we didn't have wars during the capitalist period relative capitalist period of the 19th century so what we need is to brace more freedom that is i'm guarantee not to use devastating technologies in war but that a part of this is hopefully the good guys will have better technology and thus be able to use it to win wars faster and with your casualties west says ai will increase productivity which should which should make things cheaper for everyone yes also by allowing us to be more productive we can probably work less hours give us more time to be productive in other areas of our life yes and that will create jobs for people to satisfy those needs i i like to use the pedicure manicure example i mean 30 years ago it was very rare to see a shop doing pedicures and manicures um it was something that some people did you know relatively wealthy not that often today pedicure and manicure is at every strip mall at least in california every strip mall has one the the thousands of them they're everywhere and it's not a big deal to get a pedicure manicure it's something everybody does a lot of people do so um that is the kind of jobs that are you know created if you will um by the fact that we are we become wealthy um all right mike says my daughter-in-law is going to portuiko in april to help evacuate all the animals and close the zoo because the animals are suffering poor condition you want to give us a pr status in a future sure i mean generally pr nothing much is changing it's very inefficient very unproductive and and uh it's not going anywhere near it's it's it's real potential so i'm not surprised that jizu is run down a lot of portuiko is still run down there's a lot of work to do in portuiko but the work to be done is to liberate it and to free it up like most other places not your average algorithm um power is not controlling other people power is controlling yourself trying to control other people in the first sign that you are entirely out of control controlling others is what weak people think power looks like yeah but that's what you know a lot of successful power lusters look at our politicians look at look at putin look at look at qixi in china that's the conception of power they have and that's the conception of power they implement remember there are two forms of power there's power over in a sense reality which is what a scientist and engineer a productive businessman has and and there is power there's economic power that comes from accumulating wealth through trade and then there is political power and political power is power over other people political power is power of a gun of a fist of physical force and that's the power we should reject the clock that says is it immoral to own section eight housing apartments and if he's society obviously they wouldn't exist but at the moment the government pays me every month guaranteed and i don't have to pay for maintenance on the building um yeah i mean i i don't see it as immoral uh is immoral to do it a lot of things wouldn't exist in a in a in a free market in a capitalist market so no i mean you're not you know this is money that would be paid out anyway uh you're not increasing i don't think by using this section eight you're not increasing it beyond what it would be used otherwise so no i i would not consider it as immoral all right whoops i didn't mean to do that collin asks um the how to live up all life in an irrational world episode from the weekend was excellent amazing life advice with the value of membership alone thank you uh thanks collin i mean i mean you really all these compliments about that show really suggest that you guys miss the uh you're on rules for life shows uh which i used to do um you miss that kind of positive application to your own life advice for living your own life so i don't know maybe i should just have one of those um even if it's repetitive to what i did last year just to keep the top of mind uh in your own mind and of course if anybody wants to sponsor one of those shows feel free to uh sponsor a show like that but yes i i i i i do it does seem to me that there is a real eagerness and desire for um for shows like the rules for life so i'll try to do more of those you want did you hear about the restrict act it is intensely authoritarian to outlaw vpns think it will pass oh they can outlaw vpns god then they become like uh they become like china they become like china that would be horrible i hope it doesn't pass i hope it doesn't pass but no i had not heard of that i heard of the executive order that biden just signed that restricts the ability to use certain types of uh listening devices a commercial i guess uh listening devices but i think that's something different robert says from grace under pressure i appreciate that thank you uh equal to reality new mic money as i said i just need to figure out why this computer will not connect to the mic i already have which worked fine uh roland old mic money thank you roland jake up with this with coven against australian tga doc released submitted january 2021 up fiza data released by foia no info spiked degrade circulation potential autoimmune disease noted no no study lipid nano well i i'll have to i i don't know what you expect of me i'd have to look and and find what it is and then comment on it all right submitted january 2021 come on guys um michael i had a professor challenge me that's saying fee will is self-evident because we see it like saying the earth is flat is self-evident because we see it what is wrong with this analogy well first of all you don't see those as flat um if you if you uh it doesn't take much uh even through vision this is how the greeks understood the world was not flat you know you can see the horizon you can see the ship going over horizon and you can tell that the earth is not flat just by pretty pretty simply um there are illusions but your senses give you what exists out there indeed for all intents and purposes your little piece of the earth is flat um it's it's you know what you suspect in what you see is true now as as um as you gain knowledge about the world you expand the context of what you're seeing you expand the the understanding but this is the this is the difference free will stands at the base of all knowledge that is there is no thinking without free will there is no reason without free will there is no the professor challenging free will without free will in order to refute the idea free will one has to refute free will what one has to use free will so uh it's it's it's very existence a is observable and b once it once it isn't there there's just um if there's no free will then then there's no knowledge and there's no reason and there's no thinking and and there's no correcting because it just is what it is um it's probably a better way to phrase my answer for that um i mean i i highly recommend asking you that question michael for when we have greek salamiri on the show on call one of the one of the philosophers um and i money thanks for making sense thanks for appreciate it uh doc fox says do you know of the academic agent neema pavini he's an intellectual lynchpin for the right making a video countering his arguments which sway his less extreme let me uh let me let me copy paste this his book is popular's delusion um yeah that could be interesting i'm looking for videos stuff like that to do so thank you uh for you for for sending that i'll look i'll look him up i do not know him right now palo says tips to people on how to keep up with modern tech well depends what you mean um by how to keep up with modern tech i mean first the first thing is to be curious uh get be engaged or in chat gpt comes out or you can download or you can play around with it play around with it but look there the point of and it depends on how old you are and and if you're doing this in order to figure out uh career wise if you're doing it for fun um but just be engaged just read up about it test it try it download it uh think about it think about its implication for your own career and your own job uh but read read read read read read there's no you know if you're if you're 25 then read and and experiment and try right don't let technology pass you over i mean i i'm i'm uh almost 62 and i can't afford to let technology pass me over though there's some technologies i obviously uh don't go near but uh but don't let it go over you uh read about it and then and then the main thing is test it try it explore experiment engage in it right uh the future is yours you're 25 the future is technology you better be whatever your profession is whatever you're going to do in the future the future for you is technology so invest some time in understanding it in embracing it in making it a part of you so uh and the best way to do that is to use it is to use it and see how it applies um all right thank you everybody again i apologize for the tech problems um by the time that well the next show is while i'm on the road so that's a whole different set of equipment whole different set of problems um but um uh i will i will probably do a show tomorrow from medellin in columbia uh and i'll let you know how that goes uh let's see what else do i need to update you yes and by the time i get back home i will have fixed this i might be able to fix this somebody said reboot the system and that's exactly what i'm going to do i'm going to be able to fix this in the next few minutes uh by by doing that all right thanks everybody i will see you all in uh tomorrow from from columbia uh thanks for being patient with me i with me i really


Hello, we are the conference team from Spain 2020. As you all know, the present circumstances worldwide force us to take this terrible, sad and tough decision of rescheduling the conference to 2021! Same city, same team, different year. Until then, please take care, be safe, stay connected. Spain 2021, because good things are worth waiting for. Woohoo! See you next year!


Right now It is my pleasure to announce we are joined by an esteemed partner of ours at fan toll Halva gambler follow all of her stuff on all of her socials at Aaron K. Dolan. Welcome to hammer down. How are you today? Great. How are you? Thank you so much for having me on. Hey, it is our pleasure and I don't want to start this off on a bad note and I know it's not your fault, but Will you talk to somebody over there at our partner Fandall? Sportsbook that we none of us got invited to Denver for the Fandall fan.  I know hopefully we'll be having we're having more in the future So we'll have to get you guys on the invitee list. It looked incredible. I know it's not your fault But I was severely good word though. Thank you. I appreciate it. Some of us were severely disappointed How's your time at Fandall been? It's been so much fun. I started in January So unfortunately, I didn't get to do all of last football season with them But this season we're gearing up so everything's been a lot of fun. You guys have a much cooler studio I'll say those you can see I saw my key is stuff working from home. So everything's been good though I absolutely love working. No, no, your studio looks great. Our studio is pretty cool though I appreciate the compliment jealous So are you you just talked about football season? Are you? Like as NFL what you're focusing on most right now Yeah, for sure I mean, obviously we have college football going on But I've come to the realization that you just can't be a good better and everything so you got to hone in So I feel like NFL and NBA are my two things that I love to bet on. Hey, that's very very good advice We normally ask people when they come on here what their advice is and what we always say is bet on what you know Is most likely the best idea? So so for this upcoming NFL season NFL week one a whole are you have you done a bunch of a futures bets? So I have like futures bets in mind that I would be placing Okay, general I stay away from futures bets just because I don't want to tie up my money because I'd rather just bet every single game If I get on Sunday But I guess you could do both but if I was good about anybody it definitely be the Packers 12 to 1 Okay, I think they're gonna be able to get it done this season finally I feel bad for Aaron Rodgers. He's got all these issues going on Of course in this offseason with all the drama, but hold Bonte Adams back And I feel like they still have all the pieces he obviously played unbelievable last year as long as they just don't Up to kick a field goal will be exactly. I agree Aaron's a big Big friend of this office and I think most of the people in this office agree with that Maybe if not Tom then Aaron for sure definitely Does that mean you're going with Aaron then for MVP back-to-back or no No, no, no, I actually have a dark horse and I I said this out loud to people at Fandall and they were like Aaron I don't know about this. I feel like we shouldn't broadcast this and I was like no we are I want to go with Baker Mayfield It's a dark horse 26 to 1. I know it's it's a long shot there But I think considering how well you played last season I know he's had ups and downs in his career, but I like the value there And I think if he has a great regular season he could absolutely win I don't know if when we call people you could see me or you see yourself. I can see you Yeah, so No, no, I'm kidding. I actually Took the browns. I like to separate my fandom from my bedding. I don't Need it. Hey our producer mitt. He doesn't either and I respect him No, I don't respect him at all, but I respect you doing it Are you are you from Philly then do you take the Eagles all the time or no? Yeah, well, I'm from Philly, but I'm smart enough to not bet on Philly teams Like I just stay away from them, but like I'm going to be that type of fan like I would never bet on the Cowboys I like that. Yeah, I like that a lot even though like I just said mitt is a huge Cowboys fan But he's also a Yankees fan He's not a real fan. He's also a Yankees fan and a Lakers fan, so he's the worst human on the earth People can go and like like different teams from different areas. I feel like where you're from It's just like you're born into it. And that's just the cards you drew I agree, but his dad's a coach and he's moved around a bunch of areas, so we give him a break But what I was talking about I did take the Browns to win the AFC North I put my I put my fandom aside. I don't like the Ravens this year And I'm not gonna jinx the Steelers. I refuse to do that Do you have do you did you also take them if you like Baker to win the MVP? Do you like them to win the North? Yeah, for sure a plus 155 I would definitely take them. I'm on the same bandwagon with you I think the Ravens are finally gonna see regression I feel like Blumar Jackson has not proven to us that he can do anything in the bow season But despite all that I do think the Browns just given I mean you have cream hunt Nick Chubb Odell Beckham juniors coming back their coach has been great obviously With Baker Mayfield, so I feel like you can definitely bet into that market still compared to some of the other divisions And a plus 155 I feel like you should take that now also given the Browns of one of the easiest schedules based on wind totals So that helps them they do I may even now that I'm thinking about it since they have the chiefs week one and potentially lose to the chiefs week one Those odds may even get better After actually after week one, so I'm just I'm just sorry. I'm just thinking out loud I may potentially wait until after week one and do that. Thanks for that That's the thing with futures. I feel like you do have to wait some of this out. Yeah, absolutely like and I thank you for putting that in my head I appreciate that Speaking of your Eagles and the NFC East did you take a division pick on that one since you're familiar with it? So I almost feel that since it's so unpredictable and I can't I can't come on here and say take the Eagles I don't have a specific pick I'm more interested to see what you would take just because the odds are so long right now I would never bet on the Cowboys. I don't think the Washington football team will get it done again No team has won back to back regional title since 2004 I don't see the Washington football team being able to do that But then again granted you only needed seven wins to win last season and then I'm out on the Giants so I honestly feel like given the Eagles have the longest odds as A better and also as a fan in a way I feel like I would take them just for fun, but I was interested to see what you would do in this market. So I Know the stat. I know that no team has won back-to-back years and in all of those years I don't trust the Cowboys at all. I don't part of me doesn't trust Dax Not only I like Dak I don't know if I trust him to stay healthy and their defense was the worst last year So we'll see how that goes. I'm not gonna take the Eagles yet. I Don't trust Daniel Dimes and the New York football Giants.  Listen, uh, it's not so much Ryan Fitzpatrick because Everybody loves Fitz magic. We I do too as someone in the bearded community But I think it's more of the defense I think that I think I love their defense. So in that division a Lot of tight games. I think Fitz magic will do enough. So I was thinking about the Washington football team there Were you doing did you do any other division winners or anything like that? The only other one I feel like you can bet in is the AFC South which to me I would definitely go with the Titans minus 110 right now I just think that I can't bet ever bet on the Colts because I'm such a Carson ones hater And I know that other people on the show are very Excited about the Colts always But yeah, I just I cannot get behind the Colts. Listen, I also I didn't take the Colts either I also took the Titans just because We know who the Titans are and we have no idea if Carson Wentz We have no idea if you can be good. I have an idea. Well, no, I know you have But I'm saying there's a chance that he's still that guy. There's a there's a chance that he never goes back to 2017 and if the Titans start winning it's going to be like minus 150 after week one same eyes We'll take a minus one very very true Colts have Seattle I believe week one at home and they've had a bunch of issues and stuff like that Have you started looking at week one at all?  Yeah, sorry. No, no, it's fine So you could you think you could trust Joey Barrow week one Yes, I do the Vikings play so well at home and considering they're going on the road And I just feel like the first two weeks betting NFL is so difficult So you might as well just take some of the underdogs when you can especially when it's a short line anyways EKD, can I call you EKD? Yeah, a lot of people call me that. Okay, cool. It's just easier I think we could be friends because I'm also I'd also love taking the puppies and I like taking unders A lot of people have problems with the under. Do you have a problem with the under? I? Don't have a problem with the under but just in general I stay away from totals when I I mean It's just like not fun like you want to bet the over but then if you go to the under You're just you don't seem fun and then if it doesn't hit it's just I feel like it's so 50-50 on those That it's not fun for me. I won't take that as a shot at me. That's fine Hey Can't thank you enough for coming on Please make sure you tell those people over there to invite us to the next fan fest Good luck this weekend. You doing any college? Are you taking any college at all? Any I'm going with uh, this is so bad I should not broadcast this because I graduated from Penn State, but I was you tonight minus 13 and a half Oh, wow. No, you're okay. You're loud Happy values a good time. Happy values good time. It is a good time Can't thank you enough for coming on good luck this weekend. Good luck next weekend. Come back on anytime and thank you for coming on Yeah, of course. Thanks for having me. Thank you, Erin Erin Dolan here. Thanks for watching and make sure you click below on that subscribe button for more great Fando content and check out some of our latest uploads and playlists right over here


Hey this is Jonathan from AJ and Smart and the video you're about to see is a Q&A that I did with Jake Knapp, he's the author of Sprint and we were talking about, we were answering a question about user research and it kind of went down deeper into the whole topic of user research even though we were first focusing on the design sprint itself. So the video you're about to see is from the Design Sprint Masterclass, it's an online course that we have and we're just taking a few snippets out of it and putting it on YouTube so that you don't have to you know pay to see a lot of it and yeah if you like it below there's a link to watch a one hour 20 minutes web class where we go deep into you know how to sell the design sprint, how to run design sprints all that kind of stuff so you can see that in the link below and yeah enjoy the Q&A. Hey welcome back to the Q&A part of this course where I'm standing here with Jake Knapp and we're gonna be just answering your questions that you've been pumping into the Facebook group for the last few months and we've got a great one, we've got a doozy. Okay let's have it, let's have it. Okay Andre asks and I'm gonna set the scene, I'm gonna set the scene, I'm just gonna read his question. Paint a picture. You're going into the design sprint okay you're going into the design sprint with a new client. That was the opening of the door, it's a creaky door. It's a very creaky door. You shouldn't have creaky doors, you shouldn't have creaky doors in the design sprint room. You're going to the design sprint whether it's with a client or an internal team and the internal team has a lot of biases on what they want to do on what they think the sprint should be and what they think the product should be but they've done no user research at all. It's all based on their own biases. Okay okay sure. What what do you think about that? Well because in design thinking that would be kind of a no-go. Kind of a yeah kind of a non-starter yeah so this is a this is a really good question and it's it's tough because if you do research before you come into the sprint you will always be ahead like you're always going to be ahead of a team who hasn't had a chance to do research. You're going to know more about your customers you're going to be I think of it almost as like you've already done a sprint if you've done research ahead of time and you're able to present it effectively and the team believes it. Now that's an important question because for many teams actually if they don't already believe in research you may not be able to just convince them like this is the right way to do listen to us so part of the idea with the sprint is it's a trojan horse for research. At the end of the week the team even a team who's totally averse to research will be really hooked on the idea of learning whether their prototype whether their solution works and they're going to see their customers react to it and their like research is going to happen by the time the week is over but there's this sort of bigger question about whether like where good ideas come from where do good businesses come from good you know sort of innovative products if you like where do they come from like do they come from doing exhaustive customer research talking to people and sort of discovering what their needs are and you know sort of empathizing with them or whatever or do they come from the insights that that you know people in business have you know they the way the workers or the folks on the team are thinking about the problem and you know I I want to say that they come from doing research and from really understanding customers but I think quite often they actually come from people just having an insight you know someone who knows a lot about a technology saying I think there's something really cool we could do with this technology and I think we should do it and you know a lot of those ideas fail a lot of those like technology driven or business driven ideas they do fail but I think that what where the magic really happens and if you look at the products that we all use every day the products that are success stories what happened was somebody had an insight and then they were able to figure out how to take that idea about a technology or a new business model or a new service model and then they were able to figure out how to really make it fit well with the customer they're able to sort of build a bridge from this this this crazy idea that they had this sort of brute force maybe this wasn't like something that really made sense to people right away and then they figured out how to make it make sense to people and maybe they had to like change the way people actually behaved and the way people operated like I think Airbnb is a really good example of this you know and those are designers who started that company they had this idea about this home-sharing thing that honestly like when I first heard about it it sounded a bit creepy you know I mean it's like you're going to be staying in somebody's place and like they had to sort of also change people's expectations in the world they had to figure out how to build that bridge and and they did it by taking their crazy idea you know and and their sort of insight into the business into the service what was capable with what was possible with technology and then they like figured out how do we make this fit the customer but it's like the insight or the inspiration or the opportunity first and then figuring out how do we make this fit not every insight will even be possible to fit to people and it's not to say that I'm sure there are stories where people just started with exhaustive discovery research and then came up with something but I don't know those stories the stories that we all like the products that we all know the businesses were so successful they started the other way so in a sprint I'm okay with starting with the company's insights and then seeing what happens yeah I think that's a great thing about the sprint you can start with a lot of assumptions and those assumptions are going to be challenged on the user testing day anyway and it is true I think like there's if there's some context that people need about around user research large companies let's say like a company like Slap today they wouldn't have started with user research but today when they want to tweak little things and they want to do like small tweaks to the like conversion funnel or they want to add new features today when they're already established that's when they start building personas that's when they start going a little bit deeper into user research but often at the start it is personas let's not but that's when they really start doing research and really trying to figure these things out the same with Netflix they don't they don't start with that like companies think they do but this kind of kind of almost like misinformation spreads around from these companies because they show that they do these processes and people think they did them at the start that's right yeah yeah and I think you know it's also there's look there's this I don't want us to be coming down too hard on like design in general because of course like we we think those those things are important it's important to know your customers it's important to do product work that fits your customers lives it really does matter I think that the there's just sort of this philosophical approach about whether you try to convince the team that there's a sort of golden perfect way to know your customer and like we must do like our design and our research this way or whether you try to help your team and I think that the I mean the design sprint my standpoint was I had I had tried in the past before doing this to like figure out what the golden way to do design was and I sometimes try to convince people look this is the right way to do it we should do it this way you know you should feel guilty if you're not doing it right but the reality is I don't know that there is a golden way instead besides the design sprint size of design in a design sprint you're you're really just trying to be helpful it's like look whatever you're trying to accomplish team and that might be that you are dead set on this one solution the design sprint is going to try to help you get there now along the way it's going to turn out that you're going to do a lot of design work you're going to consider carefully different viewpoints within your team you're going to put it in front of customers and you're going to find out really quickly if that's actually something people care about you're going to do all those things that as as designers we often want to do those things will happen but they're not going to happen in a way where you're trying to like convince somebody like force them down like just like you know ram through your your vision or make people feel guilty instead you're going to be helpful you're going to be helping them along the way so you'll take their energy and their enthusiasm for their solution you'll help them perhaps they'll be right if not you'll have shown them a way to learn and I think that's what it's all about to me that's a better way and a more fun way to work together great great answer Jake oh oh thanks that was amazing thanks hope you're enjoying the course see you later see ya so welcome back I hope you enjoyed that video um it got a bit uh I'm sure there's going to be a little bit of controversy I'd love to know what you think about user research um maybe not just related to the sprint but just do you think uh do you think products need user research especially new products or do you think that it's going to kind of make them a little bit too vanilla or do you think it's just like extra work that doesn't need to be done I'd love to know that in the comments so I hope you liked it give it a like if you enjoyed it um subscribe if you haven't already and as I said earlier there's a link the first link below is to a one hour 20 minute web class where I go through pretty much every little thing about why we as AJ and smart got into the design sprint and um you know tips on how to run it tips on how to sell design sprints if you're interested in that um but yeah that's it have a good one bye bye