 density plastic flow, not a regular low density flow, but this is a solid density flow to astrophysical plasma flows. We use high energy lasers to study hydrodynamic instabilities and material, mixing or interpenetrating in three very unique regimes. So I will talk about three experiments today. We do a lot more experiments, but three experiments today. One is Rayleigh-Taylor instability and mixing in a solid state, I'm sorry, let me try to get used to it with a remote, flows relevant to planetary formation and a meteor impact dynamics. Basically we are using Rayleigh-Taylor instability to study the material strikes. Second topic of today is radiative shock stabilized Rayleigh- Taylor instability, which may be relevant to supernova dynamics. This is the two dissemination of such a case. Top is Rayleigh-Taylor instability under very high radiation environment versus the classical Rayleigh-Taylor environment. You can see the Rayleigh-Taylor is very much suppressed under high radiation environment. So we try to verify whether this is the case or not an experiment. The third case is actually plasma interpenetrating cases. That is the Weibull instability mediated plasma mixing in high velocity interpenetrating plasma flows, which is relevant to astrophysical collision shock formation. This is the 3D simulation of the magnetic field map when the two plasma flows go each other and creating these Weibull instabilities and as well as magnetic field. As you can see, this is a very turbulent nature and it's been seen and we are trying to experimentally verify this is the case or not. So we use the omega and a nip laser to do this high energy density experiments. Omega laser is in the University of Rochester, New York, USA. It has a 60 beams of the laser converging into the spherical geometry, which is about three millimeters of diameter of the target chamber. It has up to about 30 kilojoules of the laser. Right next to it is omega EP, which is the four different beam facility, same size of the target chamber of the three meter and it has about five kilojoules of the laser. But two of the disbeam can turn into short burst laser, which is up to 10 to the 20 watts per square centimeter of intensity. So that's a very unique. Now we do the experiments on the National Ignition Facility, which is located in Lawrence Livermore National Laboratory in California. We have 192 beams creating about up to two megajoules of the laser energy in three omega converging into the 10-meter target chamber. These pictures are not really scaled. Actually, the laser bay alone is a three foot board period and to create the two megajoules of the laser. So this facility has been operation since about 2009 and we've been doing the target physics experiments. So the first topic is the strengths. Rayleigh Taylor instability and mixing in solid state plastic flow can be used to infer mature strengths. So what's the mature strengths to give you just a definition of a strength? Strength is the resistance to deformation. So when you apply the shear stress onto the mature, the mature experiences the resistance against this stress and that can be defined as a strain, which is the deformation amount over the unit length. So strong means that small deformation for a large applied shear stress. And this is a macroscopic phenomena, but then you can go back down to the very fundamental unit of the microscopic view, which is there's a dislocations and then they try to glide along the lattice plane and how well they play, basically their generation, how many of them are there are versus and how fast do they move can determine the mature strengths. So we are trying to determine all these are mature strengths are using high power lasers. Let's go to the next slide. And of course, there are many models, of course, just like any of the theory and models exist, but the strengths cases are more of the phenomenological model and very little known is a high pressure and a high strain rate cases. So there is a typical of the parameters of pressure and a temperature and a strain rates. And there is a conventional model of a Steinberg-Geinen and PTW models exist, but they are basically experimental mockup and then they try to fit the experimental parameters at the low pressure. These days, we developed a new model called the LMS of multiscale model, which starts with a fundamental atomic equation of a state and a potential and then get into the dislocation mobility and then getting into the dislocation dynamics and then getting into the continuum methods. And then all these things were basically physics based and no really phenomenological model, but all these models are known at the very low pressure and a low strain rate, but then we wanted to get into the high pressure and high strain rate. So that's where the laser experiments come in. Laser experiments can reach high pressure, basically. Just like Hopkins bar, they are very low pressure. So we started this experiment on omega and a NIF using Rayleigh Taylor instability properties to infer dynamic flow stress. So as you can see, probably in this community, it's very familiar with Rayleigh Taylor instability. In a classical, there's a low density goes to the high density and then classical growth is well defined by Rayleigh Taylor equation. However, if this material happened to have a strength, then it would be the Rayleigh Taylor growth would be suppressed. So we are designing this experiment with a pre-imposed sine wave and then we try to measure the growth amount by the radiography technique. And this is the one example. Basically, we give a very thin x-ray source and I try to measure the growth amount of the, just in this case, was a tantalum sample, which is in a solid state. So that's how our experiment works. And then this is actually a NIF experiment configuration, which is sitting in a hole of the 10 millimeter by 13 millimeter. Target represented is mounted on the side of the package. The whole thing is a 40 millimeter, which is quite small. But then this hole is driven with up to about 200 kilojoules of the laser energy. And we accelerate the sample. We try to measure the growth amount of this sample by x-ray radiography technique. So this is how our entire analysis works. This is actually our set of the data. The rippers are made on a tantalum sample. In this case, we prescribe different recipes trying to induce the more information. We have the knife edge trying to measure the spatial resolution. We have steps on the sample trying to calibrate our radiometric unit into the absolute height. And then we also measure the initial sample before it goes. And then we come up with what we call a growth factor, which is a driven ripper amount over the initial amount over the spatial resolution. And we've been conducting this experiment on both omega and NIF. And then we measure, we call it growth factor. This is the omega condition at the peak pressure of the 1.3, 130 gigapascals, which is 1.3 megabar. And then as you can see, our measurement is very suppressed compared to the standard Rayleigh Taylor growth amount. And then, of course, there are many different models, which is lots of acronym here, Steinberg-Geinen. That's the people's name. PTW is President Tank Wallace, Steinberg-Lundmatter. And LMS model is the one I described from the fundamental way of describing the strengths. Our data happened to match LMS model very well. And then now we begin to the experiment on doing at the NIF. This is the first results from the 3.5 megabar case. And then again, we compare our measurements with the different no strengths case versus many different models again. And right now, our conclusion is that our data actually matches with the LMS model of 3.5 megabar peak pressure in both cases. And so this is actually quite amazing because the material behaves very strong under a high pressure and a high strain rate. Now, this community, I put together these slides because how can I, what does this mean? What is all this model means? So let's think of this as our plant, the tantalum material, which is solely the matter, is a very viscous material. Can we explain this one as a lettuce of viscosity? So instead of the regular standard Rayleigh-Taylor growth factor, we introduce over this viscosity term, which can be expressed in this formula. And this theory is developed by Karnic-Michaelian. And then we measure our growth factor in this expression way. And then we try to see where our data fits in dispersive curves. And then I turned out our data fits in 25 poise, which is an incredibly strong viscous material because you name it like a water is a 10 to the minus 6 poise. So 2,500 poise meaning the material behaves incredibly strong under high pressure and high strain rate. So that's a very, very exciting results. And then a vanadium was also showing very similar results. So this was our material strength experiment. Now the second category is whether we can probe the Rayleigh-Taylor instability properties to understand the Schupanova mechanism. So most of the Schupanova mechanism, basically the Schupanova explodes. And then the shock goes away in the front. But then there is an interface between the high density to the low density, which can create a Rayleigh-Taylor instability medium. So far all the state of media never includes the strength effect here. And then all radiation stabilization effect because the radiation goes in front of it and makes a really hot media in front of it. And does it cause whether there is instability, reduces this Rayleigh-Taylor instability. So we started doing this Schupanova Rayleigh-Taylor experiment. And this will be important to understanding the observation and then evolution of the Schupanova. So our experiment basically trying to create the mimic of the radiation environment in front of the Rayleigh-Taylor unstable interface. So our experiment design is that we have the, we use the laser to create the high radiation environment. And then our shock tube has the heating medium, which is the foam medium. And then we have the referred surface. And then we drive and at a certain time later, and then we use the backlighter trying to see how this ripper grows under two different cases. One is that we call it high drive, very high radiation temperature case versus a low drive, which is the cold medium places. And then trying to see whether this ripper grows a matter at all. And then we have done this experiment on nips. And then the prediction is that we created a two different environment of the radiation temperature case of the 325 Eb to 200 Eb. And then you can see the simulation shows that at the high drive, the Rayleigh-Taylor growth is very much suppressed compared to the cold drive, which is the suppression amount is not visible. So the question now in this case is what is the actual mechanism having this Rayleigh-Taylor suppression is happening. And there is two theories happening. One is, oh, so we went on and did the experiment. And this one is the low drive, which is a relatively low temperature case. And then you can see this is a shock front. And then a shock front moves along as function of time. And then you can see it's a little low contrast, but then you can see the ripper growth. And then the ripper growth as function of time and then it goes really growing. And then high drive, which is the same inner phase of position. And then you can see even by your eye, the growth amount is already quite suppressed, meaning that it doesn't grow like this mushroom kind of a futures. And then it's much smaller. So the next slide shows this one much closer up look. And this is the data at the low drive, meaning there's no radiation is happening in the front of this rippers. And then it grows much higher compared to the data of the high temperature of a cylinder degree. And then we compare it with a crash. So we're trying to understand this phenomenon in terms of two ways. Basically, see what type of a Rayleigh Taylor separation mechanism can happen. So for this experiment, we are coming up with two ways. One is that ablation stabilization. Basically, what's happening is it could be, it could have a very, very high temperature in front of it. And that makes it basically, the ablation happens very fast. And then it cannot suppress the growth. It can make it look like a smaller growth. Or basically density scaling stabilization. That means we have, in this case, we have a different density. The density is much lower. So at wood number, in this case, is much smaller. So it looks like it grows as a last. So we are in the middle of trying to compare of these theories of the two different mechanisms of the stabilization of the Rayleigh Taylor growth. And trying to do the simulation and theory. And so far, our understanding is ablative stabilization is a more dominating factor. And so here is the case of showing you that in front of our ripper growth, there's a high temperature is happening. And that will suppress our Rayleigh Taylor growth. So we are preparing, one paper is already accepted and by nature communication. And we are preparing another one in a more detailed describing this phenomena. Okay. So the remaining hour, my third topic is collision as shocks. So the height mark number plasma flow mixing is interest to astroputical community. Basically, if you look at the, sorry, sorry, this one is going on many different ways. So we are interested in basically plasma flow mixing, how that controls the collision is a shock formation. And whether they turning into the turbulent mechanism and how that creates the magnetic field in the universe. So if you look at the universe, the first of all, everybody knows that universe has a very strong magnetic fields everywhere. Sorry, I'm pushing, keep pushing the wrong buttons. So if you look at the M31 Milky Way, there is a magnetic field in core to the micro, micro Tesla to all the way very, very small amount of a magnetic field. So the question is how these are magnetic fields even generated? And another question in the universe is we know that cosmic ray particles can be accelerated really up to high energy. And then the big question is how does the cosmic rays are being accelerated? So the idea is that maybe there's some kind of explosion happens in a plasma flows and then it creates the instability that traps the ions and then that can be the mechanism of the creation of the shocks and then also acceleration of the particles. So this is explaining that if you have a very high speed of plasmas each other and then their interaction length, which is the cool or mean pre-pass is much, much larger than they actually trying to meet each other and create a shock. However, just like it's a very analogy. I know this community is very familiar with Rayleigh Taylor instability. Rayleigh Taylor instability is basically you have density, density differences. Whereas in this case it's a velocity differences. Two different velocities also can create different instability and that's called a Weibull instability. And then the unique about this Weibull instability is so they should go through. They are very, very, very fast moving plasma flows, but then they can create an instability and then that traps the these ions are moving together. And unique thing about this one is Rayleigh Taylor instability makes this Weibull growth and different spikes and bubbles. And in this case it can create basically a magnetic field out of kinetic energy. So that's a very unique thing about this phenomena. And we wanted to study this one. And of course laser is really great because we can laser is the platform. You can create very high velocity plasma flows. So we are trying to make a scale experiment. So if you look at another phenomenon, if you look at the Schuphernauva and Schuphernauva expands the plasma very, very high speed. And then as I said, in a regular theory, this plasma should just move on and then there should be nothing. However, we see these are basically shock is formed, very, very thin shock is formed. So how do we understand that this type of a phenomenon in laboratory? And then you look at the Schuphernauva system, what happens is that the Coulomb mean pre-pass because of this Schuphernau explosion is a so power event, which is a scale of about 40 light years, which is much, much larger than the system size, which is the Schuphernauva size, which he and then now we are seeing basically the shock width created by this system is very, very small. So when you look at this one into the laboratory plasma physics, basically Coulomb mean pre-pass, how they penetrate, they pass through, it has to be much larger than the system, which is my experimenter scale size, should be much larger than this instability scale length, which is in our case, we have electrostatic instability lengths, and we have an electromagnetic static scale length. So if we can create this type of environment, and we have basically a scale experiment on how we can create this collision as a shock in a laboratory. So we began this experiment on Omega first, which we have about 4 to 5 kilojoules on a simple plastic force, and then plasma is creating about 10 to the 9 kilometers per second of the flow velocity, and then in the mirror is our probing region. And then we first we had to demonstrate that condition I explained that the mean pre-pass should be much larger than our system size, which is about 9 millimeter size, which has to be much, much larger than our plasma instability scale length, which is the frequency, the instability frequency length. So once we demonstrate that the mean pre-pass is much larger than our interaction system size, which is much larger than our instability scale length. So once we demonstrated that, we went in and started doing what's happening on our actual instability cases. So we have two flows coming in, and then we decided this is electromagnetic nature of our unstable, so it's not the actual density of it. So we use proton source to probe what's happening in our electromagnetic scale length. So this is the image of a time sequence of the very early time, and then time evolves, and then you can see that very turbulent nature is very clearly visible at very late time. In the beginning, that's the arrival, and then it creates, it evolves and develops more, and then it goes on more. So with this, and then we are saying that basically, this is so clear, the viral fermentation was predicted about 1950s, and then our set of the experiment was the first experiment that clearly demonstrated the viral filaments actually exists. So we accumulate these filaments, and then we measure basically the conversion from kinetic energy to the magnetic energy is about 1% level, which is quite significant. So that's how the universe is magnetized. So if you see the Schuphernau explosion, and then there's magnetic fields exist everywhere, and then basically the most fundamental mechanism how it creates from kinetic energy to the magnetic mechanism we think is a viral mechanism, and then we demonstrated in the laboratory. So that's the viral civility, and then now we wanted to really create the shock. So we began our experiment on omega, and this was the omega case, and then now on NIF, I'm sorry, on omega we used about four kilojoules of the laser on each four, but on NIF now we can afford to much larger laser energy, 250 kilojoules each, and then now we use the same trick of probing our interaction region with the D-Helium-3 backlighter in terms of a proton, and what is there? So the D-Helium-3 backlighter generates the high energy protons and low energy protons, and this is an example of the map, but to give you our quick summary, this is the summary as of today as how proton radiography looks like a proton radiography, don't think it's like a density, think this is like a magnetic field map, how they are evolving when the plasma and plasma interacts, and then at early time we see the very two distinctive futures which we think that's the Birman battery created from the target surface, and then it evolves, and then later the field gets much stronger, and then eventually all the basically because of the field is so strong, and then we consider this is a possible indication of the shock formation, and we by comparing this one because of my length of this presentation, I didn't include all the simulation, but we think the B field strength is about 3 to 5 mega-gals at the saturation, and then at the end probably filaments merge, and then shock is formed. We have a couple of papers published, and then one is in preparation. So to show you what's actually happening, and this is a 3D peak simulation, particle in-send simulation, where we use the two flows, the two plasma flows coming from each end, and then the plasma density and the velocity is from our experimental measurements, and then the top is the basically plasma density plot, which is how much is over the initial, the bottom map is actually the magnetic field generated by two plasma flow interaction. As you can see the shock is being formed like about three or four times of the initial density, and the magnetic field as you can see this one in the beginning, it's a very nice and a wider kind of simulation, but they develop more and then turning into more turbulent region, and which is the title of this conference. So there is not only just a density turbulence which is a lot about the Rayleigh Taylor, but this is more of the magnetic field turbulence being created, and then you can imagine this magnetic field can do a lot of damage harm on the universal objects. So this experiment is happening. Now, so more relevant to this conference is now density, I'm sorry, density case, sorry. So we not only measuring the proton radiography, we also use the Thompson scaring to understand the actual density, ion density, and an electron density evolution. So we have done a series of the experiments. This is for the people who don't know, I don't have time to go over the details of the Thompson scaring, but Thompson scaring measures the scattering of the electrons and a scattering of the ions, and then by their original wavelength shift amount, we can come up with an electron density, ion density, and an ion temperature, and a velocity. So this case is time-reserving. The dispersion curve means the velocity, and then when early time, they look like nice and smooth. But then the later time, Thompson scaring breaks, and it looks like they are going back and forth between two flows. So this is one flow coming from one side, and this one is the other flow coming in, but they are just basically making a flashing between the density. So this was a very curious thing to do. So we went on and did another experiment, and an imaging Thompson scaring, and this is the target, and as you can see, it's evolving quite a bit. So there's a lot of turbulence going on this, even a plasma interactions, and which was quite exciting results. So I will conclude my talk that we have conducted high-power laser experiments to provide an exciting to provide energy density regime. I just explained only three cases, which was the material strength under high pressure and under high strain rate. It shows a very heavy viscous of plastic flow. Second experiment was the effect of radiation on the supernova instability growth case indicates that the radiated instability can be suppressed under the influence of the relative stabilization. That's what we are still doing more analysis, and so we concluded with a more dominating ovulation versus the density gradient. But that is a significant effect that we show that radiation matters on the Rayleigh Taylor growth. I showed you now a completely different regime of the plasma-plasma turbulent mixing cases, and this is a very important observation, and we are doing the laboratory experiments to tie together some important astronomical phenomena, such as shock formation and particle acceleration. And I just covered only three, but our laser facilities are so broad, and then there are many other experiments that are going on, and relevant to this conference's topic, we are studying the effect of a reshock, we are studying of the multimodes, we are studying the bubble mergers in a non-linear regime. So it's a very, very rich area doing the experiments of studying the turbulent phenomena in both the materials and the shocks. The next one will be by Bruce Remington, and then how great is our ICEP application of this one. So thank you.