I'm going to talk about extreme field visits, uh, using, uh, Power Blazers and activities.
And this was back many years, and Bill Scott there, that's just come into the.
Reminds me of some of the work that we did when we were working the fundamental physics. So we had this set of fundamental physics. We would discuss some of these.
I outlined each ideas, um, that seemed to be so far in the future that we've never actually achieved anything. But now, um, I'll show you that we're now, uh, knocking on the door of some of the interesting fancy.
And before doing so, I'd like to just, um. Acknowledge all the people that I've worked with, um, on, uh, the various topics I'm going to be talking about.
And I'll make mention to Jack Paragie, who's, uh. He's in the audience just now, and he'll get this straight when it's, uh, when I've got the butler. We'll talk some more about lasers than I do.
John Lucid Gagori is also, um. Key to this, because he was one that… key founders of some of the experiments that we've, um, proposed, actually. And Ava Moss is now leading up.
Some of the experiments you were working on. A lot of the work has been taken from some of the students that plan over the.
Last, uh, few years. And so, um. A lot of it, it's due to them as well, so I'll talk about them and what they did, but what I'll talk about, initially, is what is extreme physics, and.
Um, what you would think we did get forced to do it using, say, high-powered photon beams that are coming out of these, um.
We've built things that are being built. So you… and a lot of, um… inconvenience. You're told to go home, etc. The buildings have been closed down because they're changing.
However, things like that, or the internet's not working. And that's all because, um, EPAC.
Invoked in 2020. We've seen big calls out here. Uh, that's for Volpi 2020. Epac's finished, and it's out.
It's rolled some of the car park space that you used to park in, and it's now there. It's now… Um, you could do that with lasers, and those lasers, actually, will probably be up and running.
Uh, next year. Hopefully, we'll be able to look at the lasers, um, in a year's time, come back to some of these problems.
First of all, let me talk about the peer plasma experiment that we've been doing at, um.
At SIM, as well. Then I'll go into photon-photon scattering, something that Bill Scott and I looked at many, many years ago.
Put an IPN coupling, it's a new thing that, um, we've been starting to look at, and then.
For some gravitational wave coupling. Which is more or less very similar to the photon vaccine, and then this plasma material coupling, they're all very similar. The equations, basically.
Our identity. So what you solve, one solved them all. And so, uh, I'll just explain that as we go through. So, what is Strongfield? Well, strong fields can be found in astrophysics, and probably one of the, uh, strong examples of that is these, uh, magnetars.
A little bit, um, magnetic fields that are about 10 to the 14 Gauss, and that's, uh, very, um, near the Schwarner limit. So we're generating.
Very large amount of selection plasmas in these fields of the star itself.
And so, we're looking at, um… the ability to be able to generate election positive on payers, i.e, we're looking at vacuum fields, we're looking at physics of the vacuum, basically, using these high power lasers. And this is an example of, say.
Magnetic fields in astrophysit. Now, I did mention photon-photon scattered. Now, I know that, uh, you guys in CERM.
How protected photon-photons happen, but you've used it using collisions between, um.
Crouton beans, that the elements see. The electromagnetic fields, the virtual particles that are generating as you climb the particles together, are actually scattering photons. Now, that's.
A very intense environment. I'm going to show you some experiments that we.
Proposing that haven't been done yet, but proposing to do that are probably not as intense, but in a much more controllable.
A much more, um, amenable, uh. Environment where you can actually stand next to the experiment.
Um, and fiddle around with it. Gamma-ray versus another area where you get very high yields.
And you also get very strong fuels and plasmas, and these are the first papers.
We were produced to show that we could actually get very intense fields by colliding, say, two laser beams. I'll talk about the intensity in a minute, and you're.
Thank you, uh, production of electric post frontiers here. So these… teams have been known for a long time in the simulations. No one's done these experiments yet. Uh, same with the… So the targets, that is something I will mention. We do actually generate electricron pairs from the solid.
These are possible interactions, and that's something I'll come back to later on.
Uh, so it all kicked off, more or less, about 19… middle of the 1980s, when.
Uh, general rule, and Donna Strickland, actually, um, came up with this idea of church call sanctification. Chuck Paul, um.
Amplification means that we take, um. A short pulse, stretch it, amplify it, then compress it again. And that gets you up to very high intensities. And at the moment, the RAL machines that my one group, the ones I'm going to be talking about, that CPAC and, um.
Vulcan here at, uh, probably the, um, reaching the highest intensities. We'll go up to about 10 to 22, which is round about here, but won't be able to shoot up to about 10 to the 22… 10 to the 24.
What's your sentiment. Now, that's still quite a long way from the nonlinear QED, uh.
Limit of about, um, say, 10 to the 29 watts per square centimetre.
And there are trips that we can do to get up to that intensity. We'll see how we can do that in a minute, so… All something, again, I… with Kibble and, uh, really policy going way back, I mean.
Judy and 53, and Kimball in 66. I remember when I was doing my PhD.
I was reading papers on, uh, that Kibble had written on laser plasma interactions, or laser matter interactions. He was looking at how a laser would interact with electrons, and these were very insightful papers, actually.
But that worked more or less, sort of, remained dormant for many, many years, until.
These hypothesis came along, and the key parameters is this parameter here, which is zeta, which is basically.
Velocity. Of the electron in these very high fields. So if you take one of the lasers which is operating about 10 to 18 watts per square centimetre.
Immediately an electron in that laser will be accelerated to the speed of light, or very close to the speed of light.
That's one of the key parameters. The other parameter that they looked on was yota, and that is, um, the comparison between.
The trainer, um… the laser field here, the laser field is the ERMS field.
And that's a key parameter as well. So we're trying to… get that file view up as high as possible.
To the 16th, so how do we actually get to that value without pushing the limits of the lasers, which we can't do at the moment?
So the trick is to use this idea of saving. Lorraine Scala, the intensity is not Lorraine Scala, so if we've got, um, say, the… opportunity of generating a GEV electron beam, so we've got a GEV electron beam, say 10 GeV.
A demo about 10 to the 3 to 10 to the fourth. Then we can take the.
Um, the bushed thing here, and we can increase the intensity, so the intensity I… dash will go up by gamma squared i, and we're getting then close to the Schwinger limit. So in the boosted frame.
The field you have is at the swing of limit, even though it is laboratory frame, it's still at 20, 10 to 22 watts per square centimeter. So.
Using an optical metalworld system, which is released that I'll mention in a few seconds.
With this trick of actually, um, Compton backscale nonlinear and Compton backstaffing from the… we can get up to intensities, uh.
Close to the human limit, or even higher. So that's the trick that we're going to.
Achieved. So there's been great progress in the last 20 years.
This is a very busy slide, but I'll just… talk through it. We start here, 2004. This is when we saw the first, um.
Beams of electrons that are being accelerated. These are unique beams, so that you've got an energy of about, say, 100.
That blocks by 85 or something, um, and that's the… Um, the divergence of the VIN, but what we have risk.
Very well collated beans that are being generated. If you look at the history here, it goes up to 2006, we're up about a GV now.
2014 year, we're about, um. 4 or 5 GDP, and then now we're up at 10 TEP, so we're… we're reaching the… the limits of some of the.
Um, problems that were thought. One of the things that will limit that is defacing.
And running out of energy. That's why you would want to keep building.
A much more powerful laser, much more energetic laser, so we'll be… getting regular beams at 10 GED out of these labour systems, and they'll be operating at herbs.
Uh, so they're basically miniature accelerators. The layers… the accelerators were gone.
Are of the order of centimeters in size. Of course, the laser takes up.
A huge room. I mean, the lasers… I think it's in the… Yes. They're all upstairs, but the beans put down into the experimental chamber.
So the, um, conventional, um. Accelerator, it's this one, yeah, I narrated that. Uh, accelerator, and it's about a meter for about 40… megabolts per meter, whereas this one is about, uh, 2cm for about 100.
Give the difficult permit. So, these are… incredibly efficient at getting up to the energies that we require.
And so it's not difficult. People have been doing this now for about 20 years, and we can actually really produce huge amounts of particles every attempt, actually.
Hopefully, so that's something that would… looking forward to switching one leads a little bit.
We're already producing these things, uh, in Gemini, which is over there, and that, of course, that is interesting.
So, in the ways of, um… is being fitted out from this building now, that the counterpart was.
Um, it's about 106 million investment for the site. It's going to be one pet loser.
Operating about 10 tasks. And it's basically designed.
To produce 10 GED and LGBs. And these elected beams will be used for.
Fundamental physics, as well as radiation sources for other material science diagnostics, et cetera, et cetera. So we're going to be exploiting these lasers.
That are going to be built over here. This is just, um, when we started, this is the crosshall that we started.
That's doing a strictly. I think she was first steps into.
Dig the hole for this with cement that's sheet in the belt bags are available.
So, I'll skip through this, because we don't really need to worry too much, but just, um… to tell you that laser books, they have the open gun into these experimental holes.
And you end up with electron beams or X-rays coming out of a very compact.
About a meter or so in size. Um, accelerate that stage.
And smoking, which is not finished yet, and it's undergoing all this, uh.
Construction at the moment, or people are in there digging holes, you see all the goodness, no sort of the homes are thrown out, and then… I was spending January, who could tell me what all these holes were. But it's an old place, the original laser that was.
Who on site the N77, but now we've taken it through, uh, decades of, um.
Upgrade, and we're now building, or hoping to build a slightly better work, 20,000 razor in that building that's being constructed at the moment. And that will be for extreme field sites and high energy density exhibits.
So we'll be able to reach the highest intensities of any laser that's on the planet at the moment.
And that's something that we're looking forward to in about 4… I think that all year's name, who were really, uh.
Pushing the boat out and going to these, uh, intensities. So, both in 2020 science, it's very… it's very, very important, actually. We'll get 20… affect what some 20 kilojoules.
Of energy available to us. And one of the important things that we're going to be looking at is.
Point collector dynamic post-axis. So we'll be able to get to.
Of course, the swing a limit by doing this pushing the frame.
Problem, and getting very close to, uh, parameters where you have to look at, uh.
No longer is QUE going to be a linear process. It will have to be.
Fully nonlinear. We still really don't understand. What that's going to, uh, include… In terms of sites. Fundamental physics, that's the stuff that Bill Knight talked about many years ago.
We're going to be talking about the vacuum nonlinear, so we'll be able to produce, uh.
You couldn't took space where the vacuum is actually nonlinear, we'll be able to do the experiments in there.
I put it down this thing called the unroll. Radiation, that's the… what we believe to be.
The laboratory equivalent of, say, torque radiation. And of course, none of our coverage of QBD.
Um, there's really a bit other things going on, so there's, uh, no states of matter, warm reds matter.
So I won't talk about any of those, but we will be talking about, um, city hubs, uh, massive physical problems in the next few seconds, actually.
Maybe that's problem, yeah. So, I'll just, uh… Oops, this is going to lower the answer physics.
For a long time, we've been… trying to get to, um, a situation using lasers, where we can produce useful electron deposits on beams that can actually start questioning some of the laboratory aspects.
Key issues that they've tried to address. Without actually doing an experiment.
And so, a number of the experiments that we've been trying to look at involve jets. So these are.
Um, Blankton Positron Jets, and… A key thing here is to look at the glaze object. This is an interesting problem, because there's a.
A deficit of GEP photons coming from the object, and one of the experiments that, um, Jackie had pioneered in CERNT, which I'll talk about in a second.
Was to actually understand how an intense election positron beam. Of, um, of the deal that last month.
Move through and adjust the other medium, and what are the instability associated with it. So we're really interested in finding out.
About this problem, and so this is the place object. So, police object is, um, producing, say, TVV photons.
These, uh, TED photons. Are actually interacting with the background look at red.
And it produced a pair of cascades, so the pair of cascade is the pair of plasma that's moving through.
Galactic space here, and by the time we see it. It's actually, uh, just the four times that we see, we don't see the jets at all, we've seen in the photons. But the idea is that if these jets are actually coming out of this, um, say, glazer itself.
They should be actually interacting with the cosmic microwave background. And unfortunately, they would be generating upshifted and producing GEV photons.
That's not seen, or there's a deficit of. So we don't see that.
So we actually thought, well, this is a very interesting, uh.
Experiment to do. So, uh, Jack was working at Oxford at the time, and he, uh, put together a very.
A comprehensive team of people. If you look at some of the instabilities. And so, the… Most important instability, perhaps, is this forumation instability. It's a green plasma instability, it's a positron beam.
Election being both from, uh, last month, going through interstellar or intergalactic medium.
And it's interacting with plasmax there. And what happens is that it would actually filament.
And create magnetic field structures. So this would be… a reason why we don't see.
So, this is a neutral beam. Yeah, it's a neutral beam. Both the atoms and polyphrons.
And what you find is, and this is, um, the example of the blue would be electrons in, um, the red is positrons, perhaps, in this.
Image that is separate, because you've generated smaller magnetic fields around the pipe.
And then they've generated as a result of the instability amplified, and then the scatter.
And so that was the… that was one of the solutions to explain why we don't see these GED.
Workforce coming from glaze objects. That was not the case. When we measured this, we didn't see enough.
Um, magnetic field to actually explain the, um. The physics of what was going on.
So when there was experiments done, and this is just going back to producing electron deposits on jets, but one of the things that we have to look at, this.
Using a high-powered laser. So, people have been doing this for years now, who've been trying to generate collection points from.
Hint from laser macular interaction. This is a laser.
The laser interacting with the plasma. Generally through a week period accelerator, an electron beam and that electric beam is interacting with high-Z material here, and that generating electropositive, uh.
Articles… Now, none of those were very successful.
The very reason that, um. You're not producing a plasma. So these.
These things that are being generated are just individual public walls, so they're not actually.
I generally think, um, what we'd call plasma itself, and we'll come to that in a few minutes, what constitutes a plasma?
Yeah, if you have not particles in the device here to make it a plasma. If you don't have enough plasmas in the bicycle, which will come to you in a second.
Then it's just a collection of individual particles, and it's just… these particles don't… In fact, collectively. And that instability I talked about was a collective instability.
A lot of collective instability's happened in. Um, in that challenge because of the possible inflections as well. So these experiments.
Um, couldn't be used to do the experiment that we're proposing to do.
And so we had to go to, uh, Sam. And we use the, uh… SPS itself, we're not using LMC itself, we're using SPS, and using this facility, it's called the HILAT MAP facility.
Jack built, um, the kit that was getting down into the, uh.
Down to the tunnel. And they set up a comprehensive experiment, which is about… at the moment, it's about 3 meters.
Lone plasma, and we're producing electron-positron pairs. By taking the SVS, which is 440 GAB.
Swift lines, smashing it into a losie target. And then the hydrons will then cascade and produce, um, DEV photons coming out of the.
No, this, this is not the tiny bit, this is just, uh, representation. These targets are about.
And we could walk or something like that, and I think… Uh, the base target, no, is about.
Graphic where you haven't used, uh, IT material. Since the first exam.
So the experiments are using just long. And we're producing large amounts of, uh, electropositron, uh.
Can we add to that? And this is… this is constituting the, uh.
We are just now. So this is a project on the older volunteer, this is the… positron density along here, and what we have is… The calculation was done through the measurements of the.
Why? Like, the number of particles in the device here.
Dictate if it's a plasma or if it's just a collection of… So the advice here is just a screening distance. So, if you think of, kind of, particles that are just a collection of.
Charges, um, and do equal and opposite charges, then you think the will try and cancel each other out, and they do. And they try and formative biosphere. The demise sphere is determined by the temperature of the particles, as well as the number density.
And that if the temperature is too small, the number density is too high, then you will not form a very large device here. So the number of particles, n plus and minus, will be relatively small.
Just individual particles that are moving towards the dispute of life. So we had to get over that part, though, and we're successful in the domain where we can really call this.
An electric bus driver. So, any instability that's going to happen will be.
Through a collective process. And this is going back to the… the idea of.
The jet propagating through intergalactic space. And it's generating some stability here, and this is a favorite, um.
Mechanism, the filamentation mechanism I talked about, was a favorite mechanism to generate multiple magnetic fields.
Which we then scatter and emit as particles, and they prevent them from generating.
Significant notice of… GED protons that we would see.
So we don't see them, so there's something else happening. So, the other solution to this problem.
Is that the region is already magnetized. So, what we've got here, uh, it could be something like, uh, primordial field, and that was something they asked.
Astrophysicists didn't really, um… think would be possible, because they would… thinking the fields were too small to see these primordial fields were too small to see after the photons, but we believe that there is.
Little pockets of strong fields. In, uh, space that two ducks would do this, and it seems to be typical.
So that's a summary. More like said that, and I'll… thing that's sticking one, so going to… are we?
Right. 10 months back, 20 minutes. Oh, well, that's a lot of time. So, right, so put on foot and scale. I said earlier that Sam is already, uh.
Um, sort of achieve this, but what we are trying to do is achieve it in a laboratory, uh, that's.
Good to just, uh… reach us away from here.
And using laser beams. So, we've got, um, 3 laser beams that are coming in through an intersection point there, and then we're detecting a scattered photon that's coming out. So these.
People who support funds are coming into the scanter region here, and they'll, um… reduce in the vacuum.
I know when you have, um, signal. That will scatter bliss into this group.
So that's the first… that would be the first direct wheel photon-photon scattering. We could argue about this with the.
The, uh, some people, if it's really important to turn scattering, because you'll generally be.
In your, uh, collision region. So this would be, um, I think, the first direct quote-unquote on Southern scattering experiment when we move back in. Now, this experiment, um.
There's lots of… if this is possible, if we can do this, we'll be able to do this other experiment, which is a double-slip experiment.
We can actually then send, through waste of units and set up a standing order.
Understanding Wave will be regions of very high intensity. So those high load intensities.
Would appear to another laser beam as being, um. Changes in refractive index. So they would normally have changes in refractive index, and you'll get.
Um, I've done more… young slit kind of experiment going on, so we built it.
Change. The, um… They set up, and see… the nice, eerie particle that you get.
So, the photon-photon scattered will give some background here, because it is quite important. So we use this Heisenberg.
And this allows us to couple. Um, St. Paul likes it deals with, um.
Electric fields with authentic fields at the Parliamentary action, and we can work down and, uh, see… the equations for the electrodynamics, and we end up with this equation here. 1, E2 relative field of laser 2.
An E3 electric field of laser 3. And that will be the scattered wave of the.
So this is, like, a third-order. Um, normally, to susceptibility, but this is due to the fact of.
And this work was done, um, here. Uh, the relevant group of some students working in the center for Fundamental Physics.
And that was a week back, you know, 20 years ago now, and this was done here, but at that time, we never thought.
The lasers we require to do this experiment would be built.
Excuse me, both, yeah, so what's roughly the dimensions of that spot where you… Ah, they're about 4 microns by.
Yeah, it's a… it's a spot that… and this is at a very crucial point in this, because.
This is an ultra-high vacuum region, and what I didn't say was that we're developing techniques to create ultra-high vacuum by sending.
In a pulse, laser. Which will sweep out any particle that is in there before these other particles collide.
I mean, it's a tall order, but I'm not sure by the experimentalists that they can do it.
So this is the basic experiment. You've got, uh. K1, K2, main views coming in.
T3 then scatters from the, uh, nonlinear. A vacuum here, so you can have one linear refractive index, and the scattered G4. So that's… a forward type of scraping process.
And it… basically, it's exactly the same as you would do for four-wave scattering and nonlinear proofs of.
In the laboratory. So what, um, we've got here is the powers… The number of scattered photons here.
Which he's saying is what I've already talked about, but this is the color of the laser, so the power of the laser.
It's a tough bet for what we did this, uh, calculation years ago. We're getting about a quarter of a.
Each collision, we're getting quarter a photon. So we'd have to do many, many collisions to build up statistics to see the photons.
One bit of work, we're getting two photons out. These are very difficult four times to detect. So, uh, usually… and these are… these are powers that we've already got.
The experiment has not been done, because we don't think it's possible to just measure those.
Um, very, very small towns. So, for photons. So we're going… We've waited until we've got the… 20 bedrock, um, these are… and this is an example of what we've got that.
2.5510, 25, 50 petawatts. As you go up and… However, you can see that you've got many more photons, uh, to detect. Now, the difference between this column.
And this column, it's the… you've got… two pump waves and 3-point waves. So, if you've got two pump waves, in other words.
Game 1, I say K1 and K2, discussing from that perspective using K2.
In the factory, it produces K3. And that would probably, uh, be a weaker effect than if you have your tour.
Put on screen into the data center, but that's a difficult thing, having four photon mute.
Focus to the same spot, but at the same time. Is quite a tricky thing, but the technology is developing very quickly. So what we're looking at here is the number of photons you'll start to see as you go up in power.
I grew up just waiting. And a number of groups around the world.
Waiting to do this experiment, as most people are trying to go in bed.
I believe the champions are… I need to do 100 kids walk through it.
There's an interesting twist to this, and… This is a twisted laser beam, it's an orbital angular momentum, so it's stressed it.
And this would give us the ability to actually, uh. See a scatter proton from all the other protons that are in the system.
Because it would have a unique. Spin to it, so we'll be able to identify this orbital angular momentum photon, so we know.
Rather than just look at the energy of the photon, this would tell us something about the… uh, scattered photon itself. So this is an interesting twist.
So, IT and 4. Igm problem. See, it's virtually the same as what I've just been talking about.
All these processes look very similar, because they open through the same kind of arranging.
So we're talking about, uh… problem now.
And here we've got a 3-wave kind of coupling process. We've got.
Lead a very intense laser bead coming in. And it scattered us, um, from the vacuum into another photon, omega gamma.
And an axon, which is the energy meteor. So you've got the possibility now.
Driving, um, the vacuum into a modern enough state. Which would then generate an idea. So, this is something that was done a few years ago.
And it's one of the experiments that's planned as well. So this experiment will actually look at the possibility.
Of driving, um, uh, Naxion. With a very strong, uh… Electric field that's coming from the laser.
So, again, we're using this Lagrangian here. These are the two key terms here, and E is the amplitude of the axiom, E is the.
The amplitude of the Navy field of amplitude. But the other electron indicated with. So when you take these waves, couple them together.
It's something that we've been doing for a long time, but not with Axioms, but with plasma.
Um, most of the time. You know what would be a plasma wave.
And we would couple a reasonably to a plasma. Generate a plasma wave, for instance. That plasma wave could be the wave field, and you're generating.
An accelerated… I'm sorry, a weak field that's growing. Perhaps closer to the speed of light.
And you can then accelerate particles using that plasma wave, because it's carrying electric field in the same direction as it's propagating it.
Identical equations, so we can just carry through the analysis. These are… these equations are very familiar to anyone that's working in laser-plasm interactions.
Except we'll just replace Asia. With… sorry, the… will replace the plasma wave with A, which is the oxygen field now, and we can do.
We'll calculate a dispersion relation, and this dispatching relation tells us that we've got.
Scattering of a laser beam in the bathroom into an axiom, plus another laser be.
And that would give us the opportunity then to study, perhaps axions at different, um.
Masses. So this is, uh, again, the mass of the axion.
And this is the coupling here. And so we've got this, um… To date, we would probably be a way up here. We are… where everybody helps us, especially the limits of the item mass. So.
If we can actually push it down to here, we're getting closer to where.
There's gaps in the… measurement of IT and mass. So there's no ICM roundbook here at the moment, or Norwood's doing any experiments in this region here. So we could probably start to push.
The limits of that, technically. And you'll recognize that task here is the experiment that was carried out in.
And, um… and that's looking at the… the, uh… So, actually, sort of telescope.
So they were looking, I think, from the sun, coming as a result of the photons that the sun in getting.
So this, this brings me to the experiment that we did do. We haven't done these experiments yet, because we're still far away from the.
Limit that we need to get to. The new links that's coming on along this limit will be.
Actually reduced here. So this is the experiment that was conducted.
Again, this is done, um. Using a laser? What was that?
A free electron waves up, so it was an x-ray laser.
Jack designed the equipment here, and the laser… pre-electron laser phrasing.
Was used to interact with the crystal plane here. So the crystal plane has got benefits.
Very locked electric field. The medium field… it's a medium crystal has a field of about 10 to 11 volts per meter.
So the magnetic field. Um, parallel to that electric field in the cleanup, the crystal would give rise to a nasium, so we're seeing.
An idea of going out. You also see that the gamma ray coming out here, because the gamma ray will be.
Baked by Crystal as well, so the… You put a shield here, which means that you've got light shining through wall experiments, so it's a light shining through wall experiment.
Stops the light going through, and then you absolute through. Reconvert in the almost identical.
Situations you've got here into a photon, and you detect a photon. So that experiment has been.
Success Week, uh, completed, and the work was written up and, uh, published in the annual.
And that was the… those were the limits. So we're… with me.
European Excel work out here, so it's a region where no one is looking, actually. And of course.
Which is your huge unique excellence. We're out here with the, um, bounce racket at 10 to the minus 4 Bob, that's an older plot, but… Is it? Yeah.
So, having close to no motivation, yeah. I'll go exactly.
Thanks, Jordan. So again. Having fun.
Maybe 12 minutes long. Okay, total application, wake up and… Okay, this is now exactly.
This is… this is all due to, uh, paper that came out in about 62.
Yes, it's in effect, and it's very similar to the accident effect, actually, because.
With the action, you've got the possibility of generating the ICM by putting an electromagnetic waiver through a magnetic field.
You do the same thing here. You get the Graviton, which is the H strain of space-time here.
Is interacting with them. So what we've done is we've taken this idea and reversed it.
So we're taking the photon, put it through, um, not a magnetic field, but we'll pour it through.
There's another leader. So the leads up here.
Snatching off that gravitational wave. And it's scattering in a similar way to the parametric instability, so you're scattered from this gravitational wave.
And the way this picked it up on this detective, so they… The frequency of the wave is.
That you detect is when we got the grappitional wave frequency minus omega of the laser beam.
And that actually will get us into a regime where. The frequencies are way higher than anything that's ever been looked at.
Contemplating, looking at these frequencies. These are in the optical regime.
Of the updates for WAVEs, and I'll show you the thought here.
This is my role. This is where we are just now.
This is the plot that, um, they've been able to, uh.
Detective gravitational waves, we can see. The way down here in the tens of Perth region, whereas we are way up here.
Uh, with the lasers. If you go to terahertz, you have a problem.
Back that way, in terms of frequency, you can… you're not pushing very far down, but you can see that the next upgrade of lasers will be getting.
Close to what we think is a detectable signal. So, the next upgrade of high-power blazers, which is not going to be in this country, it'll be in America.
Um, that will be pushing this limit down. The reason we have to go to America is they get more photons than we have.
But does that mean they get more energy? So they're being sick.
Much, much more energy than we have. So, but what's the source of these gravitational waves?
Well, we're not specifying the source. We're saying that if the… that's a good question, because.
At the moment, this shouldn't exist. Right. If they do exist, it means that there's physics beyond the standard of language.
And that's… that's what they're obviously leading to. That's a… I'm glad you brought that up, because it would lead to something beyond the standard model.
Some would observe them. So these are relatively cheap experiments to set up. They're not expensive.
In terms of, uh, possible, if you're building a, uh, say, the next, uh, collider, these are relevant.
100 million, etc. What's in this arcade? Oh, that's an interesting… yes, that's, uh, an asphysical measurement that people… taken part of the cosmic microwave background in a frequency range.
That's different to the frequency range of the taking part in the cosmic microwave background, the high frequency part, and the look that changes to the.
The radio frequency. Due to adaptation waves, to see if there's a signature.
And that's a ground-based experiment, or…? Ground-based, yeah. No, sorry, that's a satellite basis.
So, finishing off there, I mentioned that. I'm saying, um.
I just input on… I like to read positively exposed it, they're all very similar. They all fall into the same.
Kind of account. And here, what I've got here is kind of two-seam instability. I talked about a two-seam instability after the election. Borusson really going through low-density plasma.
The same thing can happen with neutrinos. Neutrinos moving through, uh, an Earth.
Lunch month! Moving close to the speed of light.
Will generate plasma waves that are also moving at speeds very close to the speed of light.
And we think this could be due to the anomalous heating of the supernova II.
Itself. So this could get right to the explosive event. Now, before you say the neutrinos don't interact with anything, we're talking about.
Huge foxes on humans here, so there's lots of neutrinos. It's basically, um, take the 29th, 10 to the 31 per square centimeter.
And the density of the medium that I'm moving through is about 10 to the 29 particles.
It can be centimeters. So they're inside. They are very close to the proton nutrient star of a supernova itself.
So you can actually get, um. An instability going on, which is a two-stream instability, driven by a material being.
And you can also, uh, get dampened of possible waves, and this could be due to, um, say, the process of.
Lundo Dumpy. And we've assumed that this could be.
Associated with the cooling nutrient star. So you've got nutrients, uh, neutrinos that are inside.
Against, um, volume of fructonneutral material, and they're killing that material by.
Taking energy away from the plasma waves, which is normally associated with it.
The other, um, instability we've got here is I'd like to wait.
Why… why will incivility? And we've thought that this could be too… this could produce the free diastatic magnetic field, maybe even.
Be responsible for the primordial structure in the early universe. So, it used the same kind of, uh, physics.
In this case here, we're using the Hamiltonian for the. Uh, the neutrino, these are electron neutrinos.
And you give rights to, uh, two forces. One is the force on the, uh, the… background electron, so it's a gradient of the density of the electrons, and the other is forced on the electron to the gradient density of the neutrons.
So you get these, um, combination of forces, which actually help drive the instability. So these are very similar to the.
Paper forces that you can generate in that. And that plasma medium.
And when we looked at the anomalous, uh. Looking at two genes below it.
We find that we can capture about 1 to… Let's see, 0.1% of the neutrino energy that's coming out of a supernova in the.
Material that's surrounding the… still short, and it could re-energize the shock.
This is, uh, something that… We're still working on, and there's a lot.
Interesting studies to be done there. The geomundo Dummy? What does that mean?
That means that if you've got a distribution of, uh. A lot of people, in this case, the distribution of electrons. Uh, materials that are moving.
Who pays to launch the APD fine. Sorry, please.
Most of the dispensable to the plasma waves can take energy away from the, uh… electrons stick away from the pathway by being accelerated. So these neutrinos.
Are being accelerated if they're based mostly on the north side is mostly based mostly of the electron passing away.
I think, uh, the genome interactions, so just summarize that very quickly.
Uh, so they can generate intense relativistic plasma waves by the distribution stability.
We can be accelerated by plant waves to higher energy. And we can be responsible, perhaps, for supernova explosions.
Now, those… those intense fields of neutrinos that we're using here are way beyond anything that would produce any alarms, and so there's no.
There's no hope of studying that an experiment book. Yeah, theoretically, sounds like not.
Lastly, I said that was just, uh, mention this. This is something that, again, Bill and I talked about a long time ago, unknown radiation.
And, uh, it's something… I've just got a few slides in this, and it's another experiment.
No one really is aware. Oh, um… The possibility of doing this experiment using the… This has been, um, on the cards for a long time, and it's the equivalent, uh, principle that tells you that an accelerated path door.
Would be exactly the same as possible sitting in the field of a black hole.
And so you'd see, or expect to see, equivalent Hawking radiation, which is given by this, uh, equation here, Hawking radiation.
That temperature would be T is given by the acceleration due to the black hole.
Exactly, uh, the same kind of relationship you've got for the unknown radiation, whereas the temperature of the radiation that it is.
Observable, see? It's given by the accelerated, um. Acceleration physics. He or she is experiencing. So you've got this.
Passing here, accelerating, and being accelerated by, uh, value A. And then we actually constitute them through the performance principle, a temperature. They would see the temperature. Now, the problem is.
Um, is that possible? You see, there's lots of people saying there's no such thing as, um.
Under radiation. There's, uh… meetings are left, people discuss it a lot.
Um, but it's something that if you actually could determine whether or not there is a real.
Possibility of looking at new radiation. We could possibly do it with, um, the high-power laser that we've got.
So this is an image of what we're actually looking at here a little bit, too.
Um, high power lasers with an electron beam going through, so these red… Regions here, uh, on an iPad basis, we are centrally polarized.
Electron beam is moving their circular orbit. And we are accelerating that in circular, and we ship.
If fucking relation does exist, they may be able to detect it by.
Looking at the green… wouldn't see it. So that's, um, that's… Something that we've talked about for years and years, and still.
Really do want to win for them. Movement and this in… We've got lots of papers going out.
Whether it's real, whether it's not real, whether an observer can see it.
Who's not in accelerating film, etc. So there's lots of GR, uh, puzzles here that we have to.
Understand. And so. Inclusion said.
Lasers are closing in on the intensity frontier. You guys do the energy frontier, but I mean, also.
Admit that you can do the intensity frontier as well. Uh, new accelerators are being generated. It takes us to tens of GEV.
Um, new compact light sources, x-rays. Democrats, etc. And fundamentally, using these lasers is developing extremely quickly.
Many people around the world, um, I know working in this area.
And it's opening up lots of, um. New things we like to study. So those are only a fraction of the things that I… that were going on over at, uh, EPAC, or we'll be going on over a deep time.
Thought that, um, looking for a strong interaction with particle physics, you know, because you guys.
Know more about some of these problems than we do. So, uh, I'd like to stop there and thank you for your attention.
Thank you very much talking with you. Uh, let's, uh, questions.
Just a comment on your last statement. Yes. What are the… places where you see.
Gpd working together. Oh, and closely with all of this. I mean, um, I mean, we're very strong in foot-on-foot and scattering is definitely something that we look at.
Yeah, doing something we haven't done. There was an experiment that was done in Slack a number of years ago. We could do it, uh, easy idea with the.
So there's lots of experiments that have been done. Um, in the past, that we could redo with.
A new setup, and I think it's just a matter of getting.
Together around the table, and talking about, uh, forming collaborations. I mean, the collaboration that I'm involved with with Jack is opening up a little bit of that. A number of people who are.
Impossible physics who are also involved. I mean, we've been an example of Super Saka, you know, Subir?
Yeah, he's heavily involved in these experiments and the work. Particularly angsty and stuff.
Some of the students we're looking at is a middies. Period and lots of units are.
So I think that… I think we've got to a point now.
Fundamental physics, where the laser people, the laser, uh, traditional people.
We need your help. Now, to tell us what experiments you would be interested in.
That's… that's really why we're talking to you now. And I've always, always talked to the past few people.
But you like to build big flavors. Yes, and I think.
Provides my accelerators can play a role there. We can build a collider, perhaps, in the future that may.
You need also to accelerate positive. Yes, that's true. I mean, the positron say that, because people aren't working.
And if not yet, we were trying to generate. Plasma polite that will accelerate budget times, and the lifetime of those photons is quite large.
And we can't actually… some experiments have been done very accelerating posture, but you're right.
With a flight that we could possibly do that. But the other… Um, problem we've got is, if you can get up to 500.
G, we could probably use an afterburner. By sending those beans into plasma to boost their energy.
Up to a TV, or beyond that. And those are proposals that are already out there, and people have been talking about that.
I think on the side of things that we thought I was talking about now is using conventional collater for deposit runs, and a wake field that later out front. There's a sort of a stepping stain.
May I please ask you to go back to this neutrino? Yes.
I can tell you a paper on it, that'd be easier. Which one? Are you able to, uh… So, I mean, yeah, just a… are you able to have… Here… which we are able to… no source on the planet would be able to do these exciting experiments.
Even if you built a neutrino battery, the flux would be too… One of the things that must, um, point out is.
The MHW effect. Is a plasma effect on the sun.
So it couples to that plasma gradient. So, if that gradient is a space-time.
Structure. In other words, it's a wave. You still get the same, uh, effect happening. So the neutrino will exchange momentum.
With that, uh, structure. And that's very similar to what I've been doing, yeah. So what I've done is I've just taken the MS long-year formulism.
Replace the density gradient. We've done moving structure that's got a space study in football.
And that gives me the coupling, then, between the retrieval and the plasma wave.
If you wanted to look at, um, say. See, labor oscillation, like an MSW thing.
You'll have to walk around, you know. The sun's density is 10 to the 26. We can't produce that density.
You know, you have to have the density of that over a million kilometers, and we can't do that.
But you really… I mean, if it's possible, you could see the MSL yesterday.
That was the key, because MSW. Couples into the agent's both done, and also it's a validation report on. So all these things are very, very similar.
I think there was, um… I can give you the paper that points this out at night.
Yes, sir. On the neutrino topic. Um, would you be able to see anything in the energy spectrum neutrinos from the Galactic center?
Yes, if you, if you, um, have got… if you've got a spectral.
Stopped, you know, it's actual, you could be able to see.
Uh, if there's a component of it that is non-thermal. And that would indicate that these particles, these neutrinos are being accelerated.
Through some turbulent media website. So I'm… so it's coming from a pristine source, say, like, through, um.
Very turbulent, like, percentage of the, um, the galaxy. And if you see a shift in the spectrum.
We discussed this a number of years ago with, um. Building these guys, and it's something that we've got could be a possibility.
But no one's got a neutrino detector that can do that yet.
I don't know if that's true. Yeah. …that are coming online. Yeah.
Hopefully negative self aspect, right? But Julie… Would they be able to… I mean, we've only seen, what.
Um, is it 19 materials that are… you know, outside the solar system, coming from outside the solar system. And that came from a magnificent vote in 18878.
So there's also, um… well, there's Ice Cube. Yes. …getting an upgrade, and then there are other proposals, there's another proposal for a big… between infrastructure and the Pacific.
If we can get, um, uh, enough, uh, neutrinos. Yeah, you can see a spectrum.
Then, if there's a shift in the spectrum, yes, you should be able to identify some of these effects.
Particularly the, um, material. You can either… you pull it down or you accelerate a small foot.
But I've been looking at some of this for a long time, as you probably might. And I haven't seen many genres coming from it saying that the solar system.
Yeah, a big, uh, deal with consumers coming constantly out from the son of… nuclear reactors, yeah.
Is it on Zoom?
Maybe I can ask anyone. One thing I was wondering, uh… applications in the lithography, I mean, on the development that goes into the laser physics and photonics, and these applications.
I mean, that's a big money game. Yes, yes. Uh, is there… And, I mean, okay, ASML and ZS and they are the divers of that.
Is there some role where, you know, from academics, uh, which you think can match that, or complement that, or, you know, somewhere, somewhere… I think we are generating, uh, very… running eggs resources. You know, we've got a compact accelerator, we generate X-ray source.
Then I think that will lead to applications in that area. I mean, Jack may be able to tell me more about that, since he's closer to the.
It's a practical applications that I… I mean, there is already, you know, money coming… comes into Verich University groups from ASML and the like as well, it's not like they… they interact with the community in various different ways, so yeah.
They do? Yeah. Okay. I mean, I think what we're trying to do is here is trying to get more interaction with you guys, so… Because we're building a very extensive.
We wanted to have ideas, and you guys can say, well, have you thought of this? Have you thought of that? We don't, I mean, we don't know.
As much of the fundamental physics area as you guys do.
Yeah, I think that sounds like a nice call for us.
I think one thing that, um. Bill, myself, Norman.
Even though it's a few other people. We've set up this, um, fund-centric fundamental physics. We've got small amount of money from.
I allow you to… It's right.
You know, sensible week when you threw money there, so we held meetings, and we held small… What a shock she thinks it had for you to bring people to come on top of that panels. And a lot of these ideas.
We're generally good about that. But the leaders didn't exist, so no one could.
Keep doing it with each experiments, but no work in the strategy that we need to do something with it.
Colts mentioned the latest in the UK, but there are also lasers in Europe and in the US that are… kind of pushing similar… levels of intensity, repetition, right? So, it's not just here, it's pretty global.
I mean, it'd be good at doing a PEV accelerate something.
That's it. That's something that we need to work at. In fact.
When the relevant design for a TED accelerator was, uh. Move forward. We did work with, uh… profitable physics table. We have strong interaction with people like, um, Frank Wilson, people like that.
Come here and do that. Tell us what Lini did. But I'm just for a plate of.
We knew about the convenient at that time. We need your refresher, and I think Chris works very closely with people here with it.
By impossibleities.
Okay, no.