Presentation slides: https://doi.org/10.5281/zenodo.8400348
Delivered as part of the 6th IAGA School (2023) hosted at Niemegk Geomagnetic Observatory of the GFZ, German Research Centre of Geosciences near Potsdam and Berlin, Germany.
For more information, see https://iaga-aiga.org/iagaschool/
Later than have only one okay but we’ll start today with J Johnson and he from the University of university department of engineering right and will I tell a little more about your and yeah this is first session in the morning and the break will be on your
Whenever in and yeah many things that you to be part of the summer school and really appreciate yeah Johnson I’ll SP physics how many of you are in the field of space and the rest of you you all know what a magnetosphere is okay when when we think about M Spirit
Physics what’s the first thing that comes to your mind what else your space weather space weather Aur what else plas how manyas all of you all right so yeah storms sub storms things like that the sun all right well let me just tell you a bit about myself and I think as advice
For you just entering into the field when you get to your later career the thing that you’re most going to be proud of is the people work so you know that’s really you know something to think about the collaborations that you forge even now maybe people need the
School someday are going to be colleagues that you consider friends that’s probably the the need part of being part of science is you know it’s great to do the science but people really make an important contribution to your career so my career started as an undergraduate at the University of Colorado working
For Marty Goldman and I went into his office and he was working on some sort of solar problem he was looking at some sort of distribution of Energy and he asked me to solve a dispersion relation and uh so I did work that I did as an undergraduate um I subsequently went from the University of Colorado to MIT where I worked for ching and he was one of the most theoretical people I’ve ever met in the field of space
Physics uh in fact he wrote a paper using a path interval formulation of ion Heating in the so anyway he he taught me to really appreciate Theory and did some really NE work with him uh on mode conversion looking at waves that will convert into other waves um in the
Aural region and we were looking at wavs that would propagate down the magn field line generated in Equatorial region and then they would heat ions and the ions would come up fields and space tornado so that was that was fun and and from there I went to the University of
Alaska where I did a post off Alaska is a great place to do a post off because you get to see the aurora and I remember Tom Chang always used to post that he had never seen the Aurora being a theorist but when I went to Alaska I
Actually saw the Aurora there you can see it the at least maybe one out of nights or so it’s really impressive from there I went back to MIT worked uh a little bit on uh some sort of nonar type of structures glora and then I one day uh Frank Chang from CL Physics
Laboratory came to work with us at MIT and uh he sat down with me and we were having discussions and the next thing I know he offered me a job at Princeton so I went there uh and uh as a post do we work together on uh transport at theuse
Uh ion cyclon waves and and basically all sorts of kinetic modeling of wavs um and he he is also theorist in the so anyway uh while I was there you know eventually I he was the head of space just starting up the space physic program there at Pon plasma Physics
Laboratory and 10 years later I took over as the head there I had a series of post talks un Kim who later became now she’s principal research staff there at prinston um Peter Damiano U so un un and I have worked on developing a global model for Electro electromagnetic cyron waves actually all
Waves with finite element code and so this is actually revolutionary way of modeling waves in the mosphere that takes into account all sorts of mode conversion um and actually a global model and goes Way Beyond approaches that have traditionally used rate tracing Peter domiano was another postop
Working for me he’s now a professor at the University of Alaska and he developed a code to model electron acceleration in the aural region so we modeled wave uh particle interactions that actually produce the Aurora and that’s actually pretty cool thing and then Peter perazic worked for
Me developing a gyro kinetic model for the magnosphere and then later we modeled radiation belt electrons and how many of you are familiar with something called The Lost cone few people know about the Lost cone so if you look at distribution of particle energy there’s some particular
Angle at which the particles will go into theere particles are not stop hon well we were we were working on designing an experiment uh and that experiment was to shoot a relativistic Electron Beam into the oser which what we found is that if you if you shoot the Electron Beam into the
Traditional L cone the the electrons will actually bounce back they won’t actually get into the so that the project would not be able to function where the experiment would not be a to function what we found is that the Lo actually shifts so you have to actually the electron be at a different
Angle in order to get those electrons to get into the that the project the mission could be possible um he’s currently a research physicist at Lawrence laat the great people that work for me my key I worked with far who is now the Ambassador uh from Iran or Iraq to he was Ambassador France he was a post stent of all the uh collaborators that I’ve had being a theorist so I would urge every one of you if you want to go into Theory make sure that your best collaborator is an observer or if you’re an
Observer make sure that your best collaborator is a theist Forge those Forge those bonds that it’ll just make your work so much more meaningful U and yeah so Simon Wing at John hin Applied Physics laboratory is one of my best collab cators we had had my most Publications with him
And I would say my my work has become much better through my interaction with with him as an observer because I can do all sorts of theoretical modeling but it doesn’t mean a whole lot if it’s not connected to observations and similarly you know as an observer um you know supervisor
Taught him sort of like just phenomenology just so he was he was looking at dmsp which is a low orbiting satellite from military that hours or so and based on that they would measure precipitation patterns in the osphere and what they would do is they would just identify well there’s this type of
Precipitation that type of precipitation and so forth it just descriptive type of thing once he started working with me um you know we began to think well what is what is causing this what is causing that and um you know I think both of us found those types of discussions to be really
Useful markit and another Observer who helpful in showing you know this is the type of wave that we’re seeing why why is it important um and you know this is a wide list of people who I’ve worked with Through The Years um hopefully at the end of your
Three will’ll be able to put up a nice portfolio like this and say this is what I learned from this person that person that person that’s what we worked on um even solar projects a couple people ion projects other soles a lot of wave bobblers in here and even a collaborator in
Neuroscience all right well let’s get to space physics so the context of space physics is the heliosphere the heliosphere is just the region surrounding the sun basically the region that’s sort of carved out in the intercell medium uh and The Helio CLA but we’re concerned about everything that’s inside of this
Heliosphere and if we’re thinking about the magnetosphere or that sits within there so let’s just review what’s going on so the sun is responsible for the given a spere the given a spere is caused by a wind that blows from the Sun sound very hot um if we look at the sun itself
There’s a region inside the Sun where fusion occurs and there’s a radiation dominated transport photons take a long to get out of sun we see from the Sun actually long the uh outer core is radiation dominated transport and then have convection so convection heat up material and the material Rises when it gets
Hot density just like cooking and so this convection is very interesting that there’s some sort of a magnetic field that’s inside of this contion Zone generated by a Dynamo other dyn in the CER of the Earth this Dynamo on the outer shell of the Sun and this convection will drag the field
Inside of there is what we call a low B beta plasma infection is going to drag the field wherever it wants and so if youve actually drag the field up to the surface it’ll emerge and then that’s where you’ve probably seen you see these arcades when the flux
Is brought to the surface it produces these AR usually bipolar coming out see the types of abruptions that you getal Mass injection material just exploding off of the surface of the Sun processes these these movies are incredible see now wavelengths presume mag fi structures that you see only the
Surface but I you can see how sun is anyway the origin of space weather is basically coming from the all right so that’s activity of the sun call that Sol activity if we look at the so Yoko looked at Sun wav the course of a solar cycle
And this is supered image of what how the Sun evolves during the of a solar cycle and so you can see what call an active sun and then here the sun is not very active and bective again an 11e solar cycle that was is well known where you have a
Change in activity from being very active not and this has been seen a long time people sunspots in iniquity me once they look at sunspots sunset with their naked eye don’t know good idea they said they could see so I don’t know how the original observers were observing the sunspots if
They were looking at them late in the day with their naked eye maybe smart they projected them oner anyway it’s been known for a long time that that there’s a some sort of an activity cycle from the Sun that’s about 11 years long and the origin of this solar cycle is
A a dyn process and probably somewhat different than the D process so um the D the solar cycle is thought to result from the soal Omega effect and Alpha effect so the primary driver of the solar Dynamo is the rotation of the Sun so um let’s say you start out with a
Pidal field that just means that it looks like a dipole field and the sun is actually rotating but there’s differential rotation so that’s arrows different length so that the equator is actually moving faster rotating faster than that higher latitude so what that does is it takes the field that’s internal to the
Convection Zone and it starts to rotated around um in the tal dire that’s just going around so we start with the pidal field the rotation of the sun because it’s differential it begins to wrap up the field in this helical type of form and so when the field field starts getting
Dragged at the equator around and wrapped up what that does is it actually intensifies the field because now you have stronger field and that’s after a while what happens is so you get this transformation from from a sort of like a diapo field to this field inside it’s all wrapped
Up and then the socalled alpha effect or that fism strikes in and what’s happens is that this field uh material is heated and begins to rise as it rises up uh the flux will emerge from the surface but it gets twisted and the reason it gets twisted is because the coris force twist
It rises up and then twists what that twist does is it restores again the poid or dipolar like compl so the field begins to look more diol again and until it it’s it’s back to the original state so during this period here that’s where you see a lot of flux emergence and
That’s the solar maximum so that’s sort of the fundamental solar cycle is this Omega that’s usoc velocity of the Sun and then the alpha effects this Rising of the these Bubbles and twisting to restore the component of the field sort of all right this is a cool paper I I saw
I just want to show it so so these guys were looking at the Stellar cycles for solar light so they’re basically taking the Sun and they’re saying well let’s just change the rotation perioded time scale yeah so this so the parameter that’s important here is the rotation So the faster the star
Rotates you can see that the pattern of the Velocity on the surface changes so this is called meridianal flows that’s sort of surface High latitude theal dra down upes returns back the surface so this this is the flow back toward the pools and so you get these
Interesting patterns like this the sun I think is probably somewhat like this so you have this midal flow and then maybe a higher latitude you have so anyway the flows that this like this are important solar cycle and what happens is that initial right after solar solar maximum flows here are
Actually eming and then later on they here and you have sort of shift from higher latitude and that is what you see you probably have seen the butterfly how many you seen the butterfly okay so again this is the sun here we have sort of little activity so that would be
Solar minimum and over here you have solar maximum like that so see the lots of it’s it’s sort of interesting these spots only appear in a certain band and around 30° and they shift down toward the equator um they sort of annihilate the center get and that’s
What you see here if you look at a function of time you can see well so the pole the PO sort of tells you the poity of the of the Sun time so you can see the polarity is reversing every 11 years and then you see these sunspots
Appearing they appear first at about 30° and then they shift down the and then see thatting again stting you can see theity is flipping recy and if you were to count number of sunspots the Sunspot number has been done since the 1600s so that’s when people were first looking at
These things you actually see this solar cycle variation and there is a big U minimum yeah yeah there is a big big minimum yeah so even at the time when people rep reporting these sunspots there was this uh minimum around in the 1600s when you basically didn’t see any activity there no
Aurora called a little ice so you can actually extend this back by looking at Carbon 14 or 10 going back with ice and you can see that that these things sort of track very well with the solar cycle that we’ve seen and so backward in time what the solar cycle
Look like you can see another another minimum here the spor minimum the M minimum the W minimum the medieval maximum and so forth and these are yeah so this is called a grand minimum the have people wonder whether even today we’re coming to some sort of a minimum beening the last
Couple that’ll put us out of not exced all right so anyway so you another thing you can see is the polarity here is on top yellow on the bottom but then flips on the bottom that is a result of interesting uh if you look at bral paintings back in 1560 right here
Minimum there’s a lot of ice in the Netherlands probably not so much ice now um and during the little ice age was very cold so you have a lot of pinkings that have cold temperature all right so what does this have to do with the Earth so the
Sun uh is basically blowing uh material out so it’s very hot you can see that there’s explosive activity material comes out away from the Sun and uh Eugene Parker derived a model for the solar wind and this is what it looks like so see that there’s a spiral structure
To it coming out and this is called the par spiral it’s like a sprink going around shooting out water as sprink rotates the pattern that comes down as like Spiral another thing that you would expect to see is warping of like current sheet get any typ of offet being purely aligned
Plane that and so these are actually really important things because the magnetic field of the Sun as it comes out basically have some sort of So eventually wherever the Sun comes out B coming field coming that and so when Sol wind gets to Earth you would expect that it’s mostly going
To be directed in the ecliptic plane but it’s these little undulations ripples inad totic field being northward or compared Earth’s magnetic field and so these these ulations uh are are very important for driving the Dynamics of the osphere because northward and South when the field is align with
An all right there’s a lot of variation in the solar wind during the solar cycle so here’s the Sunspot number that we looked at earlier this is few Cycles ago um but you see at solar minimum that you have a lot of veloc so this is from ues U an orbit that’s out
Of the plane and so ues can actually measure uh the velocity of high latitude so you can see that there’s really high speeds velocity coming out at high latitude when you have solar minimum but when you have solar maximum you can see that the velocity is much much different you you
Have sort of you can see it’s it’s not well structured it’s very sporadic and it’s basically all latitudes um and then you see a return back to this velocity so you can see that the velocity of the solar wind varies during the solar cycle quite a bit and that can also effective geec
Response oh all right so this this is also a interesting the concept of the magnetic carpet so this is actually high resolution simulation of the solar surface so you can see all the flux emerging from the solar surface it almost looks like that picture I showed you initially right this this is
Actually R high power computer so you can see what the the field L that all tangled up this really turbulent now barasi did a study of the mag field near the Earth and found that all this mixed up spaghetti makes its way so you may think if you saw the
Parker model of the solar wind that the solar wind is just this nice lamin or thing that comes past the the Earth but in fact what the field coming past the earth looks like is just a bunch of spaghetti that’s sort of mixed up and if
You look at it head on this is what the solar wind looks like it’s just all these sectors of and in these sectors the magnetic field is in different direction um and so when we encounter one of these we encounter some type of magnetic field direction for a period of
Time but these things only um May persist uh in EN counting Earth for maybe three hours or one to three hours and so that’s you get a lot of variable conditions in the driving of Theos because of this sort of like spaghetti like nature of the solar wind
Um and this is actually very interesting question people have is is this spaghetti determined by what’s at the surface of the St is it evolv and sus out and that’s still something area active all right so we finally get the magnosphere so the sun solar wind all this mixed up spaghetti
Field um encounters the planets and at Earth venu is very particular but all the planets that have here planets like Mars and Venus field um these other planets have very interesting interaction with the solar wind much different how big do you think the manosphere of Jupiter would be if you
Looked at it you see it yeah we looked up in the sky and sometimes you can see you can see it magn how four moons that’s about one it’s about the right so yeah it’s an enormous thing I me but yeah so the rest of this taking a look
At but uh just to emphasize the study of the med is very interesting it’s coupled to the sun it’s coupled also to the ionosphere and so it’s really a very complex system and so this is just shows some things that are going on in the ionosphere I noticed there was no
One section two or section so bring in a little bit of that so here you can see feel the line CS that’s one of the primary W of the magnosphere communicates with the ionosphere field currence the ionosphere is a source of plasma for the mosphere so you get all sorts of processes happen
Sort of at high latitude that heat up the ionosphere and cause keep theere ande theere magne field is weaker andic that motion as a consequence of conservation of energy something magnetic M and sort of heting process down Theos basus to Mo up into and so Theos significant source of plasma in the manosphere
Um we have storms you also can drive fields in the atmosphere all SS of things neut winds gravity waves the iosaur is really important yes I you want to know SC oh we don’t have a scale yeah so the ion itself is so you have different different layers in theph and Beyond
So the densities drop off exponentially in a gravitational all right so anyway ion is a complex all sorts of cool processings going down there and the H is really important for our lives because we all now rely on our cell phone communication there’s a lot of communication satellites up there and
When they’re sending signals down uh there can be and get phas delay any some really regions caused byess all right someone asked about the importance of field so sometimes you hear people say that it’s really important to retain the atmosphere and so one thing it does is the magn field Shields Cosmic r
Really glei May emitted by the Sun or it can come from Source but when they encounter the Earth’s magnetic field they get trapped and they shielded so the mag field will actually deflect them impact the Earth cosmic rays of course if they were to impact the Earth can lead to radiation
Mutations can also affect climate Deb about that cos seed clouds and things like that um the magnetic field also helps to retain the atmosphere so here are some simulations that were recent paper the last couple years of I think these are bars it looks at the loss
Of loss rate of oxygen so you can see that L rate is if you convert these units to per year it’s about 10 to 30 34 particles per second we have the atmospher particle of then 43rd the atmosphere can be lost time scales Venus and Mars have no Feld the
Field prevents ions that flow out from our planet from actually escaping retains the atmosphere all right people mentioned about Aurora that’s what we know so that’s probably one of the first things that people noticed about uh the first thing people really saw about space weather is Aurora and probably
This pretty significant space weather because people lived at low latitude um and so saw Aurora at low attitude it was a big deal um and so it’s something that you might only see in your lifetime years something like that and so people would say there was an aurora
Back when Julius Caesar died there was an aurora when Julius Caesar died and they would probably tell all the people and then until of the Hun came to attack the Roman Empire and there was another Aurora that happened at that time as well so people would associate it with bad
Things there was a a story about two armies that were having they were going to have a battle the next day that night there was an aurora that they interpreted being some sign that they made peace um yeah there were various interpretations of what a was but you
Know this is what they might VI be um the expeditions to the pools people would see the aurora so a lot of the exploration that took place going to the Northwest Passage into Antarctica some of the first real interesting understanding some pictures I a place here’s the Aurora from the image
Satellite so see that the Aurora tends to be onal it’s at the open CL looks like from space can see it’s very active all right how does space further affect our lives so yeah so protons from Sol flares more important energetic electrons storms electrons are injected into the
In manosphere they get up to energies and when they strike satellites they damage the components this can be very expensive a lot of money to the place the airplanes actually will rout when AAR studes induced curring on induc and D power here but yeah unication probably one of the most
Vital things have now disrupted by car to class C presented by science in mid ail scientists government officials and others converged on Colorado for no as space weather Workshop an annual Gathering to discuss the perils and probabilities of solar storms the current solar cycle is weaker than usual so you might expect a
Correspondingly lowkey meeting on the contrary the halls and meeting rooms were a with excitement about an intense solar stor that narly missed first the close shave happened almost two years ago on July 23rd 2012 a plasma cloud or CM rocketed away from the Sun as fast as
3,000 km second more than four times faster than a typical eruption the storm tore through for but fortunately Earth wasn’t there it did however hit the stereo made spacecraft researchers have been analyzing the data ever since and they have concluded that the storm was one of the strongest in recorded history
If it had hit Earth we would still be picking up the pieces says Daniel Baker of the University of Colorado who presented a talk entitled the major solar eruptive event in July 2012 defining extreme space weather scenarios this the event of September 1859 was a Ser of powerful CM that Earth head on
Sparking Northern Lights as far south asah intense geomagnetic storms caus Global Telegraph lines to spark setting fire to some Telegraph offices and disabling the Victorian INRI a similar storm today could have a catastrophic effect on Modern power grids and telecommunication networks according to a study by the National Academy of Sciences the total
Economic impact could exceed $2 trillion or 20 times greater than the cost of a hurricane like Katrina multi-ton Transformers by such a storm could take years to repair and impact National Security a recent paper in nature Communications aued by UC Berkeley space physicist jenet G and former
Post. describes what gave the July 2012 storm Harington like pocy for one thing the C was actually two c separated by only 10 to 15 minutes this double storm cloud traveled through a region of space that had been clear C only days earlier as a result the CN
Would not be cated as much as usual by their Transit through the IM medium had the eruption occurred just one week earlier the BL site would have been facing Earth rather than off to the side so it was a relatively narrow Escape when the cartin event developed Earth in the 19th Century Technologies
Of the day were part sensitive to electromagnetic disturbances modern society on the other hand is deeply depend some sensitive Technologies such as GPS satellite Communications and the internet the effect of such a storm on our modern Technologies would be tremendous as during informal discussions at the workshop mat go Swami of the Godard
Space FL Center noted that without n stereo we might never have known the severity of the 2012 superstorm this shows the value of having space weather buies located all around the Sun it also highlights the potency of the Sun during socaled quiet times many observers have noted that the
Current solar cycle is weak perhaps the weakest in 100 years clearly even a weak solar cycle can produce a very strong storm say Faker we need to be prepared for more information about storms on Earth and Among the Stars stay tuned to science.nasa.gov yes so the uh space space at that time
On the other side of the Sun so they can actually detect this indeed one week earlier right prob uh between the 23rd of October and the 6th of December 2003 there was a series of storms called the Halloween storms this actually picture of the Halloween storms so um 47 satellites reported malfunctions uh
At that timeing another satellite cost 640 million with a total loss more than 10 satellites were out of action for more than a day it’s going be very expensive B so in 2021 there 550 satellites init each one of them is very expensive to put up a lot of them are at geosynchronous
Orbits these are good weather the same place sensing forward orbit that’s yeah this is just new febrary 2022 40 Starling so Elon must put up and 40 40 I think there were 49 almost all of them were knocked out by a GE storm and thison in that case it was not from
Electrons but it was the got heated up and raised up high enough that drag on satellites and so the radiation belts were discovered by Van Allen he set up saite saite went I guess this prob the original drawing and what they found was there’s actually two regions two
Regions where you have radiation belt particle the in radiation belt radiation belt mostly it’s populated by cosmic rays they stay there a long time so that radiation Bel is basically persist all the time the lifetime of the particles there is extremely long and then you have the outer radiation which consists
Of particles that are injected in Thea particles go in and get trapped there those particles then are unstable and waves which some of those ELR upes place toelles we take a break and then we will take a look at the morphology of the manosphere and the Dynamics dynal process so we can just
Take the stor is it’s a motor stor 71 or something but it is a kind of double Stone dip and after after some time again so a double yeah like the3 Halloween Stone yeah so I feel like it will have a big impact on the thermosphere yeah for Well yeah so I think right so it’s actually because otherwise ex like w Think so I think probably the first place fine for The time show you that he’s very good man verying speak very slowly very good that by it’s very stud that using different Satellites every Yeah The caring the did you that car9 there was Big St at that time there is no technology here there Telegraph L and the caring the scientist who observe the sun there is something different happening and what is consen that after that storm all yeah it’s at that time it’s only that if
It happens like such a kind of storm now it cost of dollars we lost many things in 1989 she saw the picture of the Transformer B it’s a transformer in and all Transformer B no power 9 hours it’s kind of a big deal I think now you Right Spe GR All right let’s take a look at what makes up a MAG here all right so look at the magnetic field current systems associated with the magne field plasma populations so this is a schematic of a mosphere so wind coming in from the left arms out a hug cavity in the solar wind it’s
Very continuous here solar wind about five okay how one yeah it’s very there’s hard is populated by particles but there’s hardly any parles and actually the solar wind is much has many more par so actually not are actually getting into the mag from the solar wind closer 10 in fact the cross-section for
Particle entry into the magnosphere ISR small all right let’s take a look at some of these currents so we have boundary currents at the boundary we have the ring current tail current Brooklyn into the out and I all right so some simple enm if we want to consider the what happens to the dipole when we have a
Solar wind uh the simplest model is to just say well we have some sort of a super conducting boundary here that doesn’t allow the to penetrate over to the right and so yeah what what would be how would we solve a problem like this you’re taking DM
Class solve a problem this by put di here felds and what it will do is it will make it field the mag field has no normal component at boundary and then there’s a current flowing on that boundary and you you actually get some features that are very similar to the boundary
Of sun boundary of the you have sort of a compression of the dipole the DI it’s all its fluxes forced to be on this side of the boundary so you get this impression you get a neutral point up here this is where the cusp comes from fi has some of
Cusp some type of open field L here and so that’s Cho simple mod you consider a just compress a DI in a spherical Med spere we just take a a sphere and we require that the field be contained in that sphere again we look for a solution we can use
A scal potential for the and at surface require that the normal component of f be zero and that gives us SC this what we find is that at the boundary we get about three times the field strength so the actual compression somewhere between two and three here this is if you put a
Parabola you can solve zer on this boundary and that will give you see the compressed magnetic dipole on the right hand side of the boundary through the boundary mags these are your currents so you get a current that’s flowing around like this and on the
Other side and we have the set up so we can actually rotate the magne field dle in any orientation you want the other and in addition we can put a solar wind magne field on the other side and then the difference in the fields that sort of Windfield will break across
The boundary the difference in the fields on the two sides everywhere on the boundary anyway this is what the Chapman fer print system looks like at the boundary so this is what what you would expect to see all right do this system uh F build that all right so discussion storms
And the compression of the of the Magneto boundary that will strengthen this okay in the in we want want region so there are three adiabatic partic motion so oscillatory motion if you change the parameter field slowly in time or in space this mag first that’s temperature F so if you slowly
The then you have a balance motion balancing as well and then you have a drift motion so the drift motion um yeah the in the West in the west west if you think about Earth it is going in the West okay V cross v b yeah go B then um then left left
Okay I got this right okay yeah that’s right okay so that’s right so now the the important thing is if we have a strong mag field a weaker field field this is called gyro all right so the gyro radius gets bigger or smaller as it’s it’s that’s not when it get weaker
The gyo radius would increase so right so the orbitar parle is large so the particle Orit there’s aadi mag you go toward the and so that leads the ions they’re going to go around the ions are going to go Sun that way the this and the electrons will go in the opposite direction
Resp so this would be like going going toward the Earth this it’s drifting like that This then field is actually and that’s exactly the ions go one way the electrons go the other way okay so this is the origin of the Ring print and the energy can written as a function of balance VAR okay so um you basically get some current that
Results from this radi of the magne field and if you calculate you know so the velocity is actually going to be proportional to the temperature the hotter theot isft parles to DFT more than parle but you can actually estimate that the magnetic field so once you find
The current you can estimate what change of magnetic field you’ll see at Earth for a given energy uh andle magne field and Delta is 100 Tesla energ particles 100 PR big storm but yeah that’s about 10 15 that’s that’s a pretty big how much energy
100 so every time we have a storm it’s like 100 ear pretty Prett all right okay there’s a cross tail okay so the M field gets stretched out and you basically get to what are called the Lo is up here and down here loes are basically empty of plasma then you get
The CR sheet here where plasma gets compressed in cringy and the F gets stretched and so when we stretch the F something that if you have a field that’s like this what do you need right in here whatever all right so there’s all right so you have a cross tail brch
So down the tail close so there about 10 that’s quite okay and so we talked about a ring current here and then we talked about a tail current out here and there’s actually some sort of a disconn r that really nice paper what they did is they took s ankle mod for
The flux surface and then solve for the equilibrium that you have with the stretch cable configuration but what you have is a CR scale here and it actually closes into the is so this here so you the whenever you take the magnetosphere and deform it deforming it
Will require there to be some sort ofine and that is the electron precipitation see a lot of currents from low satellites and that can lead to Aurora in the upper curent if you don’t have enough current carriers provide currere they’ll be accelerating potentials which will energize electrons that they
Can all right another important concept is mospheric conection so what I showed so far is a bunch of magnetic field and current structures but in fact there’s an interaction with the solar wind and that’s driving something like Dynamic so this is show so inter so when the interplanetary magneet
Field get Southward it’s opposing the mag he of Feld like this have Al this and when the interact what happens here reconnection happens and reconnection happens geologic change and eventually add and if this happen over and over bring more and more strong pressure so what happens here another reconnection this reconnection notas
Not so easy there so you can build up flux here until so this reconnection can take place sort of in a steady way but this reconnection take place in a steady unsteady build up because stabil has to build up pressure here that have come around the third dimension back here to
Replace the flux and that collap to the point it so we’ll look at that looking at simulation but in the meantime if we look at this convection process how do we know that this is not just Dre there are these Radars that superon radaro a whole bunch of super Radars all over
Place and they Measure the velocity of plasma inere and from the velocity of the plasma you can some paroc the electric field so these are con of potential associated with the electric field and lines here would correspond to the velocity so this is a velocity coming from noon to the night side and that
Corresponds to a field line that is moving across the pole from the day side to the night side from basically what you’re seeing here that so have a velocity that’s pattern so at no the FES move across the poap and then they move back to theas this comp cell that’s something like
This that but up here you have other see there a big difference of what’s going on with North or so from The Polar cap measurements you can find the potential drop across the C typically it’s about 50 Earth field and if that potential maps to the
Tail uh that will give you a cross tail potential drop of about 640 KS um actually if we look at this cross potential look at if we just consider what the solar wind velocity velocity so you just take the solar wind velocity M field of the solar wind that’s and bar of the
Tail should be about 640 K so potential drop in the solar wind across the mag about 640 K uh but in the bullet it’s only 50 KS that tells us 1% of the solar wind flux reconnects from sou and with North IMF it’s a much
Smaller and only about 1% of so 10% of the mag field the solar wind is actually connecting with the Earth peeling It Off yeah so that that’s a fairly significant thing reconnection dominates sou conditions for North IMF it’s not so clear that that’s a dominant mechanism it’s not clear that this isn’t just
Some this up here may all right man plasma pop already mentioned some of these uh so we have a plasma sheet have a l it’s hardly populated we have a manle that’s basically plasma come in like that you have a boundary layer latitude boundary layer there then have if you
Look down from the top this is from the side top we have a plasma sheet and in here we have some reason called the plasma steer so let’s try to make sense of some of these objects okay so to understand the plasmasphere theere so that’s this object here these
Are C particles they actually sort of co- rotate with the Earth has sort of a weird shapes it all right so if the Earth is a a conductor rotating through its own magnetic field the lent force acting on the particles the Earth will give you some sort of charge that char
Surface this creates a quar electric field in space that will then cause a force on the plasma to try to co rotate with the field as the Earth with a magnetic field in it it starts to rotate that rotation will cause the plasma to try to co rotate with the magnetic field
And so we can so we can find electric field velocity we put B in’ll find that the electric field was like one square of the distance and we can write in terms of potential that goes like one bar so particles are in and thatal is given by this here and
So the manosphere itself is driven by this convection as and then we have this coration contribution and then this this contribution here is from the particle drift that I mentioned earlier okay so this basically accounts for that coration so that’s the magnetic field kindy to T the particles around
With it that’s this term this is the convection electric field that’s this conection driven by the Elric field that actually penetrates into and this is the curvature okay so we write it in terms of a potential so the total drift of the particles will just be e cross
B and so you the potential lines that give us the stream lines and so this is the origin of the plasmasphere and if we just talk about F particles we can drop this term here we can look at these two terms when they balance that gives us this boundary right
Here dependence here that us the Symmetry okay so particles C particles would come in and drift around this way they going to they going when they’re far out here the one small and so the conric felds in turns them around like this and then particles inside here are trapped so they can’t get
Out that’s the plasma population the populations that’s trapped inside so these the if we’re at a position fig than r z those particles are ConEd if it’s smaller than that Rus they’re tra and even estimate the size of this this plasmasphere you see when is the plas what will cause the plasmasphere
You want to shrink so we can’t actually okay so we control e so the stronger the stronger you drive stronger you drive smaller that will be so what happens is that this reg will shrink when you have strong con and it will be populated by these particles that are
Coming through and then if you suddenly have a reduction it will expandly and then it will TR par so there other things that can happen but that’s that’s a primary parameter e yeah so you you if you have a sudden onset of convection it will DET trap
The because all the particles that were trapped now become untrapped because the boundary and what will happen to them is that they will actually Mo slide actually shows that yeah so here’s the plasma sphere so this is meas satellite so this is the image you get
And so you can see this is this is what you expect from the M right that you shrink here’s your plasmasphere and shrink that region like I show and everything out here that remained outside is now free to move to the so that’s actually pretty cool you can see the
Plume so that that’s actually all right what about the hot particles so now we have something called he and you have hot and particles positive and negative hot particles and so now that’s this term here that’s sit down and derve this particle orits that I show you are Orting
In this is the potential of those particles that describ drift in terms of effective potential the particles are actually jumping from one field line to another and yeah so that that is that is correct so you have the and you have particles are undergoing orbit out here they’re moving from yeah they’re
Moving from the sidef yeah so normally one of the great things about magn Fields is that it confusion particles and so yeah normally Orit like this around the field and it’s stable it doesn’t move this it can move along the field really well but when you put in this
Radi drifts are also a problem in device device counter D drifts one way and bring the field up top it’s like turning okay clear all right so anyway we have this effective potential here and so we again are driving particles toward the Earth but now they’re really hot this is going to
Divert so we go back here and the ions are coming in but their orbits are going to be diverted around the ions come in by this Cur C they’re trapped okay and the negative particles all right so now we have the idea that we have H particles we can
See and we can we can estimate the size of that region too and again you can see that these These are the ring so the ring current is actually carried by theide so if we want to increase the ring current we increase convection that increases r0 and so that
Will push the particles closer in and then we decrease R e0 and that will expand partic inside and so then you can see how it’s done the in this convection Feld is all right and you can see that the edge actually has any symmetry between ions okay this is observed as well
So this is a satellite uh gas from emsp so emsp is a low satellite it’s coming passing from low latitude to high latitude pass lude to high latitude looking at fuz the on the bottom the energy is inverted here so what you see is that you see the cold particles first
And then you see the hotter particles colder particles for and that’s so the so these particles have been injected here and now they’re coming around so let’s take a look at the trapping also depends on the temperature so U temperature so the hotter particles have a larger boundary and the older partic
Have a smaller so this boundary is fuzzy it’s not a hard boundary it depends on the energy of the particles so in fact the less energetic they are the closer they get to the Earth and more energetic they are that’s because the curvature gradient is proportional to the energy greater the energy bigger
The and so the hot ions really ions will come in and they’ll be diverted here where folder particles will get in there first closer and that’s precisely what you’re seeing as the satellite goes up here first it sees the near particles and then get out here it sees the
Further so first it sees the cold par colder and then it gets hotter CER so this this population is observed as well and this is the origin of the Ring C and how it can get pumped up during a storm to en all right we
11 so now this is the part of the lecture that discussion that you find that whatever I describing already description so there there are the most interesting events actually particularly like the steady convection but the the things that we did discuss give a framework for just understanding the
Different andr system and so they’re very important foundational things but let’s take a look at coupling this with and so there are three processes that are particularly important in coupling between the solar wind and the magnetosphere the first I mentioned already is reconnection so in this case solar wind punctures the magnetosphere and
Mention crosssection Australia like that where the solar wind can enter in felvin Holts here’s a nice example of that so you have a wind solar wind is coming this way and this is the bow shock and this is called the magnito sheep the shock wind and then this is
Mago and the magnito boundary goes on stable hel bolt stability and what can happen in these War diseases you can get mixing of and you actually get transport of momentum around here so that’s one way to drive the circulation patterns in tail is also interaction AC here addition
That and then solar wind compressions so the solar wind can compress the mag through which will increase the meduse currents create injections and it will also generating a lot of waves so just waves rapid so those are three important processes so let’s take a look at simulation
Here and the first question will be what do you see in this so why don’t we just play this and you guys can discuss among yourselves what are you seeing in here so let me just describe this is showing the density on the left and on the right shows field lineur into the
So Direction at when it’s zero again discuss among yourselves what you 360 that just I’ll play it one more starts out north all right what do you guys see um let’s just started out with northward and stop it you recognize any of the things that we’ve talked about yes the convection
Pattern in the fs there are okay so you’re seeing the convection pattern in the when it is northward it is like very complex uhhuh and when it’s Southward it’s much simp developed all right that’s a good observation so you can see this is North it’s complex you
Got two cells here yes two cells here and we move that to sou contrast that simpler not as complicated this this okay what else do you see North what else you or any other things that you see that we were talking about all right all right uh
So I think you’re you’re you’re right at the end saying yeah so so those are called flow channels so right you’re talking about stuff like this yeah so those are flow channels so it’s not it’s not steady conention at all so I talked about a dawn electric F
And a general convection for the Earth but that’s not what you’re seeing right statistically there is motion from the tail right so statistically there is in fact this convection from the tail toward the in spere but it’s not happening in any type of steady process right it’s very these some these were
Discovered I think by Angelus and they called B blows they were discovered observationally first so when I first came into the field they would run these mhd simulations and no one ever saw in fact they no one believed I remember no one believed in kelvin HS so
All the global mhd moders they didn’t believe inin they never saw kin and now we see them right the the first B clows they never appeared in the simulations why do you think yeah resolution resolution has increased rtic res so they have much much better resolution there diffusion so the
Numerical diffusion prevented the kin homeability simulations so you you never saw this in fact I could play a simulation like this from 10 years ago and and it looks very different from how how it looks now uh so what’s some other things we see so this looks like a
Pressure here this is looking from this so that’s Z so this is looking from the side you see your inrent okay yeah maybe I think they probably have some but this they have to couple this to another model for the r simulation doesn’t describe okay what else do you see here so you
See Kelvin helts so you see these Kelvin helts here um even at this you may see some movement okay there’s South IMF and suddenly now you have really active channels coming in s IMF has much stronger convection in the tail now you can start to see usually there’s some sort of
Localized connection that occurs in the tail and then you get a slot very interesting all those B CL so yeah howf is really characterized by uh these flows coming in from the tail the inter so it doesn’t happen as like a steady process that it happens through these channels
Coming look over here at the field sometimes we’ve seen pictures of region one and region system here that looks really nice and I think we actually did have a something like that ear Sim this looks a lcer but during during the we saw with the impulsive injections all right so we can
See a huge a huge difference so for South AR the transport is dominated by inter periods of fast and these are bur cloes and Global reconfiguration occurs probably periodically driven by Ste so the substorm so aasu used to go out at night and look up and he would draw the subst
So this is the first paper of subst describing um some sort of process in time and it looks like right here you have sort of a big motion forward and that’s what you call the onset of the substorm and then expand forward what does that me or something
Expand this is Bas looking into the and we see something expanding thing so the the or the where you see the Aur is really television scen telling you about what’s going on in the rest of the so let’s take a look at some real observations of course so this
Is this is a substorm that’s observed over North America so feus is a mission that was put out to actually look at sub storms and even if let’s hope the next so these are ground based magnetometers they’re reconstructing it from a whole bunch of them so you’ll see forward motion
Any that’s what sub looks like from the ground cover the entire North America so here’s a view from space so here you can see definitely an so substorms occur about every about every hours statistically but it is in towards the day side if you you play again yeah it’s like sure usually onset
Is oh all right so how many have heard of the yes yeah so if you look up and you see something at higher latitude so fot points of the field lines don’t change but in any case you’re looking further out all right so the theis vision was launched to look at
Substorms and five satellites they going to be lined up the idea was to line them up in such a way as to see whether there was an in out or an out in scenario so I guess idea is there a reconnection that takes place that then snaps material and pushes it
In is there an instability that happens near Earth that occs sub sign that out that later so yeah anyway that was what the mission was designed for to basally had good coverage from deep in the tail all the way Earth and be able to see what’s going
On and so this has been very exciting Mission because there been a lot of interesting results um so here here are typical type of simulation that might driving convection field tail men just add more and more flux the tail the tail more thin until it goes unstable
And so this is the typee of thing you might expect tail here basically foring it from the top and the bottom pushing squeezing the tail and thinning it down and eventually at some point it pinches and reconnection occurs when the reconnection occurs you end up withow entropy plasma which isant and moves the
Earth and that’s the type of things that might result so that’s of plasmo that’s one Thing so the hitting of the plasma sheet can also result so people run Sim flanks but there’s actually a more effective way of fitting the plasma feet and that is that you have constant reconnection occurring on the day side that flux has to be replenished and it’s replenished through this
Azimu motion of the flux and then that will pull flux in from the tail and the tail will class get strong that forms this this is probably more effective so yeah entropy is pretty important so when reconnection occurs there’s a sudden change in the entropy and so you can see that the ENT
Initially black all and then here the ENT of that before it reconnects high and then after it reconnects you can see drop so at the moment of the reconnection the iny of the plasma drops and that’s actually causes it to and you can see a wave as time progresses
Profile out as more and more and you can sort of see that Simon Way one of my collaborators basically has these DP satellites that can measure the satellite use here and you can see the ions precipitating and from that you can actually infir what’s going on in the
And entropy one of the important things of entropy is that is an extensive property and so that means if you break off part of your domain it reduces the entropy and uh what we what we found when we looked at this is that the entropy gets reduced generally at the time of
Substance this is a statistical study of the plasma sheet before and after Subs you can see that the entropy is reduced in the plasma at the O subor but the interesting thing is that the specific ENT is not is not changed which means there’s basically no heating it’s all done from
Topology it all results from topology here’s a simulation of so this is actually showing that the reconnections lead to these Jets coming in like that and so reconnection can be responsible for those jets that you saw coming in but it’s also interesting if you look at
The substorm just prior to the onset of the substorm you see these beads beads that develop very highly structured beads in the in the ionosphere and these look like they’re a high ASM number mod and if you look at the wave spectrum just prior to Onset be onset you can see
There’s a low frequency mod that preds onet model as ballooning mod has all the right magnetic field properties and then at the onset you see all sorts of waves lots of so anyway this this slow frequency mode May and now if we look at the simulation that we just looked at here
Is the same type of situation here you see Kelvin helt on the flank but more importantly right here in the inner plasma sheet if you blow this up you actually see ballooning instability ballooning instability was denied by the global simul years they said they don’t they never Ballo mod
Simulation which is totally nonsense because plasma beta you should have mhd inability ballooning so anyway ballooning is seeing here and these can be the seeds for channels go so anyway it’s it’s an ongoing debate the reconnections given channels or channels also of see gets deed yeah so these streamers are we’ve been
Seeing the streamers that you’ve been seeing uh they also give you signatures in the ionosphere so what you saw in the simulation earlier with streamers going in uh a paper that tries to tie the structures to ionos Signature tries to identify those Bol flows with streamers and this a another type of simulation
This is a hybrid simulation so simulation I show you MD this is a particle also particle simulation you can see some different things the one thing is there because it’s a particle simulation can’t have as much resolution and so you don’t see as clearly the uh you can see the Kelvin
Helal but it’s not as structur make simulation anything you notice different in this simulation than in the previous one this is the pointing flux into the anyone notice anything different in this Simulation any so the dominant flow channel is coming in over here almost all the flows coming in are coming Dawn side instead of the Dust side that’s actually a kinetic effect see most flow channels coming on this you also have some way you have a very interesting
V and you also have a very strong very strong wind so so one thing that you can see here is the there’s a strong flow along this way that comes from the the particle drifts that we talked about earlier there’s no particle drifts in the m and then
This so anyway uh it’s important to also be able to model kinetic processes too because you can see that even here differences so you really want to model all right um this isort interesting so some storms uh when at what time of year Subs be
Seen so you have the AR spiral of the sun solar field is in theic plane mag field INE like that so what you can see is that when there’s more tilt of the dle toward the magnetic field Direction that’s going to more then if it’s more perpendicular so actually have the
Equinox is when you have the greatest tilt the direction of the Feld y comp a particular time of day there’s more likely to be alignment analment F and in fact the onset of geomag a little bit about geomagnetic storms so there was a mission Rec Van Allen thres objective to understand magne
Storms in particular hazards from radiation belt particles so storm is based on measure called PST storm index similar equatorial so anyway what’s measured is the deflection of the magnetic field so particularly the big storm gig so what you see if you if you have your magnetometer if we have our
Magnetometer right here you would see that the magnetic field measured would be 300 nanotesla smaller it normally is and that would be an indicator that there is a storm going on so storms have three phases initial phase down maximum main phase maxy coming back from the maximum the main phase typically is about
Hours of the r days week so we have sort of like two times now this can be compared with the time scale of substorm so substorms so storms usually last about a week or so one to five days the basally on day or many day recovery
Phase substorms on the other hand have a growth phase of about 30 minutes an onset that’s very rapid an expansion phase is about 20 minutes and then a recovery that’s on so vastly different time scales the main difference between storms and substorms is I think storms are primarily caused by the external
Dynamics of the mosphere of the solar wind and substorms are caused by internal damere okay we look at the radiation belt fluxes so these are I think I mentioned the radiation belt earlier look at the l l so we plotting L of four it means fi six is almost synchronous
Orbit okay so if you look at the radiation B fues what is the thing that strikes you most is the the variability of the R it’s just highly variable and can see at different energies it has different variability now if I were to plot the DST against
These sometimes when you have this storm you see DST negative sometimes when you have a storm radiation Bel gets really strong right here another time when you have a storm the radiation belt may just disappear and it’s not clear what’s going to happen when you have a storm sometimes it will lead to
More particles being energized sometimes to fewer to more particles being lost anyway thetion was aimed at looking at that I want to mention one of the most critical things about storms about how the response is going to be is the wave environment so here’s this really cool diagram I think Floren has
A anyway it shows the distribution of all these types of waves so you have Ulf waves that’s low frequency that’s like perod in some seconds you have emic waves which are about one second so his which hangs onto the pl plasmasphere look like might these when theere er it seems to light
To form in that and then you have EF chorus magnetosonic waves all sorts of waves and it’s thought that these waves can some of the waves can energize the particle and some of the waves can cause loss one of the major ones is the emic waves
There’s a narrow band you have it must be this hash region right here a very narrow band uh particles are really energetic so the radiation par probably come around drift other particles radiation way and so they’ll pass every 10 minutes to here they can actually be the FX Tu can
Be emptied in a second all right so and you know these are it’s not just this fancy diagram here’s a compilation of all the mod that you have ranging from electron Pyon chorus this over here Amic waves emic waves waves all these waves are being the particles move through all these
Fields and some of the key issues are where do the waves occur well I guess that’s to some extent understood fairly well now what level do the amplitude saturate that’s an important question because the wave part interactions depend on the ude what’s what’s the losses generally happen we have this distribution of
That this L any particle here will the particles out here will not go into theer comp the field and the hotter the particles is stronger that force will be it’s called force and it will cause the particles to that what waves will do is they will scatter waves that way
But when they SC scatter them into the lone then they precipitate so that’s out of the way control the acceleration radiation a lot of people try to model this loss process and and what is the feedback of the waves on the wave environment model how theise how they change the distrib
Distribs the wave environment so yeah the types of waves that are interest Ulf waves big large scale waves be induced by PC W glass in any case you can see that these waves the electrons will experience these waves different um yeah here’s just a people put particles into their mhd simulation
The electrons and you can they became energized through radial another process by which particles are lost um it’s called Magneto shadowing so I just I showed you what happens to the plasmasphere when when you change the convection velocity use confinement of the plasmasphere and a plume that goes out
It’s the same way with this Al layer so any ELR can also be um in this case it’s facilitated by the waves that may be generated helmet boundary uh so what happens is that the electrons fluxes the electrons come around this way they encounter the waves they get scattered and they actually get
Scattered out and then you get filling in this so get changes in the radiation flux BAS Bally hit the Lost then the waves will push them out um slides here I didn’t want to show this these are electromagnetic this is in the solar wind if there’s a source of waves
Here it’s these waves can actually generate waves in the equatorial reg andere and it’s actually sort of Co so this is what you callate down Theos here andate weird this happen this and this is really important when you consider the DI tilt because now the waves are generated here by the
Solar compressions coming that as Source in the solar wind and it’s going to generate all these Wes that can rapid whistlers are a very important loss mechanism as well so they’re caused by anop as the particle injections from the tail and the electrons which way do they
Drift um electr dri around right hand side dri this way and so as the waves drift around this way they excite Whistler wave as the electrons drift this way they excite Whistler waves and one of the consequences of the Whistler wave is that you can actually see diffuse electron precipitation in
The iOS this is the DSP obervation now looking down on the ionosphere and these are the diffuse electron a roll FL so what we’re going to see is you have an injection from the tail electrons move and start to drift around this way these are lower energy electrons not go unable wh
Westing Wes Whistler waves will then scatter particles into the a that’s sh here and I want to show you the evolution here as a function of time so it takes time for the electrons of this energy to go around and you can see the precipitation pattern actually shift around that you can
Ites basically track there’s also all sorts of cool things with the whistlers Shing there’s also some really neat dynamics that you get uh amplification of these waves trapping discuss that well the one of the big questions uh addressed by this radiation mission was is there local acceleration
Fusion part of the conclusion is that you do see localized R acceleration but then you see filling in after both mechanisms are at work giving you the um yeah this is sort of so Kelvin hel’s instability interesting so this is like what happens at the V so you see this boundary going
Disable yeah to get a Cascade you can see how the the boundary can become very dist and when you do particle simulations these structures here will out and you can get a lot of transported Mass into the vandos spere and just there are two mechanisms of Transport so one being high this is
North now Kelvin helt dominates transport sometimes for nor along with a reconnection that occurs at high latitude and this is a simulation where take particles from the solar from the from the solar wind and then look how they enter into the mosphere itself actually north is very interesting because the plasma sheet actually
Populates and becomes really dense when we I told you that reconnection maybe only 1% of the field reconnect enough but somehow lots of particles actually enter in and you can see they’re entering in through the flanks where the where the hom inability is and then some of the particles these
Sort of like pink ones are coming from the cusp those are have this have reconnection there and there that capes some of the particles but most of them are from the flame are anyway this isim I promise to talk a little bit about and you have processes that are static
Field current systems and dynamic induc static Aurora that you see and when you look at the Aurora you see sort of like General stable configuration and then sometimes you see aora highly variable so yeah Brooklyn discovered these current systems you saw in the simulation that doesn’t this way
This is just an average of the current systems you have upward currents which ones andur into the black ones so currents that are into the currents that come out of the isosphere are carried by electrons coming into theere and I showed you earlier that these field align currents develop when
You stretch the magnetic field you distort the shape of the DI when you distort the shape of the dipole it’s going to be the current systems like this if you don’t have enough density in the tail in the plasma sheet to carry the current into the carry the current
Out of Curr comes out the electrons into to carry the current what will happen is a parallel electric field will develop along the field line to push the so there’s not enough current carriers in the L cone the electric field will push accelerate the particles until you have enough
Particles to carry the current so it’s really the uh the lack of current carriers and and the Distortion of the magnetic field that will lead to these really energetic electrons specifically that’s a key key source of acceleration of of particles of electrons in veloc and I think I
Will show the dynamic C that’s actually so there are some Aurora many Aurora that you have pointing flux carried into the ionosphere and these alane waves so you heard of alane playing the strings of the magnetic field the strings and and they’ll have a natural frequency okay
You field here a peration will go down the field line and that peration will actually electr that’s detected when you see these types of waves coming that here yeah if we talk about different type of electron precipitation we have mono enerc monog energetic electrons and then we have Broadband electrons so
These broadband electrons are always seem to be associated with Alan waves and the monoenergetic electrons are more associated with the currents like I talked about but you can see that the fluxes of ions that come out of the osphere are also extremely large when PL the fu it accelerates the electr B
Aad and makes the ions come out and here’s just an example this is a monoenergetic here this is Broad and here’s a simulation so model the magnetic Fielding the field set standing what we see is like this and this is what happens to the energy we
See here we see almost like model andand ELR just like in the data um all resulting simply by plucking when you have a subor all right any questions much but I hope this give a flavor for some of the the issues exting I think the high resolution simulations that we see now are
Really yes thatu that’s so it for sure comes with better and smarter Compu comp so that’s this this is actually one of the big challenges is how to deal with large amounts of data so there’s data being processed being gathered actually process what are we going to do with
That so yeah that’s that’s actually one of the big challenges Segway so so yeah if you’re interested in statistical measures methods in machine learning this is a new opening field how do you deal with enormous amounts of data um so how are you going to analyze student that’s workation gab
Data that’s it’s really a challenge data everywhere and there’s both observations simulations yeah the same problem with simulations you’re generating an enormous amount of data with simulations so anyway these are these are huge challenges for the future how to deal with these enormous data sets and I can talk more yeah
So future strategies what to do so with data analysis I guess one of the one of the issues is to try to put fpgas on the satellite so you can try to process the data inog data processor on the satellite so you can actually do processing the data
Prior to transmission so you can send process data down that may be one way to transmit information that can’t transmit all the data that you gather at some so you might want to focus on various things feature identifications causal relationships predictions assessing uncertainty those all ch um simulations how do you extract teaches
So can you find reconnection sites in these simulations um causal Pathways when when you look at the simul what’s causing what in s figure it out are there methods to try to find that and how do you how do you verify that the Dynamics in the simul are the
Same as the Dynamics in the DAT and can how do you exrain the simulation for so here’s an example feature so here’s here’s data and train this is just method that CES in and tries to fit this data distributions so we have these G randomly distributed galaxian distributions they look for data they
Try to to go and capture it and after a number of iterations it’s actually model the data like this this is one way you can try to extract features from from data um shows here appli information to the solar surface to solar active regions find To actually identify these structures and then to look at how they basically information flow so does this structure how long does it persist like that are there and what they do when they’re moving around so you have to follow them and and be able to identify do they look the
Same or does it Evol so it looks different um yeah looking at Cross cutting applications so that’s one of the neat things about these typ methods is that apply Neuroscience just as easily as so here we’re looking at spikes in marmaset and it’s the same type of Dynamics as x-ray
Fles SO waiting times between X-ray fluxes and wai between spikes and normet data deep learning um this is an interesting thing okay you have a bunch of observations can you actually take the observ and figure out a differential equation that describes the system from just from the data and and in fact
It does fairly well on some some known equations you just take the output and it will reconstruct the equ so these are some neat things can uh here’s another example distribution functions have a particular skew in them when when you simulate when there’s a Rec there’s reconnection so
They this this simulation they actually identified locations of reconnection based on the distribution function and so went through and data mining find the sites so anyway that challenges of big Well there a really Applause