Thank you very much. We will go straight to the flag that the injured flying eagles have arrived at Buja today after crashing out the quarterfinals of the 5th and the 20th World Cup in Argentina. The players, including the coaching crew and officials, touched down at the Inlandia Azeco International Airport via Ethiopian Airlines. The team finished as runners-up in Gupti, which has Brazil, Italy and Dominica Republic. The first knockout stage game against the Oce Nation, that's Argentina. The flying eagles were called a shocking 2-0 win. This is the first time ever that the flying eagles will beat the South American team at the Under 20 World Cup. We all could remember in 2005 when we lost to the team led by Messi in the finals. Away from football, we go straight to volleyball. In Cardona, over 205 young volleyball stars, male and females, accost Nigeria, adjusting for a slot to be picked for the National Under 17 team. In the three days, open trials at the Amor de Belio Stadium also in Cardona. The development is coming, following the very fact that African volleyball confeditions decision to give Nigeria an hosting right for the Under 17 competition slated for September 2023 later this year. More in this report. This screening exercise includes over age, height and the best players fit for the national game as 145 boys and 60 girls young volleyball players are in a three day open trial camp. Speaking at the camp, the technical director of Nigeria Volleyball Federation, Martin Smelandi says the talent and level of skills displayed by some of the players are commendable. This one is to give every player opportunity so that we don't just sit at home and start selecting our brothers and sisters to come to come. So we have done the screening this morning to screen out over age players and also those that we feel their heights for now will not be beneficial for this competition. The Under 17 coach Sunday Acapsin describes the boys and girls as dedicated, noting that the players are interested to play for the nation. The primary way so far is the fact that those players are interested to play. They want to play, right? Now it's left over with the coaches to invite the right character in them because the primary thing that you need is for the players to have the interest to want to play. These players that are here have the interest. I think the bulk of the work right now is on our head, the coaches. Because if you fail these kids knowing what they have in their hearts, I think Nigeria will be disappointed with us. And of course we are going to jump into their future. Some of the players express delight in being in the open trial camp saying height will not deter them from participating. Another hundred percent sure because in volleyball height advantage is also harder. It's going to be the glory, it's going to be the grace that I'm picked.  The game is the thing that is involved. It's a privilege for me to be happy that I'm here. I will work harder and I will do my best to be among the equalities to select. The under 17 volleyball trial will select 25 boys and 25 girls who will represent the nation and hopefully bring glory to the country.


From Las Vegas, it's theCUBE. Covering VMworld 2018. Brought to you by VMware and its ecosystem partners. Welcome back. We're here at VMworld 2018. You're watching theCUBE, two sets, three days, 95 guests. I'm Stu Miniman, my co-host is you piss car and we've got a little bit of news to talk about. So lots of announcements made at the show. One of them is that VMware has purchased the intent to acquire Boston-based cloud health technologies and I am thrilled to have on the program. Back to the program, actually. I've had in my Boston area studio and seen it lots of shows. Joe Quincella, who's the founder and CTO of cloud health. You got it. Good to see you again, Stu. Good to see you. Absolutely. So just to get out of the way, the Boston Business Journal says for about 500 million, so I know you can't comment on the dollars, but this is a big deal. 200 person company, as I said, Boston based right down the road from us. Upstopping, your new headquarters is opening on Thursday, which I'm stopping at on the way back from the airport. So congratulations first of all and tell us what's the feeling like of your firm? It is exciting. We certainly weren't looking to get acquired. So as you know, we raised a fairly large D round last year and we were focused on building a big public company and what we found along the way of talking about a partnership with VMware was there's just a lot of synergy, both vision strategy as well as cultural synergies. And I think it somewhere along the way we realized this made a lot of sense. So it is a big deal and we're very excited about it. Awesome. So Joe, one thing I like, I see you and your company at cloud shows. Yes. You know, this is where we have, one of the things that excited me this week is we talk about like, I'm a networking guy. We talk about the networking. They're talking about multi-cloud the way that NYCERA was pre-acquisition. So VMware talking a lot more about multi-cloud. They had Amazon up on stage and I think the acquisition of cloud health technologies is how does VMware become more of a cloud first? So for people that don't know cloud health technology tell us a little bit about the origin, your founding and where are you playing the ecosystem? How much of a part is VMware today versus everything else? Yeah, we're down to that. So I founded the company six years ago and it was, I was an early pioneer in the public cloud. So in the 2010, 2011 timeframe I was building out large scale public cloud infrastructure. Sounds a lot less impressive when I give you the numbers now but then it was very impressive. And in the process of doing that just realized the incredible complexity that you had to confront to actually be successful in the public cloud. Both complexity of deploying and managing, you know, efficiently that infrastructure but also the complexity of all the tools that surround that management. And so I set out with cloud health to build a single SaaS platform that customers could use to what today you might call build out a cloud center of excellence is kind of the terminology which is to have one central platform where you can centralize and distribute cost management, security compliance as well as proactive governance all the way to integrating back into your back office and your service desk and your incident management to make the cloud just part of how you deliver your business services. And so that was the journey six years ago and it's been a tremendous journey to date. Yeah, no, you were definitely a pioneer in this. So congrats what you've done. Cause I remember six years ago, come on cloud was simple. I swipe a credit card and we'll just do this and everything. And now everybody kind of understands not only cloud but especially multi-cloud getting my arms around how I manage all this environment. Maybe touch on how, how does multi-cloud fit into this whole discussion? And what does cloud health do with VMware today versus everything else? Yeah, so when I started the company multi-cloud was part of the vision but let's be honest, there weren't a lot of companies really doing multi-cloud. Usually at best, especially in the enterprise if an enterprise was even doing cloud they were choosing a single cloud provider. They really weren't trying to actually, you know have multiple, multiple providers. I think what's happened is in the last 24 months is enterprises went from being a single cloud to pervasive multi-cloud is what I call it which is their portfolio now includes, you know dozens of SaaS products. It includes multiple public cloud providers. It includes multiple private cloud providers and it's just a very complex, you know heterogeneous portfolio they're managing. We were built for that. It finally come true and I think what it does is if you think what you need to be successful in that environment, if you're going to build out a cloud center of excellence across a pervasively heterogeneous environment you need a single platform that does that for you. So today our product supports Amazon, Google, Azure and it also supports VMware. So it integrates directly into vSphere, does cost management, does inventory visibility as well as migration recommendations to and from multiple different public clouds. So it's a great synergy between what it is that VMware does across its rich, robust portfolio and cloud health. So talk a little about the new possibilities you're now opening up being acquired by VMware. What does that mean for that multi cloud strategy? Yes, so I think Pat touched on it in his keynote and I thought he did a masterful job of describing how cloud health, the brand will be kind of a core brand of VMware and this will be a centerpiece property across integrating across various different kind of properties across their SaaS portfolio. But I also think VMware is very aware that there's a lot of choices that customers want. They may want to choose different products for log managing configuration management for application performance management and I think we're going to continue to provide that choice to customers so that it won't be just a VMware centric product. But at the same time, you look at the richness of the VMware portfolio, which is you look at what they do on premise and you look at what they do around cost management inside the data center. You look at VMware on AWS as an offering. There's just huge potential synergies between what we do and how we can extend our value proposition into those areas much faster as part of VMware. So as the founder of the company, what excited me about this was this was not taking me away from my vision, it was an opportunity to accelerate my vision which is really what kind of got me there to this idea that we would be acquired. How do you think your products will help VMware? For instance, in the VMware cloud on AWS, do you think you'll integrate on that level to help VMware accelerate their proposition as well? Yes, I believe I'm actually very excited about VMware on AWS because I think we all know that VMware has been optimizing its stack for so many years. There's incredible efficiencies that have been built into it that I would like to bring up to a business perspective so that our customers can understand them and take advantage of them in an easier way. And so I think there's great potential there. I probably don't want to get over my skis too far here on this one, but I do think it's one of the things you'll see early post-close of this deal. Joe, I think the timing's really good. If this acquisition had happened two years ago, we'd be talking about vCloud Air. My joke would be to say, okay, when does the update come that says all migration should push you to VMware at 99.8% of the time? No, but right, VMware, it's not only AWS. We saw the VMware presence at the Google show, you got to do a Google Cloud show and they're trying to position themselves more in this multi-cloud world, which is where your company sits. Joe, what advice do you give to companies that software companies out there? How do they help customers in this multi-cloud world? It's a big environment. You help with a bunch of things, but there's licensing, there's all sorts of variability out there. I say it's this giant elephant there and you might have a main course of it, but there's lots of partners you need to work with and customers have just the paradox of choice out there. So how do you as a software company and be successful in this space? Yeah, so I think myself as a software company or as our customers? Well, so what advice do you give to your peers out there and if you were given Pat advice as to how do we be even more successful as a multi-cloud player? Oh, I think their strategy is very mature and that was one of the things that got me excited about it, which is I think there was a time at which I think companies were very territorial about how they approached kind of the pervasive heterogeneity that we're entering now and I think being open in the way that they are, that all of the properties that customers may choose may not be a single vendor. There's going to be lots of different vendors and lots of different choices and freedom of choice, I think, is kind of one of the fundamental tenets of a successful strategy at this point in time and so I think I would just highly encourage that for everyone, which is I think the old world is the old world now, like we've entered kind of a new frontier, we have to think differently, we have to act differently and I think what I really love about what Pat's doing is he's harnessing the DNA and kind of the strength of VMware, which is just, you know, they've been a tremendous provider of great software for two decades and kind of bringing it into the next frontier of cloud and I think they've got a lot to bring that we have not seen yet that we're going to see over the next few years and I just hope to be part of that. So you mentioned the new frontier, right? So, you know, VMware is still somewhere in between the old frontier and the new. So one of the, you know, problems we've seen in the past is VMware and its relation with the service provider world. So what do you think you'll add to that mix to help service providers maybe move from the old world into that new world as well? Now, Yub, that feels like a fastball down the middle so I just have to tell you, so the relationship with VMware started 18 months ago and it started with an SVP at VMware and it was all about partners. And so one of the things you might not see externally from Cloud Health is that there's really two products in Cloud Health. There's our direct product that we deliver to enterprises and SMB and then there's a separate product that we sell to service providers and it enables them to deliver managed services to their customers on top of the cloud and we built it in a way where the products are really one product that actually are sold as two separate products and so I think what we're going to bring is a real strong opportunity for partners across VMware and that's why the opportunity, the business relationship started as a potential partnership around partners and eventually evolved into where we're at today. So we're excited for that. I think it's, I tell people that the cloud is the single greatest threat and the single greatest opportunity for partners and the difference between which one you're going to experience over the next few years is whether or not you can figure out how to harness the disruptive potential of the cloud. All right, so it sounds like I've got a question for AJ Patel tomorrow when I interview him towards the end of the show because yeah, service providers there. All right, I know you can't talk a lot but give us roadmap. What sort of things is it like, I see NSX being pervasive. Are there integrations today? Do you have visibility in Cloud Health? Is that something from the networking side that you do or would tie into? I think back, I've been in this long enough when EMC bought VMware, it was here's all the cool stuff we could do and I was in engineering being like, oh my God, it's going to take us five or six years to do most of this stuff. It got done, but there's long hard engineering work. So 18 months, what can you talk about that's been done and gives a little bit of what should we be looking for? Yeah, I mean NSX is tremendous offering and I think what you see is I'm really looking at this as more kind of like tier one, two and three integrations and tier one, I think you're going to see more around the cloud properties, probably things like VMware and AWS and you'll see the SaaS products such as Wavefront and things like that. I think that's, there's a natural extension and a natural movement and a natural value proposition we can bring on top of those. I think tier two, I think you'll probably see a lot more hybrid where you're going to see us kind of take advantage of that rich portfolio and VMware and extend it and add value on top of it to our customers and I think tier three, I'll think I'll leave quiet for now, but I think there's some really amazing potential of what it is that we can do together based on what I'm seeing exists in VMware and things that maybe are being built that are not yet public. I think there's some really great potential of what we can bring to the market around how they can manage their multi-cloud portfolios into the future. All right, Joe, last thing I wanted to ask you, Boston-based company. VMware had a strong presence in the Boston area. I know a lot of people in their Cambridge facility, but talk about the tech scene in Boston, being a founder, you got a new headquarters, getting acquired, I'm a bit of a homer, supporting people so that I don't necessarily have to travel across the country or across the world, so give us your viewpoint on the Boston area these days. You know this, which is it is incredibly vibrant what's happening in Boston, which is the businesses being built, the entrepreneurs that are there, just the entire ecosystem is working at a pace I have not seen in over two decades and they're building real meaningful businesses. When you actually lift up the cover and you look at what these entrepreneurs are building, they're going to be, it's going to be an important tech scene for decades to come based on just what I'm seeing happen today. I look today and a lot of people like to give the credit to the person who founded the company. There's thousands of people who touch this business, just including to the tremendous effort from every person who joined this company, there's been people like yourself and people who've added value in many countless ways along the way and it all came primarily from a Boston community that was there to support me and my company as we grew up in the Boston tech scene. So it's been, I've been blessed actually to be surrounded by great people in one of the best cities in the world. All right, well hey Joe, congratulations again. Thank you. If you don't know, they even have superhero stickers of this guy that they give out at Tom and Tessa. Joe Concella, Cloud Health Technologies, congratulations to you. I'm looking forward to seeing the grand opening back in Boston when I fly back after the show. For you, Piscar, I'm Stu Miniman. Thanks so much for joining us on theCUBE. Be back with lots more. Thank you.


students. This is Mr. Nagesh Artambaki, Assistant Professor, Department of Mechanical Engineering, Valshan Institute of Technology, Sholapur. Today, we are going to discuss on the topic attachments of leg machine, learning outcome. At the end of this session, students will be able to explain attachments of leg machine. Before going to discuss the attachments of leg machine, what type of operations cannot be performed on leg without attachments that we are going to think. Please think on this particular question. The operations that are that cannot be performed on the leg machine without attachments are grinding, milling, copying and then relieving. This type of operation cannot be performed without attachments. Now content in this particular session we are going to discuss. Introduction of leg attachments, grinding attachment, milling attachment, taper turning attachment, copying attachment and relieving attachment. Each general purpose conventional machine tool is a designer and used for a set of specific machining work on jobs of limited range of shape and size. But often some unusual work also need to be done in a specific machine tools. Example, milling in a lathe, tapping in a drilling machine, gear teeth cutting in a shaping machine and so on. Under such conditions, some special devices or systems are additionally used being mounted in the ordinary machine tools. Now first one we will discuss that is the grinding attachment. This grinding attachment is placed instead of tool post of a lathe also known as the tool post grinder. It is mounted on the compound rest as a substitute for the tool post. It consists of a base plate, grinding wheel and a motor. The workpiece is held in a chuck or between centers. It is widely used for grinding lathe centers in position. Grinding operations can be performed on the lathe with this attachment. This useful attachment can be mounted on any lathe. Grinding hardened workpieces and ensuring a smooth finish. Internal grinding can be carried out with this grinder. Milling attachment, we can able to perform a milling operation on the lathe machine with this particular attachment. This is a milling head comprising a motor, a small gearbox and a spindle to hold the milling cutter mounted on the saddle after removing the cross slide etc as shown in the figure. Milling attachment are generally used for making flat surfaces straight and helical grooves flanks, long and deep screw threads, worms etc. In centerless by using suitable milling attachment, taper turning attachment, five types of taper turnings are there. One is with the help of form tool method. Second one is by combination field and third one is by tailstock set or method and fourth one is the taper turning attachment. And also fifth one is this prevailing compound rest method but we are going to discuss this attachment. The function of a taper attachment is to guide the tool in a direct path set at an angle to the axis of rotation of the workpiece. A taper turning attachment consists of a bracket or frame that is attached to the end of the lathe bed supporting a guide bar, pivoted at the center the bar with graduations and degree can be swelled on either side of the zero graduation. It can be a set of desired angles, desired angles can be given on the lathe.  And also we are going to discuss benefits of the taper turning attachment. It leaves the alignment of dead and live centers untouched. So both straight and taper turning may be performed in one setting without a downtime. Once the taper is set any length of a piece of work could be turned within limits. Several work pieces could be turned. Internal tapers can be turned effortlessly. Now next one is mechanical copying attachment. Suppose we have performed a one masterpiece and if you made a guide of that definitely that particular guide will help us to give the multiple jobs with a copying attachment. A simple mechanical type copy turning attachment has been schematically shown in the figure. The entire attachment is mounted on the saddle after removing the cross slide from that. The template replicating the job profile desired is clamped at a suitable position on the bed. The stylus is fitted in the spring loaded tool slide and while traveling longitudinally along the saddle moves in transfer direction. According to the template profile enabling the cutting tool produce the same profile on the job as indicated in the figure. Next one is hydraulic copying attachment. The stylus moves along the template profile to replicate it on the job. Now if we compare with the mechanical copying attachment mechanical copying attachment produces a vibration and noise because of that we cannot get a finished object after a mechanical copying attachment many times. Therefore in hydraulic copying attachment hydraulic copying attachment is costlier than the mechanical type but works much smoothly and accurately. As compared to the mechanical the hydraulic copying attachment is accurate. The cutting tool is rigidly fixed on the cross slide which also acts as a wall come cylinder as shown in this figure. So long the stylus remains on a straight edge parallel to the lathe bed the cylinder does not move transversely and tool causes straight turning. In cross fit direction the ports open and the cylinder starts moving accordingly against the piston fixed on the saddle. The slide holding the tool by same amount traveled by the stylus encloses the ports. Last one is the reliving attachment. This attachment we are using to produce the gears to produce the slots on a circular objects. The teeth of form relived milling cutters like gear milling cutters, tabs, halves etc are provided with flank having archimedes spiral curvature machining and grinding of such curved flanks of the teeth reliving motion to the tool or wheel as indicated in figure. The attachment schematically shown in figure is comprised of spring loaded bracket which holds the cutting tool and is radially reciprocated and the saddle by a plate cam driven by the fluid rod is indicated. So due to continuous reciprocating action it will give us gears and different slots on the circular object, equidistant slot on a circular object. Now these are the references Hajra Choudhary, elements of workshop technology volume 2 media promoters, PM Rao, manufacturing technology, battle cutting and machine tools. In this particular session we were discussed the different attachments on the lathe and these attachments that we require when that we require for the smaller objects. If we do not have the milling machine then grinding machine then such type of machines then definitely with the help of these attachments we can perform the allied operations and we can perform a job of required ships. Thank you.


Holden Special Vehicles, known also as HSV, is an automotive design and engineering organization that works closely with original equipment manufacturers to enhance their products. The company credits its success to its international partnerships and relationships with around 50 international suppliers. HSV has invested in its workforce as well as digitalization projects to improve production efficiency and innovation. The company export revenue continues to increase, with new markets offering opportunities for future growth.


Hi everyone and thank you for joining in. My name is Christian and in this presentation I'll present the research that I'm doing during my IS fellowship at the August Institute of Advanced Studies. I'm an IS Co-Found Fellow and Assistant Professor at August Institute of Advanced Studies and here I'm researching in comparative animal physiology where I want to understand how animals function in the in the natural environments. And here I study a subgroup of animal physiology called respiration physiology with the goal of understanding how some animals can take up oxygen from the environment transported by the blood and release it to the tissues. And here I'm particularly interested in animals that have higher capacities to perform these physiological functions and try to understand the physiological and biochemical mechanisms that these animals utilize to better transport oxygen within their bodies. So the oxygen transport cascade is a multi step process where first oxygen is taking up into the bodies of animals either over the gills or over the lungs. It is transported by the blood to the respiring tissues and the final process or the final step in the oxygen transport cascade is the diffusion of oxygen from the red blood cell into the respiring tissues. And here oxygen is gradually depleted over distance so at the capillary wall the oxygen levels so the partial pressure of oxygen is very high. But when oxygen diffuses into the tissues, oxygen is gradually taking up into the cells and the oxygen levels are reduced eventually reaching zero so at a point where there's no oxygen left. And here the cells cannot function anymore because they don't have the sufficient amount of oxygen to generate energy to function. And for that reason, all the cells or all the tissues within our bodies have a very dense capillary network that allows for sufficient amount of oxygen diffusion into all the cells in our bodies so that they can function properly. This applies to almost all tissues but one particular tissue is special and that is the retina within our eyes. The retina is a neuronal tissue and the overall function of this tissue is to transform the light impulses that comes into the eye into a neuronal signal that can go into our brains and be interpreted as visual input. The retina has an inverted design and that means that light must transmit through all the different neuronal layers before reaching the light sensitive cells, the photoreceptors that line the back of the retina. And here you can imagine that any capillaries or blood vessels that are present in this part of the retina will scatter and scatter light and absorb the photons before the light reaches the photoreceptors and thereby reduce visual acuity. So for that reason, almost all vertebrate animals only have a network of capillaries in the back of the retina that allows for oxygen diffusion into the retina. But as you can imagine, oxygen is rapidly taken up so that reduces the the thickness of the retina that dictates visual performance. So if we look at the distribution of retinal thicknesses across different vertebrate species where each dot represents a different species, some of the visually poor performing animals such as blind cave fishes, particularly locating bats or electric fishes, they have very thin retinas and poor visual performance. And here our models for oxygen diffusion applies well because oxygen can easily diffuse from the from this capillary network into the whole retina. So if we look at some of the visually well performing animals such as hawks and eagles and and other birds and some fishes, they have a very, very thick retina that is over 600 micrometers thick, where oxygen can by no means diffuse over such long distances. And therefore these animals are interesting in terms of understanding physiological mechanisms to boost oxygen supply to neural tissues. So therefore I'm interested in understanding the physiological and biochemical mechanisms that allows these animals to boost their oxygen supply to neural tissues. These mechanisms may have supported the evolution of superior vision in birds and some of the other well visually performing animals. So to understand this I want to gain information about the physiological mechanisms that animals used to transport oxygen within the retina. I want to gain a molecular understanding of these physiological mechanisms, and I want to investigate this in a more comparative or evolutionary context. So there's kind of three different layers in my research. In the physiological studies I want to understand how oxygen diffuses within the retina. So here I can anesthetize birds and and other animals and insert a very thin glass electrode into the into the eye and gain information about the different oxygen levels that are that are found in different parts of the retina. And by fitting different mathematical models for oxygen diffusion to the data, then I can gain information about the physiological mechanisms underlying underlying gas diffusion. I also apply some molecular approaches to to understand the biochemical mechanisms underlying the physiological mechanisms for gas diffusion. Here use a technique called spatial transcriptomics where we can take a histological cryo section and put it on a gene expression slide where we can capture messenger RNA in the different parts of the retina. And here we can gain information about the transcriptomes in individual cell types within the body and also with relation to the to the oxygen levels that are found in the cell types. So we can map the expression of different genes on a retinal section, and we can also superimpose these oxygen levels that we obtained in the physiological approaches described before. And then we can go in and disentangle what are the effect of the of oxygen levels and cell types on the expression of different gene products. So this provides intricate information about how animals function in terms of supplying oxygen to their eyes. And here we gain very mechanistic insight into how animals function, but I don't just try to understand how individual animals function in isolation but also try to look at this in a more broader perspective. So here I study both birds but also their closely related reptile sister species. And by by knowing their phylogenetic relationship, so the tree of life that connects these different species. It is possible to track back in time how physiology and anatomy have looked in these internal branches so that represents prehistoric ancestors that connects these current living species. And by being able to mathematically backtrack how animals have functioned and looked, it is possible to reconstruct how anatomy, biochemistry and physiology have looked in internal branches of the tree of life, and reconstruct how physiological and soft tissue structures such as the I have evolved over time. This research provides physiological insight into the physiological basis for the evolution of sensory organs with a specific focus on vision. It provides insight into how prehistoric animals have functioned and looked, and it provides insight into how complex physiological systems have evolved over time, which has always been a test case in evolutionary biology. Furthermore, with more future applications, this research provides insight into naturally evolved mechanisms to boost oxygen supply to neural tissue, and this may have biochemical implications if we can translate some of these mechanisms into mammalian disease models. Thank you very much for joining in and feel free to contact me if you have any questions or comments.


Saba is kind of the, she's like the Wii Council guru in the school. To me, Wii Council has helped me not only understand my own privilege, but understand how to use it in order to help others on a local and a global scale. She really helps students grow. She teaches how to have initiative.  Wii Council enables me to teach them how to be change makers. It empowers the students to be the change that they want to see in the world. So through that, they can see that yes, they do matter. Their voices are heard and they can make a positive impact in the world. And as an educator, when I see that recognition, that is the most rewarding feeling.


Good luck. Hello, everybody, and welcome to the Latin American webinar of physics. Today is a very nice speaker that we're going to have here in the webinar cycle. It's going to be the webinar 141 of all the stories that we have here in the physics. So the speaker today is Valerie Donk from CERN, and she got the PhD from the University of Hamburg. And after that, she has done postdocs in SISA, in Trieste, and in APC in Paris. After that, she was a junior faculty at DESI in Hamburg, and currently, since 2020, she is at CERN. So Valerie that is here is going to talk about the asymmetries in the early universe. So, Valerie, welcome to the physics, and you can start your webinar whenever you want. Thank you. Thank you for the invitation for the opportunity, and also thank you for the nice introduction. Okay, so let me tell you about the symmetries in the early universe, and let me start by telling you what I even mean by these words in my title. So normally, let me first introduce you to the standard law about asymmetries, in particular about barion and lepton asymmetries in the early universe. So the standard thing that you'll hear is that we know very well the barion asymmetry, both at Big Bang nuclear synthesis and at CMB decoupling from the indirect measurements that we have at that time. And from these measurements, we know that at that time, the barion asymmetry was very small about on the order of 10 to minus 10. And now in the standard model, B minus L, so barion number minus lepton number, and B plus L are conserved below the electric phase transition. In fact, in the standard model B minus L is always conserved. And B plus L is conserved at low temperatures, and at high temperatures we have the spiral processes which drive B plus L to zero. So if you take together this information and you say okay well I know my barion asymmetry is small. I know that I have a dynamical mechanism that drives B plus L to zero, then you would conclude and say okay but then the lepton number obviously alters to be small right and can be at most of the same order of magnitude. So that's kind of where the standard discussion stops right, the standard conclusion is that any asymmetries in the universe or meaning any imbalance between particles and antiparticles is very small. And in particular is bounded to be of the order of 10 to minus 10. And these asymmetries, this imbalance between particle and antiparticle is directly violated or directly related to the amount of CP violation that you have in the early universe. So that's the standard story. Now I want to question a bit the hidden assumptions in this standard story. And they're actually quite many hidden assumptions. Because there's many caveats to the statement asymmetries in the universe are small. The first caveat is very obvious right the first caveat is that the B plus L asymmetry can easily be much larger at earlier times. And then okay we have this dynamical mechanism which drives it to zero at later times but maybe at the very early times, it could have been very big. And the question is, did that leave any imprint in the evolution of the universe. Then the statement that B minus L is conserved is true in a standard model. Strictly speaking, but as soon as you introduce right hand neutrinals, which you kind of want to do anyway to give masses to the neutrinos that we observe. You basically automatically introduce B minus L violation. And then again these these statements as I phrase them above here are no longer true. So given that one can then wonder if we have independent probes of the asymmetries in the early universe, which do not rely on these assumptions. Or maybe what's appropriate symmetries at different times. And one thing that we can check is the asymmetry in the electron neutrinos. Particularly during BBN. So during BBN we have the formation of the light elements and the formation of the light elements involves electron neutrinos in order to convert between neutrons and protons. And so having changing the amount of electron neutrinos versus anti electron neutrinos. This is this is a change to which BBN is very sensitive to. So we can check just from the BBN measurement alone without making any other assumptions. What is the sensitivity to an asymmetry in the electron neutrinos and actually the bound is surprisingly weak. So from from BBN and seem easy even weaker. Well, it's at a similar level so from BBN and seem the observations without making the assumptions that we made above. So we can just conclude that the asymmetry in the electron which we can parameterize by by chemical potential is smaller than about 10 to minus two, which is much weaker than the 10 to minus 10 that we had up here. And even that still has a caveat, because this is only true under the assumption that there's only an asymmetry in the electron neutrino and not in any of the other neutrino species. So if the asymmetry is also in the other neutrino species, then I will have my train oscillations, which will set in just before BBN. So at the time of BBN. The asymmetries will be relatively evenly distributed among the species. So I can imagine a caveat where I have the total asymmetries in all summed over all neutrino species to be zero so total left on number to be zero. I could still have relatively large individual left on flavor symmetry so I could have larger symmetries in the electron flavor, and then the opposite, but same value larger symmetry into me on flavor. And in that case we could not use this bound at all because the neutrino oscillation would have would have pushed these asymmetries to zero. In fact, you can check how strong is the bound from BBN on this case, and it's really only order one. And order one here like telling you telling me that the asymmetry is order one mean the chemical potential over the temperature order one really just means that there's there's no bound at all right because kind of an asymmetry like this this is expansion of the chemical potential doesn't even make any sense. It is it is numbers not smaller than one. So what I want to say here is that despite this kind of standard law that, okay, asymmetries in the in the universe or smaller 10 to minus 10 is actually not true. Right, or that there's cavities to that statement. And in fact, we can relatively easily construct scenarios where we really have very large asymmetries potentially order one asymmetries in the early universe. And that's kind of where my talk is heading today is is kind of wondering. Okay, is that actually true is it really true that we could have a completely asymmetric universe at early times. And we would not know about it today is is that really a true statement. And that's what I want to dig into a bit during during a seminar. So, why is that an interesting question to ask at all I mean one. Okay, it's simply kind of the question what can we actually observationally say about the early universe before we go into any any model building exercises. Then going to model building. Once, if you have this this possibility of having large asymmetries in the early universe that has consequences for barogenesis that have consequences for CP violating BSM physics that has consequences for face transitions because larger symmetries tend to change the temperature at which these face transitions happen. So it has knowing how large these symmetries can actually be in the early universe has consequences for a bunch of BSM models, and also, if you want to chase an ambulance or you can actually even chase a two ambulances here is that our recent hints, I would say, from from BBN and from CNB, which may point to large asymmetries in the early universe. So that kind of has made this a bit of an urgent question to understand what actually are the other asymmetries in the early universe. So the goal of the stock is the following so I will first talk about a bunch of relatively old stuff and the sunset I'll tell you about the ingredients that I need in order to make the argument that I want to make. And all these ingredients by themselves have been known for a while. I mean, some of them for a couple of years, some of them for 20 years. So I first kind of talk you through all the different ingredients separately that I need. And then I put them in the second part of the talk is the following so I will first talk about a bunch of relatively old stuff and the sunset I'll tell you about the ingredients that I need in order to make the argument that I want to make. So I'll tell you about some of them for a couple of years, some of them for 20 years. So I first kind of talk you through all the different ingredients separately that I need. And then I put them in the second part of the talk I put them together. And I show you how from that we get new bounds on the left of flavor asymmetries, which will mean that actually what I said beforehand that we can have these lot or the one asymmetries will turn out to be not true with just standard model physics we can put a new bound. And I'll also briefly touch upon implications for barogenesis. Okay, so let's start as I said by by a couple of ingredients that I need to introduce. And the first ingredient that I need to introduce is the standard model. And in particular the interactions and the conserve charges in the standard model. And as you probably will know this in the standard model above the electric phase transition this tree exactly conserve charges, which is hypercharge and the tree flavored be my cell asymmetries. But if we go to really the very early universe on top of these exactly conserve charges we have approximately conserve charges. One of the reasons is that, as we go higher and higher in temperature, means we go to faster fast expansion rate of the universe. And at some point to different interactions meaning the do cover interaction that this follow run process cannot keep up with the expansion of the universe. And so what this plot on the right indicates is the difference standard model interactions as a function of the temperature of the thermal that when they come into equilibrium meaning when they become efficient. So at very high temperatures, barely no interaction is efficient the top is the first to actually become efficient compared to the Hubble expansion rate. Over many orders of magnitude, all the standard model processes become efficient until the last one which will be an important one is the election you cover, which becomes efficient at about or we say it becomes into equilibrium at about 10 to the five GB. And that means that at any given point in this diagram I can basically separate my conserve charges or sorry my my effective interactions from my ineffective interactions. And for every ineffective interaction it means I get an additional conserve charge, or at least an approximately conserve charge in the limit that that interaction is zero. It means I, I turn off an interaction meaning I have an additional conserve charge in the system. And this just means I can rewrite this this plot as a simple linear algebra system, telling me kind of which interactions which efficient interactions relate the different charges and which charges on the other hand are conserved. So concretely, here, what I'm showing here is for different temperature regimes going from from cold to hot. Now we here have the different interactions that all the different standard model interactions, and the check mark indicates that the interaction is efficient so in the 10 to the five GB, everything except for the electronic cover is efficient. And every time when the chart something is not efficient right instead of the check mark I write the corresponding conserve charge. When we go up in temperature we get less check marks, so less interactions are efficient and we get correspondingly more conserve charges. And this is really just a linear algebra system right so the number of conserved charges, plus the number of linearly independent, equilibrated interactions, has to match the number of total total number of particle species which is 16. So what this means is that if I start at high temperatures, and I put by hand some asymmetry into one particle species, then I need to kind of crunch my linear algebra system. And this asymmetry that I put in one species will, following the, the constraint equations that I have in the system will be distributed among other charges in the system and then as a temperature evolves as different interactions become efficient. So there will be a constant reshuffling of the charges that I put in. This is really just this standard model at work. Okay, that was the first ingredient. The second ingredient that we need is the so called chiral plasma stability. So this is an effect in chiral magneto hydrodynamics. So the system that I'm studying here on the slide is I have a hyper gauge field so you want why I have a thermal plasma of particles. And now for asymmetry is in these particles PC so I will allow for chemical potentials. And I'm describing this in a very coarse grained way, hence the word hydrodynamics right so this is really an effective theory I'm not tracking the individual particles but I'm really describing this as a fluid. These in this MHD how this works is you basically couple classical Maxwell's equation with an effective current with sources is classical Maxwell's equation. And his effective current has the term you would expect, which is conductivity times electric field that's just the standard arms law current that you would expect. And the current also has a contribution, which couples the which is sourced by the velocity of the plasma and the magnetic field, right you can imagine if I have a magnetic field and I and I have the velocity then just the Lawrence force right in that that will give me a current. So this is basically what this term is is telling you. And then, finally, we have this last term, which is called the chiral magnetic effect. So this is a contribution to the current, which is proportional to the chemical potentials a particular linear combination of the chemical potentials which is called the chiral chemical potential. But basically, what I'm what I'm doing here is I'm summing over all the chemical potentials of all my particle species. Every factor here is the helicity, the multiplicity of that species and hypercharge of that species squared. This is the definition of the chiral chemical potential which enters in this equation. And this current here is proportional to the magnetic field. Now that is maybe with surprising right I mean normally you think currents are you understand normally currents are proportional to electric fields right or currents by the Lawrence force right come with a cross product with the magnetic field. So that might at first seem a bit a bit unusual but what's actually going on here is that this is the chiral anomaly equation. This is how the chiral anomaly equation appears in an effective theory of Maxwell's equations in this kind of fluid type type description. Okay, so this is this is the effective current now we plug this into Maxwell's equations. So now I'm going in the first step. Just for the slide I'm going to neglect this term here going to neglect the fluid velocity. And then you get a closed system of equations which contains the helicity, meaning that basically the magnetic field here, the energy in so this is the yeah so this is the, the helicity of the magnetic field, the energy density of the magnetic field, and then also I will have an equation for the chiral chemical potential, which I'm not showing here. So let's look at the two equations for the magnetic fields or hyper magnetic field. So, either here is just a conformal time. And in both cases you have, and I'm doing this in forest space so hence the index k. So the first term in both cases is the diffusion term. So this is what we expect or you expect that I have a plasma. The small scales diffusion is efficient meaning I will have some term which comes with a minus sign so it tends to erase whatever is there. And it comes with a case squared indicating that it's particularly efficient for small scales. Then however due to this caro magnetic effect. I also have a second term here, which is proportional to this caro chemical potential. Depending on the sign of the caro chemical potential right which kind of I designed depending on the asymmetries that I put in in the beginning. This term can have the opposite sign as determined front. So what that means if you, if you solve this equation is a couple of equations right but you can you can rewrite it as a as a just an evolution equation with with a math effective mass matrix. For each possible sign for each of the two possible signs of the caro chemical potential, there will always be one mode, which can become negative with what the effective mass squared term can become negative. So we can have one of the helicity modes, which in a certain range of k modes on a certain range of scales below like so scales above a certain value meaning k values below a certain value, given by the chemical potential. They become tachyonically unstable right and tachyonically unstable again means that they have an effective negative mass squared. So what this means is that you get if you have a system where you have a non zero chemical potential. You can get an exponential growth of magnetic fields. And this this is the current plasma instability right so the name instability comes from the fact that you're happy or something, which is a negative mass squared. So, you get an exponential growth of the corresponding gauge field. And so we can now estimate. How much gauge fields we can produce in this way. For that, we'd actually need to the second equation I'm not writing here so there's also an evolution to close the system we need to also know how this mu y five evolves right in this mu y five. Just evolves according to the caro anomaly equation so the change in the chemical potential is just given by ff dual so basically by by the helicity. So when you plug all of that in together what you what you understand is that as long as this caro chemical potential is non zero, it will source this tachyonic instability. So what happens is that whatever caro chemical potential we have in the beginning it will be completely converted into a helical magnetic fields. And this is given by this relation here so these these factors of temperature and alpha alpha is the hyperfine structure constant. So this is the hyperfine order one factor. They just come from these coefficients and these equations, but basically, and dimensional analysis more or less but essentially this this caro chemical potential will be fully this initial caro chemical potential will be fully converted into and because we can see here we have a differential equation from this differential equation we can extract a timescale, a timescale at which this conversion will happen and this timescale we can convert into a temperature, which is what I'm giving here so this temperature the CPI temperature is the temperature at which this process becomes efficient so at which we convert the chemical potential into helical magnetic fields. And this temperature is given by, okay, here we have just some constants which are the standard model values. But importantly, this temperature is proportional to the caro chemical potential squared. And for values of the caro chemical potential of around 10 to minus three, we find that this CPI temperature is about 10 to the five GV, which is the value at which the electron you cover comes into equilibrium. And that will be important in a second. So, we learned on the previous slide that if I put a particle, if I put an asymmetry somewhere in my system, it will be redistributed across all the particle species. And now we see that this asymmetry can moreover be converted into helical magnetic fields. Okay, then this is the second to last ingredient so this is the inverse cascade so in the previous slide I neglected the fluid velocity. And that because if I put in a fluid velocity back right so this Maxwell's equation is a priori linear equation. But if I include this fluid field which is in turn sourced by electric and magnetic fields, the system becomes nonlinear. And I can no longer solve it with linear methods. But of course, reality doesn't care about that right so in reality we have this fluid velocity. But what happens if I put this fluid velocity back in the system. So, what I said on this slide is kind of all true as long as this fluid velocity is small, which is initially typically the case, but then eventually when this process starts when I have this current plasma instability. I generate large magnetic fields they intern source this this velocity, and hence eventually I will come into the case where I need to take this into account. However, this, this fluid velocity, it does not only make like complicated it also has a very, very interesting effect. And that is called the inverse cascade. So, what the fluid, as I said this fluid velocity term and introduces nonlinear mode couplings, which means you can now transform energy from one mode of your gauge field into another mode. From thermodynamics logic without even solving any equations. You know that the system will want to go into a status where it minimizes its free energy. So we'll want to conserve Felicity because Felicity is an approximately conserved quantity in the system. So we'll want to conserve Felicity but minimize energy. And the way you do that is that you go to very long way like modes because long way like modes have the minimal energy per unit of Felicity. So the inverse cascade basically tells you that as soon as this fluid velocity becomes efficient becomes large, you can convert. You can kind of push your your energy and push Felicity to very large way like modes. And this is something. Okay, this is now very kind of hand wave the argument but people in particular these these authors here have simulated this in great detail on the lattice where of course you can account for all these nonlinear actions. And this is indeed what they find so they find that as soon as your your your magnetic fields are above a certain threshold, which in turn and triggers a large fluid velocity, this inverse cascade is triggered. And the Helicity is pushed to very large scales, which means is protected from diffusion because diffusion was only efficient at small scales. So we saw previously, asymmetry can be distributed among different particle species, it can be moved from the particle species into the magnetic field. So once it's in the magnetic field, it can be pushed to very large scales, avoiding diffusion and hence it can survive for very, very long time on cosmological time scales. Okay, and then the last ingredient that we need is that if this magnetic field survives until the electric phase transition, then we get a source of baron asymmetry. And the reason for this is basically that the current anomaly, so the the ABG anomaly, which on the left hand side of this current anomaly you have. Yeah, the change the change in in baron number left on number. And on the right hand side, you have the Helicity of the of the magnetic fields. And but now what happens at the electric phase transition and here I'm talking about a completely standard crossover electric phase transition is just because you project from hyper charge to electromagnetic charge, you're changing the number associated with the magnetic fields you associate with the master's you want to feel that you have in your system. And that means you're changing one side of this anomaly equation, but that means because the anomaly equation always has to be true that you always have to change the other side. Right so this is a kind of very high level view how to how to see that if you just have helical hyper magnetic fields present at electric phase transition. That will have to lead to a B plus L asymmetry produced during the electric phase transition. Now, you're producing this at the electric phase position was precisely the point in time with his fellow runs the couple. So if you produce this asymmetry much earlier, you wouldn't care because this fellow runs will just wash it out. Now you're producing it just at the time when his fellow runs are decoupling. So there will be a competition between a source term, which is driven by these helical fields and a wash out term which is driven by this fellow runs. And this competition is encoded in this in this in this pre factor here, which I'll talk about in a second, but up to this, this, this pre factor which really depends on the details of the electric of how exactly the electric phase transition happens. This means that the entire Helicity present will up to some order one factor the entire Helicity present at the time of the electric phase transition gets converted into a binary symmetry. Now we can use the. So here, now I'm just plugging in some numbers. So this this term as I said it depends between the competition of the source term and the wash out term, and there's actually some significant theoretical uncertainty and that I would say plus minus. One, two orders of magnitude, at least, but taking the kind of the central value for this for this number, and just plugging in the constants here. We see that we can, we expect to get a binary symmetry, which is about 10 to minus six times the Helicity in units of temperature. And then we use the previous expression how we related the Helicity to any initial chiral chemical potentials. And we see, so this was just to remind you this was this this expression here. Now just plugging in some numbers. And I get a factor 10 to minus four here. Meaning, if I have really order one chemical potentials this equation tells me that I expect a binary symmetry of order 10 to minus four. This would be ginormous completely going against observations. So this this is kind of the logic of what I'm going to be presenting in a second right so as soon what the take home message here is as soon as you have chemical potentials which are larger or particle asymmetries which are larger than 10 to minus six at any early time in the right, it can be way before BBN way before CMB. Then this equation tells you that you are at least in danger of massively over producing binary symmetry. Now, and that's to be contrasted with what I told you beforehand right that I was setting for that kind of current bounds basically telling you, you can have order one asymmetries and and there's no constraint right so here we're seeing okay once we actually take these different ingredients together, it potentially is a constraint. So let's have a have a closer look at this issue. So, so just to recall the the ingredients that we have so far right so so far we said, okay it's done a model interactions reshuffle particle asymmetries, the carol plasma instability converts these asymmetries into electricity. Then with the inverse cascade the solicity can survive until the electric patient position and at the electric patient position, it can generate a potentially large burn asymmetry, potentially contradiction with observations. Okay, so now let's use this concretely actually now set bounds on asymmetries in the early universe. So the situation. Okay, so the situation I want to focus on just for simplicity is the temperature range. Just above the equilibration of the electron your cover, you can also do this in any other temperature range right and you can also look at any other combination of the symmetries. But let's for some simplicity this is some this case let's focus on that. I can compute the carochemical potential at that point where this is just the formula taking into account the hypercharge and the multiplicity of the particles and all the, the interactions that are efficient or not efficient. And this is what I get right so there's, at that time, there's two exactly conserve charges in the standard model which are the two, the sort of this tree right the tree B minus ellisometries and here, because they come with the same coefficient I've combined them right so this is the B minus ellisometry electron and this is the B minus ellisometry in the mu and plus town and then I have one approximately conserve charge which is the electron itself, the right hand electron. In principle, of course, I will have hypercharge right but I said hypercharges Europe because I do want an electrically neutral university and and now importantly we see that the coefficient in front of the electron B minus L and in front of the mu plus tau B minus L is not the same. And the reason for this is obviously that the new cover couplings associated with mu and tau one equilibrium and the new cover coupling that this current plus my stability happens before the electron goes into equilibrium, because once the electron goes into equilibrium, this equation no longer holds. And in fact, then, once all the standard model actions are our equilibrium. The, the, the interactions then dictate that this kind of chemical potential is way zero. So I can only have this car plus my stability above this temperature. Once kind of the would be temperature falls below this value which just means it just doesn't happen. But that's one condition but I gave you earlier I gave you a formula for the CPI right so this this temperature formula somewhere here right and we saw. It's this is why it shows this benchmark value right and now we see it was proportional to mu squared over 10 to minus three. So clearly I need to, in order to have this temperature above this value I need mu five above this value. So going back to now our complete example I plug in the numbers. And I find, as, as you would have just expected by looking at the previous equation that I can, the carousel plus my stability happens. If, and only if the chemical potentials in the individual B minus L flavors are above 10 to minus two. So that's one condition. And then the second condition is okay let's actually overproduce bionic symmetry right so now let's actually compute this bionic symmetry right so this is this, this expression here, a plug in the numbers here. Okay, we overproduce if this value is larger than 10 to minus five. So, clearly, this is the is the stricter constraint, right. So the statement here is, if the carousel plus my stability happens, meaning if the chemical potentials are above 10 to minus two. Then we massively overproduce binary symmetry we overproduce binary symmetry by several orders of magnitude. Right, which is also why we don't have to care in great detail about this uncertainty in this father on processes and the production of this symmetry right because we massively overproduce as soon as we hit this threshold we will produce. So the conclusion from here is that this is the bound one should consider. And that we cannot actually have order one asymmetries in the flavors in order one flavor symmetries, but as soon as the flavor symmetries are bigger than 10 to minus two. This is actually ruled out from just our observation of binary symmetry. So this is a bound which is two orders of magnitude stronger than the than the beyond bound for this particular case of a b minus l symmetric universe. Okay, because it's a nice result I put it again. I put it without the implications of this. So, as I said right so did this bound always applies independently of if b minus l is non zero or zero. If it's non zero. It's the bound is of similar strength than the bound that we already had from bbm just on the electron neutrinos. But it applies in a completely different temperature range and it's derived in a completely different way so in that case it's just an independent bound, but often similar strength. In a particular case of b minus l is zero. Then actually it's it's a factor hundred stronger than the previous bound. It applies the previous bound applied at bbm temperatures right or at CB temperatures. These applies at temperatures larger than 10 to the five GB registers really constrained on a primordial symmetries. So even if you have larger symmetries, which are then washed out over the course of the universe and they're completely washed out by the time you get to bbm, then bbm will tell you, you have no problem. But here, yes, you could still have a problem right so even a symmetries which are only present in the early universe and then get washed out via this mechanism because we kind of hide the symmetry in the magnetic field, in which it's very well conserved that can still cause issues by overproducing burner symmetry. Then now the helium anomaly that I was mentioning so the bbm anomaly suggests right I mean really suggests there's going to be even a slightly too strong word right so this. I mean this helium anomaly keeps on coming and going coming and going every five to 10 years right so not sure how seriously want to take it and I'm not not an expert on the observational observational data here. But if you take it seriously the simplest explanation to explain the data face value is to introduce an asymmetry for the electron neutrinals. And that would require an asymmetry of 10 of four times 10 to minus two, which is slightly above the bound that we put right so I would at least say we disfavor this explanation. However, there's a caveat right because here you need this asymmetry at the time of bbm, we only put a constraint a temperature above 10 to the five TV. So if you generate this this asymmetry below 10 to the five TV we have nothing to say on it. So that I'm not saying that is completely impossible to explain the helium anomaly with chemical potentials but I'm saying if you do want to explain with chemical potentials you have to make sure that you generate them below 10 to the five TV. The bound also disfavor some models of left the flavor Genesis where the idea is that you have larger symmetries in the individual flavors and then they basically leak slightly into some final be my total be minus a little symmetry, but that you need large initial symmetries in the individual flavors and again is in tension at least with this bound. You can of course, I mean, you can like I talk about bounds right because I think that's the more the most robust thing that you can do with this results but you can of course always play the game and say okay well if I have one region of parameter space where massively over produce. And then I also have another region of the parameter space where I obviously underproduce where just if I take this asymmetry to zero. It has to be physics as continuous right so there has going to be some regime but I'm just marginally satisfied is bound, but I can theoretically use this to get the correct burn asymmetry. Now it's probably going to be a pretty horribly fine tuned model, but in principle, you can you can think about building by Genesis models in this way. So we are the result is very sensitive to the exact dynamics of the car plus visibility but is less sensitive to the dynamics of the electric phase transition because as soon as we trigger the CPI, we are pretty confident that we massively overproduce. And on a more conceptual level. What we're actually doing here is if you think where the current where bound on the minus L violation comes from a bound on B minus L violation comes from combining our knowledge about solar ones which while a P plus L with the observed by an asymmetry. This is kind of the standard. How we constrain total B minus L. And now what we're doing here is conceptually actually very similar but instead of using the non perturbative as you to processes we're using the non perturbative you want why it processes, meaning this the CPI. So, if you combine these processes again with the observer and symmetry, you get a bound, which is again a bound on a linear combination of chemical potentials, but it's not the linear combination which is B minus L it's a different linear combination. Here I'm using it to constrain the flavor B minus L symmetries, but you can use it to constrain whatever right I mean it just a bound on some particular linear combinations depending on the temperature of chemical potentials. Okay, so that was the, the first two points, which is actually what I wanted to spend most time on me just more briefly talk about possible implications that this could have for for barogenesis. And the first model I want to start with is this axogenesis model. So the in the axogenesis model.  And then eventually at the QCD phase transition, kind of little QCD potential will show up here at the rim of the hat. And then you get back to the to the to the. And then you kind of start producing axon dark matter and these things. So you can get in this in this model here is that you can you can have two interesting consequences of this so one you can produce once we're in the room of this hat and once the QCD potential potential appears to add to QCD scale, and you can produce axon dark matter via the kinetic misalignment mechanism so it's called kinetic misalignment because we have this high velocity in the game. And also because you have this axon like field, which is rotating very fast, which means it acts as an effective chemical potential to the fermions in a game, you can also generate barogenesis to this this mechanism of spontaneous this. So simply true the coupling of the different fermions species to this rotating axon field. And this model is very simple because all you do is add an axon like particle with a specific initial condition. And then in principle you solve two problems to solve axon dark matter you solve by an asymmetry. However, in the simplest model you can't get both simply quantitatively you cannot right so either. You get the axon dark matter right but then you underproduced by an asymmetry, or you get this right but then you overproduce dark matter. There's ways ways to fix that right but in a simplest model this is a story. This model has two regimes. Here up here right when you're before you settle into the room and once you settle into the room. What is important for our purposes is that as soon as you have this rotating field. That's a degree of spontaneous CP violation right it induces chemical potentials and all the particle species and hence it can trigger the carol plus man stability. And if this rotating fields. It's supposed to continue for a long time right it's supposed to continue rotating way all the way down until the QCD phase transition because otherwise it can't generate the axon dark matter. So that means contrary to what I discussed before and right before and I said okay let's put some God given chemical potentials in the universe and see how things evolve. I have an active source term all the way down to the QCD phase transition. So I can in principle trigger the CPI now also below this magic number of 10 to the five Jeff, just because I have an active source term in the system. So this this makes us think that. Okay, here this this model definitely is one of the models that are at risk of triggering the carol plus man stability. So we expect that there should be constraints on the parameter space from the fact of not over producing burn symmetry. So that's what we did. So, yeah, so we, we distinguish two phases right so first at high temperatures before the settling temperature when this inspire phase and then below the setting temperature we're in the local minimum to make Mexican hat. The dark matter production happens around the QCD scale which will be lower than this setting temperature. And the amount of oxygen that you produce is just directly proportional to kind of the initial velocity of the field that you put the carol plus man stability on the other hand happens is most efficient at any time so before the settling temperature. So we can use the formulas I was showing you beforehand to compute the the CPI temperature for this particular model. And we can do the goal now is so previously I said we can avoid the CPI. If we go to temperatures below the equilibration of the electron you cover. It's definitely different right because the electron you cover temperature doesn't actually matter because we have this active source, but we can avoid the CPI if we go below this the settling temperature. But if we're both the settling temperature the CPI will happen. And then what we find again is similar to what we found previously once the CPI happened is just so efficient that it tends to just overproduce the burn symmetry in the entire parameter space. The constraint that we will set is basically this condition here. Does the carol plus man stability happen before this field settles into the room or does it not right and if it happens before that parameter space is going to be dead and if it happens. If it doesn't happen before then you're safe. And this is what this looks like in this parameter space of this model so here you have the the axiom decay constant and the mass of the the radio degree of the Patrick Quinn field. For some particular actual model right in this case the supersymmetric ksvz model. And the white parameter space is the allowed parameter space. This green constraint and the purple constraint are constraints which were previously known. And our new constraint from the overproduction of the binary symmetry to the CPI is this red region here. So, as expected you find that part of the parameter space is going to be excluded, which tells you you know that there are models out there, which were not invented with this in mind right but were invented just to do barogenesis. In principle, the parameter space they automatically come with such large chemical potentials such large CP violation that they actually violate the bound that we put. And, again, you can in principle you can play this game right and say okay if you're exactly on the boundary of this line. Then, in principle, you get the binary symmetry, exactly right. But it's going to be very fine tuned situation, but given given that this model kind of shines because it's it's very minimal. So, for a careful choice of your parameters you can with a very minimal particle content right meaning just an accident like particle nothing else, but very specific initial conditions and very specific parameter choice. You could in principle get both dark matter and barogenesis right. So you'd have a fine tuning problem you definitely have a fine tuning problem. But in principle you can do it with a very minimal particle content. Okay, I think, I think I maybe stop there. I'll give it more time for questions. So let me jump to my summary. So, what we saw is that any spontaneous CP violation in the early universe be it by chemical potentials that I put by hand right or that I put by some pre-barogenesis mechanism I put for example by gut bar, gut barogenesis. So these these types of chemical potentials or also some rotating field, which violates CP all these types of spontaneous CP violation. They can trigger this kind of responsibility, which then together with the inverse cascade leads to a production of binary symmetry that can be good that can be your model barogenesis what can be bad because it overproduces. And using this we set a new bound on the primordial B minus L conserving left on flavor symmetries of 10 to minus two. And we also see that we can get constraints on this axogenesis model or more general constraints on the axon kinetic axon kinetic misalignment mechanism. And, but in a broader sense I mean this I really just see this as both both things that I explained I basically see just as examples right because this is this the framework that we're using is I think much more general. The framework tells you if you have any model which is any sort of large symmetries in the very early universe, then you can use this to put constraints and potentially constrained part of your parameter space or maybe also turn it into viable by genesis model. Okay, thank you. Thank you very much. So, we're going to start with the question we have a couple of questions in the, in the YouTube channel. So, in the meantime, just remind to the people that you can follow us in the YouTube channel just to click the subscribe button to keep updated with the latest webinar that we are going to be programming during the, the, the year in this season. So, let's start with with some questions I don't know if there are questions from the audience here Alejandro has a question. Please, go ahead. Thank you for this very nice talk. I come from a very different field so my questions are perhaps more conceptual so if I say my question is tonight please apologies. Is there a way to understand physically that efficiency versus like how many charges do you have I think that you said like less efficiently means you have more charges. Is there a way to understand this. Yes, yes, so just imagine. This is what you're talking about right. Right. So, so imagine you have, you have a linear algebra system of, of equations. Right. And you simply have a number of equations, right which relate, which linearly relate your charges and set them equal zero right so basically I don't know an interaction of all involving I don't know a hex, turning into whatever let's say a neutrino going to a Higgs lepton doublet right would that written as an equation would mean a chemical potential of the neutrino minus chemical potential of the Higgs minus chemical potential of the lepton doublet equals zero right so very very simple type of equations. So just it's going to be some linear combination of my chemical potentials equals zero when that interaction is efficient. And the more interactions are efficient, the more equations you have simply and if the interaction is not efficient you just remove that equation from the system. And now you have a fixed number of particle species. So the number of equations that you're imposing in your linear algebra system is changing. And simply the fewer the fewer equations you have right and the system is on a constraint, and you just have more parameters in this case more chemical potential that you can just really choose. And something that you can freely choose is in this language a conserve charge. Okay, but so so so my my second and last question then related to this I was trying to think about this exactly is, you know, like this chemical potential in some sense are associated to something that that a number density of something in some sense. Yeah, that doesn't mean that the cattle charge is conserved. And if that's not the case then this cattle can potential. Is it really a potential. I don't know, sorry, I did this is not what not well posed question. The question is more about the origin of this carol potential. If it's associated to a carol charge, and if this is not conserved, or if it is. Okay, yeah yeah okay so the carol chemical potential is a linear combination of the chemical potentials of the individual charges. Right. Okay. So, the chemical potentials are only conserved in this manner right so they only conserved within. So within a given given temperature regime right so say I'm here 10 to the age, GB right, then I have a set of interactions which are completely efficient, and a set of interactions which are completely inefficient. And as long as I stay in that regime, or the individual chemical potentials are conserved, and hence also the carol chemical potential is conserved. But then when I cross one of these lines, I add a new interaction into the game, then all the individual chemical potentials will change and correspondingly also the carol chemical potential will change. So every time you cross a threshold here, you kind of will go down like we will be some sort of step, step function type function. I see. Okay, thank you. Thank you. Thank you. So, before that, if there are other questions from the audience here in the Zoom session, we have a question from YouTube from Adila Afzal, he said hi thanks for the very nice talk. Can you please comment that during the process of exogenesis, do we have the domain world problem? Ah, yeah, that's a very good question, right? So here, okay, so with the domain world problem, it depends when you break the, when you break the petroquin symmetry associated with the axon potential versus inflation. Right, so that's always the story. So in this case, the idea is that we first have inflation. What, sorry, the idea here, okay, the idea here is that here we have, we never restore the petroquin symmetry, right, so let me go to the plot. Right, so here we never discuss the situation where the PQ symmetry is restored, but we always really just work in the picture where the PQ symmetry is already broken. Right. And then in that, and so kind of our initial conditions are really when we start outside here in the room of the Mexican hat. So in that sense, so I don't know we have we have anything new to say on under the main wall, a problem here right so it depends of course on the on the on the number of the main ones that depends how you align, how you do the time watering right of inflation and this mechanism, but we don't have anything new to say on the issue here. Okay, thanks. I'm later maybe Adelaide is going to say some comments about something later. Okay, I don't know if there are questions. I have a question about the, when you were discussing about the role of action in the mechanism of the exogenesis, let's say, what would be also the possible role of other type of particular particles in the, in this scenario I mean, is it possible to generate the same asymmetry with the, let's say, my room from related with the left arm, left arm. Yeah, yeah. Charge or other role of other type of action in granularity five theories or something like that. Yeah, yeah, totally right so I think so from the from the simply from the point of view of generating particular symmetries. And then from the point of view potentially triggering the carol plus for instability and so on right it doesn't have to be the actual QCD action right I mean, and then I think this this goes to me then you know if you have any particle right then you have to specify what how exactly you are going to come into the center of particles. And your constraints will depend on on how what those couplings are. But then the that is not at all specific to the QCD action. I think what what is nice here is why I mean the motivation to use the QCD action is then okay you'll kind of get the documentary for free. You know it's solved the petty Quinn problem right. But that's really just out of minimality and all the more conceptual questions of generating an asymmetry and how does asymmetry propagates from a different phase of the universe. You don't at all need this to be the QCD action for that. Okay, thank you. Yeah. Okay, the idea of the, I understand that the, the best scenarios to talk with the minimal to start with the minimal setup with this. So I don't know if there are other questions in the adela he said thank you to you for the for the answer. I don't know. Joey, if you have a question. I have a question. So, so, in principle, if you. So here you're assuming standard cosmology right but if you assume a non standard cosmology and Roberto will laugh because we've been discussing this elsewhere. If you have like, like entropy injection, right. Could that decrease your, your bound, if you have like a scalar that will decay some matter domination part that will be came to radiation could that a decrease your, your bounds. So, okay, so in the. So in print. Okay, let me first answer in the more general way right so let's forget about axogenesis and just kind of talk talk about the whatever this bound here right. So here in, in principle, yes, right because I mean here, we're saying we're overproduced the problem we're overproducing binary symmetry right. So of course that's a problem you can you can try and solve by by entropy injection. Though you do need to kind of check how the scaling of everything goes with with temperature right because it's all the same. It's all about right because then, like, you'll be. Because then then then you have to see is this actually, I mean, then you would you would what I'm saying is you also have to take into account the entropy injection when you, when you discuss of course how the asymmetries evolves. It's all about time right so there's kind of going to be the actual symmetry in the early universe and then there's going to be kind of the symmetry at later times. And you need to connect, connect it to. Right, but so definitely depends right definitely here we're assuming a standard cosmology right and if you have entropy injection that that would change a picture. In the exogenesis model it comes a bit automatically because in the exogenesis model you can have a phase of matter domination inclination domination. So they're so the individual calculation we have to actually go beyond the center cosmology right and really check explicitly the evolution of the quantities and really check explicitly to two different scaling regimes how the boundary symmetry evolves. Okay, I'll think about that. Thank you very much. Okay, so okay in YouTube we don't have any other question I guess also for the for the time of the, for the length of the to keep consistent with the, without previous webinar, we are going to start finishing here the webinar so first of all, thank you very much for the, for the interesting and for all the people that are following us in YouTube, you can, of course, you can explore our YouTube channel and check the previous webinars and also to continue to to assist into this to attending to these webinars in the future. So, I hope everybody is going to be fine and see you in the next time in this physics webinar.


My little nub in here is about to have surgery and be in a cast for four weeks, unable to move meeting, using my prosthetic legs out the window, my walking crotch malt work which means it's back to my roots baby, good ol' underarm crutches. So I want to show you my favorite accessory for these. As you can see these are pretty old and broken down and not super comfortable. So I've done this for years, I order these off Amazon, not sponsored, these are 24 bucks, I'll leave a link in the description. But they're these little crutch pads that make it way more comfy cozy and also cute. If I had colored preferences normally, you know I would go with purple but I was just stealing the camo this time. You just pop them on, velcro it on up, and say goodbye to those underarm rashes I used to always get by using these without pads on them. Thankfully I have tons of experience using crutches on this side so now that the pads are on, we're good to go.


Welcome to Toffey TV, it is the Everton News daily. The news today is that Everton have appointed Lang O Rourke as their preferred contractor to build the Bramleymore Dock Stadium. They will hope to utilise their digital engineering team and also in partnership bring the design and delivery programme to put the stadium in place. There's also been some of the planning permission specs on the Liverpool City Council website today with the full timetable. If everything goes to plan with the planning permission they will hope to begin the demolition of the site in September of this year and hopefully start to build the stands November December time with the stadium due to be completed for final testing in July which would mean a six week final testing period to have it open in the first week of September 2023 which could see Everton obviously starting the season at home late. Possibly it might mean that we have to play the first few games away from from the new stadium but obviously we have to wait and see. The testing period could be quicker than that I'm not really sure but that is the time table as it stands if everything goes to plan and as I said we're hoping to find out in May or June time whether Everton's planning permission has been successful or whether it will be called in by the government for more inspection. I'm sure there'll be more details on that once that happens and the timetable will be adjusted or there might be some time that it's been built into the programme for that eventuality we'll have to wait and see but it's getting exciting we're finding out more about the stadium week by week and if you see the plan and permission forms so much gone into this that obviously tells you that this isn't just a publicity stunt which has been said so many times to me by Blues and Reds and it does feel like it's moving forward now so where Lango Roach is the preferred contractor to build the Bramley Moor Dock stadium which is really really good news to find out more about that on the Everton website. Man City are hoping for a summer decision on whether they will play in the Champions League next season obviously this could affect Everton if Everton get into the European places if they were to finish fifth at the moment that would mean Champions League but obviously if Man City get to play in the Champions League next season that would be Europa League place and obviously if Everton were to finish eighth and Manchester City win the league cup and one of the top five win the FA Cup or top six it would be that would drop down to seventh and it would be eighth if Man City on in European football so this does concern Everton massively they're hoping as I said to find out they're going to throw everything at your way for now legally to get their ban kicked out it could see FFP kicked out as well hopefully it will because it's nonsense as far as I'm concerned and it stops clubs from Everton like Everton from trying to build as simple as that so we'll find out in the summer and another news Everton have been linked with Marash Cumbala today a centre back from Hellasferona in Italy yeah lots of rumours of it there's always rumours in Italy and obviously there's loads of rumours about centre backs with Everton at the moment as well because everyone knows we're going to be looking for one in the summer or certainly trying to buy one in the summer so we're going to be linked with lots and lots of centre backs between now and the summer time so there you go big news today Langill Rock are the preferred contractor for the Bramley Moor Dock stadium there you go let us know your thoughts in the comments give this video a like subscribe if you haven't already and if you want more great videos join us over on patreon the link is in the description see you later


The life of homesteading, the life from the land, works on a completely different logic, works on a completely different rhythm. There's completely different forces that shape how you live your life. It's very different from the technological, media-saturated hustle of suburbia. That was what we realized in the shape of the book is sort of if you wanted to live on a homestead, if you wanted to live closer to the land, or if you even wanted to sort of have the lessons from it at all, just recognizing that whatever we're doing now, there's some deficiency. What it does to the family, particularly in individuals, is pretty clear if we really look at the history and theology of how God wanted us to live. There are things he teaches us and wants to teach us that we learn from the land, and there is no other source.