 So thank you everybody for joining us for our fourth press conference of the EGU General Assembly 2024. My name is Hazel Gibson. I'm the EGU's head of communications and I am delighted to welcome you to hear from our excellent speakers that we have joining us today. Just a couple of housekeeping items. First of all, if you are joining us online, welcome. And if you could please remember to mute your microphones, we will be going through the presentations from our speakers together and then we will take all questions and answers at the end of that time. At that point you will be able to unmute your microphones and ask questions directly of our panelists, or you can write your questions into the chat and I will be able to ask them on your behalf. Obviously, we will also be able to take questions from the room if anyone wants to ask direct questions there as well. So I would like now to introduce our two speakers today for, sorry, excuse me, press conference number four, which is titled by Jove new revelations about Jupiter's planetary system. Our first speaker is Chris. Oh, and I'm going to mess this up again. I'm so really sorry, Chris, I'm very sorry everybody. Chris Abdelidu who is from the School of Physics and Astronomy in the University of Leicester United Kingdom and Scott Bolton from the Southwest Research Institute at the United States of America. We will start first with Chris. So thank you very much. Thank you. Okay. Thank you. Thank you very much. Thank you for this invitation and thank you everyone who is here or connected to listen to our story. Thank you for the introduction. Yes, indeed. I work now at the University of Leicester in the UK. However, this work started many, many years ago while I was still postdoc at the Observatoire de la Côte d'Azur in Nice in France. That's why the double affiliation and this work was done together with my good colleagues, Marco del Bono and Alessandro Morbidelli also from Nice in France. And of course with our colleagues from Southwest Research Institute in Boulder, Colorado, David Nesswarni and Kevin Walls. So I was very proud to be in this work with all these dynamics is there, although I come from a different background on small bodies and compositions and impact studies. So I will try to keep this presentation as easy as possible by telling you a story because this work started really many years ago since 2017. And I will have the proper presentation later today and the session of small bodies and dust this afternoon and we're expecting our paper to be out three minutes ago. So, okay, let me start the story. This is in the asteroid belt with which is what you see here in this plot. It is between the orbits of Mars and Jupiter. They reside millions of of asteroids of small bodies, which they show diversity in their physical properties, their masses, their diameters, their spectral signature, which is a proxy, first proxy for the for the other composition. And in this specific plot, each one of the dots is a different asteroid and you can see here at the color map, we try using their spectral data from ground based observations but also from the Gaia mission of the European Space Agency. We paint them with different colors denoting more or less their composition what we think they are. And we can see also by eye, I hope it is obvious that there are some higher concentrations of density of objects in the main belt and this we call them asteroid families so what are the asteroid families in the main belt during its lifetime and several collisions between the small bodies and the fragments they share similar orbital elements but also they can share similar composition if the body of course is homogeneous. That's why you can see them in these plots nicely concentrated. So, our team discovered an asteroid family in the inner part of the belt is where you see the red circle, which was generated by an impact event about 3 billion years ago. For this result was published in 2019, so for almost 5 years since 2017 I was doing ground based observing it with ground based telescope to obtain their spectra in order to understand what is the composition of this family and then to connect it to link it if possible with meteorites. This family is called Ather, the name was taken by the largest fragment inside the family, the largest asteroid member. By comparing with meteorite data, we link it with a very rare type of meteorites which is called anesotite chondrites and this was an important discovery because this source is the only one that we have found so far in the whole asteroid belt. And the anesotite meteorites are the ones that have the closest composition to our planet. However, with this study we found two little problems. By trying to put back all the material together and understand what was the initial size of the parent body that generated this family, we end up with a small object in diameter. However, our colleagues that they use the anesotite chondrites meteoritic data with their modeling, they state that no, the parent body should be much larger, a few hundreds of kilometers in diameter. So we have one issue here and the second issue is that we know that this material, this body should have accreted close to the orbit of Earth, but why do we see it now in the belt? Our working hypothesis is that the parent body of the anesotite meteorites were formed close to the orbit of the Earth, then it should have suffered a first collisional event in one of the fragments which is the asteroid family progenitor of Athor by a dynamical process should have been implanted in its current location in the inner main belt. However, what we try to do with our present study that we show today is which was the dynamical mechanism that managed implanted inside the belt and when did this happen? So we did, we combine this meteoritic data, ground based observations of small bodies, we expanded the thermal modeling of the parent body of the anesotite chondrites and then we performed a series of dynamical simulations in order to study different scenarios of how this object can come from the terrestrial planet region inside the belt. So what we found, we concluded that the parent body of the anesotite meteorites was implanted in the asteroid belt during the orbital stability of the giant planets. So colleagues of our work from Boulder, they had another recent study that they put the upper limit of the giant planet stability that was first proposed in the NIST model 20 years ago in the same institute now that we did the study 20 years after. So these colleagues proposed that you cannot have an instability later than 100 million years after the formation of the solar system. I remind here that the NIST models at the instability probably happened around 600, 700 million years after that and it was responsible for the late heavy bombardment of small bodies on the moon. So now we have the upper limit from our colleagues and our study shows that the lower limit, the earlier time that the instability should have happened is around 60 million years. And we said this time because the parent body of the EL contract could not have its first breakup here earlier than this time, otherwise we wouldn't have seen the anesotite meteorites as we see them today. It needed at least 60 million years, this initial body to cool off after its accretion in the terrestrial region. So you form the body, you have to wait 60 million years, then you can break it and then a fragment is implanted by the giant planet stability in this window. So what we did then in summary with the study is that we timed now more precisely the instability to happen in this window. We have several other corroborating evidence for this window and our work excludes an earlier instability. There are some other studies that they propose the stability that happened about 10 million years, so much, much earlier. However, our work excludes that by using a lot of observational and meteoritic data. And another thing is that the major event that happened in the terrestrial planet region at this time window, it was the formation of our moon. So we had a fifth object at that time that we call it Thea and this at some point impacted our planet giving it almost its final mass and then generated creating our only natural satellite. So there have been some other studies in the recent years that they showed that this can happen. So the giant planet stability could trigger the moon forming event about 10, 20 or even 30 million years after its occurrence. So and we have data from the samples from the moon that they say the moon should have formed, you know, in this window. And now we see that with our study we coincide very well. So thank you. We will now move to our second presentation with Scott Bolton. Please give us a couple of minutes to get the slides up. Thank you for your patience. Okay, so I'm going to talk about some results from Juno Juno is currently in orbit around Jupiter right now it goes in a polar orbit and this is one of the images that we get. And there you see the familiar great red spot. Just a piece of the picture. So I'm going to talk a little bit about what we're what's called our extended mission. So here's a plot that shows our orbits. And so you're looking sideways Jupiters the big object in the, or the right side there, and the gray orbits are all prime mission and what's happening is Jupiters is twisting the orbit what's called the line of cities around. And so the Parajove, or the part that goes close to Jupiter starts moving north about one degree per orbit, and then. And then eventually we cross where the way the, let's say this pointer works here. The orbit moves this way goes over the pole, and then out the south over the North Pole. And so that's how we flew by the satellites is this orbit was evolving. And so I'm going to show some some results from a recent flybys of IO, which is the most volcanic body in the solar system. And, and I'll also show some atmospheric stuff on Jupiter, which comes from the fact that we're getting very, very close to the North Polar region. Okay, so the first thing I'm going to show is a is a photo. We have a camera on board. It's called Juno cam. And we take all that data and it goes onto a website and actually public. People make the picture. So all these pictures are made by the public this one in particular is actually made by one of the scientists on Juno, but most of them are all posted and anybody that's listening or any of the readers of your photos can go on to our website mission Juno.com and actually get access to the pictures the raw data or you can just Photoshop somebody else's picture. And when you make the picture you are the photographer so you actually have the copyright even and you can assign that copyright. The only thing we ask is if we posted on the website. NASA and scientists are allowed to use that image for science but otherwise it's yours to do what you wish with. So, this is a pretty fascinating picture because it's showing IO IO is very close to Jupiter it's orbiting at about five radial distances of Jupiter away so it's actually pretty close Jupiter is massive. It's huge three over 300 times the mass of earth. And so it's squeezing this, this small moon which is a little bit bigger than our moon, about three kilometers in radius. And what you see is this is mountains so it's actually got a mountain building going on your look along the terminator here and you can see the shadows, and I'm going to show some stuff on that. And then you see the colors here these are a little bit stretch but they're real that you see these reds and yellows and a little bit of green and that's because this body is the is actively spewing out volcanoes and that's going to be part of the story today. And those, you know, the sulfur like if you were to go to a volcanic place on the earth, it smells pretty bad and it also looks quite colorful. IO is no different. It's, in fact, other than the earth it's the only place that we see active magma volcanoes going on in our solar system we haven't seen another. We see things that are leftover but they're not active. IO is actually doing it all the time. Okay, so another picture is something I want to point out is we see this mountain right here. It's very intriguing to get this because this this dark part is the shadow, the sun is coming in from the right side, and you can see over here, it has a very sharp peak, and that was very intriguing as that what could make that shadow. And so I like mountain climbing and skiing and snowboarding. And when I see something like that. I'm very intrigued about what it would be like to go there. And also, I should mention that IO is very cold, because it's in the outer part of the solar system so the surface of it is probably minus 100 degrees Celsius or something in that neighborhood, whereas the magma courses might be 1000 degrees coming out. But it's when it comes out, and a volcano goes off, it immediately freezes and probably make sulfur snows and things like that's like quite like our stuff that we ski on, but it's got it's its own version of the Alps, so to speak. And so what we did was we used a little artistic license in order to make a little movie of what it would be like if you could go visit IO yourself. And I do want to go there now that I saw this movie I'm ready to go snowboard. So here it is. And what we did was we use the scientific data to understand the shadows and measure the distance. It may not be perfectly right but this is sort of what it would be like if you went there. We call this steeple mountain, because it's so steep there at the edge. It's literally maybe IO's version of the Matterhorn. So, I think this should be one of our ski and snowboard destinations. So, just so you get an idea how many volcanoes are going on so this these are two visible light images that have been mixed with an infrared image. And your images is an instrument called Geram which is made in Italy it was contributed by the Italian Space Agency and Juno Cam is our visible light image, and we just paste it on the hot volcanoes all of those glowing things. And so this is not just one place that has just a couple of volcanoes on it. It's all over the place and what's happening is it's so close to Jupiter it's being tortured with what's called title forces so Jupiter's gravity is pulling on it so much that the insides are literally getting squeezed and the magma is getting created and then just pops out all over the place. So this is an infrared picture this is an infrared picture that's pretty recent, and you can see this one feature here is a lava lake that's called Loki, but you can see it's covered with with lava and volcanoes going off all the time so if you were hiking around there there'd be a lot of spectacular stuff. So this is a close up of one of those lakes, also the same lake that Loki Lake right here, and it's very reflective. It's a very spectacular reflection. So the material on the top of that in order to be that reflective must be a little bit like obsidian glass which is also formed near volcanoes on the earth. I'm not saying it's obsidian, but whatever it is it's very smooth, and it's smooth to the wavelengths of light, which means it's pretty smooth. Now this is a lake basically of lava that's going around here. It's probably cooled off with a crust, and there's some edges that we can see in the infrared where it's glowing, and then this is an island in there. And while Loki Lake and Loki Crater has a name, there's no real name for that island. So the team we're just calling that at the moment, Angios Island, because it looks a little bit like an A, and also Angioletta Cordini helped build the germ instrument which is helping us discover this. So we have a little movie of that lake if you were to go by as well. And I'll play that. So here you start with the image from the top and you can see it's sort of like an A but not exactly that island and this is not, but now you can start to see the rim, just like volcanoes here on the earth. The lakes are filled with maybe colder crust, and then there's some hot lava coming out on the edges. So that's another place to go hike, I wouldn't necessarily say go skiing, but the top of that island is probably very cold, whereas the lake of lava is probably very hot, or certainly underneath it. Okay, so we also have an instrument on board our Juno that's called the microwave radiometer and it looks in microwave eyes. So we don't, we can't see ourselves that way, but it's basically a radiometer. So it's measuring heat. And this is that one of the frequencies we have six frequencies. So this is looking at sort of at the top end of IO. And if you had microwaves, this is what you would see the red means warmer. And yellow means a little bit cooler and blue means colder. And so this is the North Pole. And so what you see is his is colder at the pole and the middle around it is warm. And that's not a lot different than the earth. Of course, we have that. And it's probably partly due to the fact that the sunlight shining more on the equator area than the poles. But it may also be that there's something internal in the processes. And so we're at the beginning of understanding all of this data, but we may be able to say something about how the interior processes work by being able to study this kind of data. So just to show you a picture of all three and three different wavelengths. You have the microwave on the side. If you had microwave eyes, the visible light and then the infrared light. So these are really tools of science. And when you can look at things in different wavelengths, you can compare them and you can learn a lot, give you another example of this. Here's what it. Oh, wait, I wanted to show one last thing. This was a picture just taken a couple of days ago. We flew by IO at about a distance of maybe 10 or 15,000 kilometers away. And this picture just came down and was processed. I first saw it just last night. So I threw it in this really quick. And you, you're now looking at the south. Southern hemisphere in the South Pole in this picture, which normally we, we've never seen before. So we have infrared versions of this as well. So we're going to start to map out the volcanoes on the, on the south now. It's very exciting. But here's an example of Jupiter's atmosphere in the three same three wavelengths. So over here is the microwave eyes over here is visible and over here is infrared. Now, when you look at the poles of Jupiter, they're covered in what we call circumpolar cyclones. Nobody really knew that till Juno got up over the pole and we looked down and there were these giant cyclones polar vortices. And we first saw them by memory to the first of as we looked at many infrared and the visible and we didn't know what these were and how they were constructed. We've been monitoring them in the infrared throughout the mission and they're pretty stable and they don't change that much. But when you, and we're just getting to the point where we're over the poles close enough that the microwave can actually resolve them. And so this is one of the first images of that. And what you're seeing is deeper down with this. Here you're looking at the top of the of the reflective part of the clouds. And here you're looking at heat. Right. And so you can see these different cyclones look different. There's actually eight of them around the center one, which is right at the pole. And while these look similar, they're warmer here. And there's some that are a little bit colder. When you look over here, they look very different, even though they look a little bit similar in the infrared. When I go to look in the visible light, I can see there's differences in the polar one in particular and some of the other ones. When I go over to the microwave, now I'm looking deeper into the clouds underneath the clouds. There's almost no signature. In fact, the top one right at the pole is actually looks colder. That means that it may have more ammonia in it because we're not seeing very deep. Jupiter gets warm as we go down. The microwave can see deep, but ammonia blocks us. And so you see something cold. Here you see warm things, which means maybe there's less ammonia and I'm seeing down. And what you see is that sometimes something looking very different in the infrared or the visible. And they look very different than they do here. For instance, look at these two right here. They look very different in the microwave, but yet invisible light, they look almost identical. And the same thing over here in the infrared, they look almost identical. And yet there's something going on underneath the clouds. That's very different. This center one might be upwelling actually, you know, and the other ones may be funnel clouds going down. So I'm going to switch and I'm going to touch on a subject that's a little bit similar to what the first speaker talked about, which is the formation and evolution of Jupiter. We, that was one of our primary goals. This is an artist's sketch of looking down at the early solar system. So you have the proto, the early sun forming right here. Something happened. I ran out of battery for, I can't point, but the big white spot is sort of an early sun and then you're watching the dust and proto solar pro planetary nebula. Coming out in the first planet may be forming out there and that presumably was Jupiter. And so one of the things that we were set out to do was to understand the composition of Jupiter and whether whether there was a course that we could understand how things were formed. So we were following a mission that went in 1995 that launched literally a Galileo probe was part of the Galileo mission and it fell into the atmosphere dropped by parachute. This is a picture of the actual probe which looks like something out of a science fiction film. So I really love this. And it measured the composition. And what we found was that Jupiter is very similar to the sun, mostly hydrogen helium, but it was enriched in what cosmologists call heavy elements. Everything heavier than helium, and it had about three to four times compared to hydrogen of what the sun had. And the question was, how did that happen. And so here was the data that they got from Galileo. And so you see on the bottom our composition of some noble gases are gone crypt on xenon and then carbon nitrogen sulfur oxygen. And where the green turns to gray would be exactly the same as the sun, a ratio of one to the sun. And you can see almost all of them are about three to four, which shows that they're enriched and the question is how's that enriched. How did Jupiter get enriched it's important to us because the stuff that Jupiter's got more of than the sun is what we're made out of. So it's eyes right to us. The puzzle was the things that are in yellow. The Galileo probe measured very low oxygen abundance, which is in the form of water in Jupiter. And it was so low. It really puzzled scientists because at that moment people thought some of scientists believe that the only way you could measure was water ice must have gone in. So how could the enrichment happen in the water ice below. So it was a big puzzle. And so we showed that there were three different categories maybe that could affect different ways that you form Jupiter. And so one of our goals was to measure the water. And you can see the blue is where we measured it. And that basically shows that water in in the equatorial region of Jupiter is about the same enrichment as the other heavy elements. And so this is the real the first direct evidence of what went on with the Galileo probe. A lot of people theorized. In fact, somebody in the audience was one of those people theorizing that the reason the Galileo probe measured small amounts of water was it went into a hot region, the Sahara Desert of Jupiter, and it was just dry. And, and that was a good theory. This data shows us that the average equatorial region is actually enriched and that Galileo probe did actually go into a very rarefied region. Maybe it was unlucky or maybe we were lucky that we got to see a unique spot. This is still a puzzle because it doesn't answer exactly how Jupiter form because we also are looking at the core. And in theory, the core of heavy elements should have an enrichment that's similar to the top if it's well mixed. And it doesn't match that our gravity field data looks at the mass distribution of Jupiter, and it's implying that there's very low amounts of oxygen and heavy elements. And that's a puzzle, because it implies that Jupiter is not mixed from top to bottom. Sounds like something that could make sense, but most scientists did not believe that so Jupiter Juno as results are sort of turning a lot of these theories on their head. And we're still sort of figuring it out. And we have to mix this kind of data with the meteorite data that you heard about earlier. And maybe we'll sign and figure out how our solar system was made and how other solar systems are made that we're now discovering. So thank you. So we have now some time for question and answers just to remind everybody who is online. There are two ways that you can ask questions of our presenters. You can either raise your hand on the in the zoom room, which I will be able to see here and then call on you, or you can type your questions into the chat. And we I will ask them on the journalists behalf. If you have questions in the room, please just raise your hand and I will call on you. So I will actually start with a question that I have from online already, which there are two questions for Chris from Javier. And again, I apologize if I mispronounce your name, but from Javier Barbizano. So the question that they have is firstly, if the giant planet migration didn't cause the late heavy bombardment, what did to my understanding. I think what the majority says that they study the material from the moon and so on is like it didn't happen exactly like that. We didn't have the late heavy bombardment. So it's not that there is another process is as the general idea of the late heavy bombardment is waning as it was initially described. And the second question that they also have is how do you link the planet migration with the fear impact just by the timing. I again maybe mispronouncing fear that is T H E. It's fine. Yeah, yeah, yeah, yeah. Yes, as I showed before probably the very last slide, they were a couple of two or three works actually recent works that the dynamical dynamical studies that they showed that if we are not the giant planet stability at some time in the history of the solar system. After 10 to 30 million years, the, the giant impact can happen on Earth. So we start from a five, let's say planets in the terrestrial region. So we have proto Earth, thea and so on, and the other three. And so we have a small delay. Then we have from other independent data for the moon and the Apollo missions. I think that the formation of the moon was between like 60 and 100 or 120 million years after the formation of the solar system. So if you enacted the instability at 60 million years. So in our window, still you can have the moon formation in the same time. Even if you enact instability 100 million years with the upper limit by David and his morning and colleagues, then you still can have the younger age for the moon, which is like 120 or something like that. What it is in the literature. So we're still good. Lovely. Thank you. Any additional questions, either online or in the room. Yes, I'll bring the microphone to you. Yeah, I have a question for Scott, but first of all, I really liked that you see the skiing and hiking in those celestial objects, because sometimes I'm wondering the same about mountain biking, but it's. I usually don't share that because people always look at me like, why would you. And so it's great to find this relation. But I was wondering about all the new thermal data and the volcanic activity. How did links with the with the tin atmosphere on the moon. If the atmosphere can retain some of the, for instance, the volcanic activity. Or if it's so thin that it becomes irrelevant, and therefore it's more about. Looking directly into the spots where the volcanoes are. Well, I mean, I think from the volcanic activity, there probably is a very thin atmosphere. You know, that's very tenuous on, on IO, but it's freezing out right away. And so that's not a substantial atmosphere, but those volcanoes are all over the place and they're going off constantly, right? And we can see changes that are happening on IO and we have for many years been able to see that. So I think there is a thin atmosphere that's there. And one of the things that's happening, you know, IO is getting tortured by Jupiter, right? By getting squeezed so much. But it's getting its revenge by the fact that all those volcanoes are going off and that atmosphere is getting stripped away by the magnetosphere. So what's happening is Jupiter is filled with charged particles, right? It's magnetosphere isn't it's magnetic field is whipping around every 10 hours. So I was going around like a day and three quarters or something. So this magnetosphere overtakes it, hits it and strips away whatever happens to be tenuous, right? Whatever's coming off. And it's basically filling Jupiter's magnetosphere with sulfur ions, oxygen ions, all the different material that's coming off of IO is basically dominating Jupiter's magnetosphere. So this little tiny moon has a huge effect and you can even see light and relationships going on in Jupiter's atmosphere because IO is creating Aurora because the magnetic field has got it is like an umbilical cord tying it to the big planet. And so these particles are going back and forth. And so it's so powerful that not only is it filling Jupiter's magnetosphere with it, these things are hitting the other moons even, right? I mean, it's by far the most dominating thing in that magnetosphere, other than the fact that Jupiter's rotating around in 10 hours. I don't know if I got to all of your question on the atmosphere, but and I will add mountain biking to this because I do that too. Solar system tourism starts here. Any additional questions either in the room or online. Remember, you can raise your hand or type the question in the chat if you are online, either of those will work. A couple of checks. Nope. Okay, I think that will bring us to a close then. So all that remains to say is thank you very much to our speakers for participating in today's press conference. The press conference is has been made and will be made available on the YouTube channel within the next few hours for anyone watching who wants to review some of that amazing footage or data that was presented here today. This is the fourth press conference out of seven that we are running this week at the General Assembly. Our next press conference will be this afternoon. We have a conference at EGU-5 which is entitled Learning from the Ancients, Journeys, Giants and Calcium Buildup and that will start at 3.30 CEST this afternoon. If you need any additional assistance with your media inquiries, if you wish to speak to any of our panelists either today or any other press conference, please visit the EGU's media.egu.eu website where you'll be able to find contact information and resources to help you. All that remains to say is to ask everybody in the room to join me in thanking our panelists for their excellent presentations. Thank you very much.