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  • MICHAEL SHORT: Hey guys.

  • So quick announcement, we're not doing nuclear activation

  • analysis today, because the valve that

  • shoots the rabbits into the reactor

  • broke and needs to be repaired.

  • So we'll likely just do this next Friday.

  • And instead, we'll have the whole recitation

  • for exam review, like I think we'd

  • originally, originally planned.

  • I also want to say thanks to whoever said, please write

  • lecture notes for this class.

  • It's something I think needs to be done.

  • And I just now biked back from meeting

  • with a publisher, or a potential publisher,

  • to actually get this done.

  • Because as I think as you guys have seen,

  • there's no one reading that does this course justice.

  • There are some that are too easy,

  • there are some that are too hard.

  • And there are giant pieces missing,

  • like most of what we're going to go into today--

  • sources of background radiation.

  • And where do cosmic rays come from, and what are they?

  • So thanks to whoever said that, because it spurred me off

  • on a let's make this into a book kind of thing.

  • Want to quickly review what we did last time.

  • We went over all the different units of dose and radiation

  • exposure, from the roentgen--

  • which is pretty much just valid for those measurements in air.

  • And I realized that yesterday I brought in the civil defense

  • dosimeter and passed it to one person,

  • and we didn't continue bringing it.

  • So I'll bring it to recitation.

  • It's not in my bag.

  • There is the unit of the gray, which

  • is just joules per kilogram.

  • Which you can calculate from stopping

  • power or exponential attenuation equations.

  • This is where you start, because it's

  • how you get from the world of physics

  • to the world of biology.

  • Into units of increased risk, or sieverts,

  • which is just gray times a bunch of quality factors, which

  • are either tabulated, or I'd like to see somewhat better

  • calculated.

  • They are calculated sometimes, but by empirical relations,

  • because that's usually good enough.

  • Biomeasurements tend to be pretty sloppy,

  • and I'm not that upset that these are empirical relations.

  • I'm going to skip way ahead past the detector stuff.

  • We didn't quite finish up the IF2D idea.

  • I think this is where we ended last time, where

  • we were talking about how do you detect dose

  • during cancer treatment.

  • And I was outlining one proposed way that we're thinking of.

  • Using this F-center based dosimeter,

  • which changes color when it gets irradiated,

  • you can implant it in the tumor.

  • And as it moves from things like breathing or swallowing,

  • you could feedback to the proton beam,

  • and only irradiate when it's in range.

  • Or play nuclear operation, and try not to hit the sides.

  • However, whatever you want to do.

  • And there's multiple implantation options for this.

  • We've thought about things like implanting a fiber optic

  • cable into the tumor, and then having a port

  • on the side of you that could do some in body spectrometry,

  • which would be pretty cool.

  • Could also put it all in a chip.

  • You could have the emitter--

  • either a broadband or single color LED--

  • the F-center, and the spectrometer all in a chip

  • that's implanted.

  • And with radio frequency power transfer,

  • so you don't need to put a fiber optic port

  • and plug it into the side of you.

  • Or however it goes.

  • And what we're doing next in this development

  • is nailing down what color change is given by what dose--

  • so the physics.

  • Develop an on-chip version.

  • Find a bio-compatible casing.

  • We've done the IP part, which is pretty cool.

  • As you can see with patent office at least

  • has taken in the application.

  • But it's neat that you need to know pretty much everything

  • you learned at MIT to pull off a project like this.

  • From the nuclear physics stuff, to the material science,

  • to the 22.071 electronics, to the medical stuff for biology,

  • to the financial stuff for econ.

  • In order to pull off an actual nuclear start

  • up project like this, you need everything you learn here.

  • Which is kind of a neat case study.

  • But now let's get back into what does a sievert really mean

  • in terms of increased risk?

  • Usually means the increased risk of some sort

  • of long-term biological effect, whether it's cancer

  • or some other genetic effects-- let's say mutations--

  • anything that would take a while to manifest,

  • and would manifest by slow but steady cell division.

  • And if you notice the difference between adults

  • and whole population, let's see--

  • yeah, sorry.

  • You can see right here that these--

  • not very much dose.

  • Let's say in the realm of 10 to the minus 2

  • sieverts can give you some increased risk for cancer

  • or some other effect.

  • So we're talking on the realm of 40 millisieverts

  • or so would give you some additional cancer risk.

  • That's not a lot of dose.

  • That's up to about the limit of the occupational dose

  • that you're allowed.

  • So when we talk about how much is too much,

  • I've taken some excerpts from this Committee

  • on Radiation Protection document.

  • This is from Turner, but the entire document,

  • as I mentioned, is up on the learning module site.

  • So you guys can see the actual verbiage where this is defined.

  • So your lifetime dose should never

  • exceed in tens of millisieverts the value of age in years.

  • Which means in some years if you get a little bit less dose,

  • you can get a little bit more dose

  • and still be considered safe or not

  • have any appreciable increased risk.

  • And while you're working, you should never

  • get more than about 50 millisieverts in a given year.

  • How was it for radiation workers?

  • So for you guys, what dose are you

  • allowed per year working at the reactor?

  • AUDIENCE: About five rem per year.

  • MICHAEL SHORT: Five rem per year,

  • which is 50 millisieverts.

  • Awesome, so it's--

  • AUDIENCE: [INAUDIBLE] to your eyes [INAUDIBLE]..

  • MICHAEL SHORT: Oh sure, yeah.

  • To jump back to that, if you're saying that there's actually

  • tabulated differences for different organs,

  • that's where they come from.

  • Let's say you can take less radiation to the same organ

  • and get the same dose in sieverts

  • measured in equivalent risk.

  • So I wouldn't be surprised if these are the organs

  • that you're not allowed to irradiate as much.

  • AUDIENCE: [INAUDIBLE].

  • MICHAEL SHORT: I'm surprised the eye isn't here.

  • Does it say retina anywhere?

  • Oh, OK.

  • Well that's just one table.

  • It's not necessarily the complete answer.

  • Yeah, so 50 millisieverts isn't that much.

  • Although if you think of it in the old xkcd units of banana

  • equivalent dose, eating a banana gives you

  • about 0.1 microsieverts.

  • So you would have to eat 50,000 bananas in a year--

  • no, I'm sorry, 500,000 bananas in order to incur that.

  • Well yeah, I was talking to someone at dinner

  • last night about the banana burning

  • experiment where we measured the activity in becquerels.

  • And then we can calculate how much dose in sieverts

  • it would take.

  • And he said, how many bananas would it

  • take to get some increased cancer risk?

  • About double this.

  • It would take about a million bananas

  • to give you about 100 millisieverts.

  • And I said, you know what else it would cost?

  • And he goes, 100 millisieverts.

  • No shit.

  • And I said, that's right.

  • Yeah.

  • Yeah, he totally didn't plan that,

  • but it just worked out that way.

  • Yeah.

  • And then how much is too much?

  • Let's say for the general public for a background for excluding

  • things like natural background and medical exposures,

  • you're not supposed to get about more than one millisievert just

  • walking about outside.

  • And you don't tend to get that much more.

  • Why are medical exposures not included, despite them being

  • pretty radioactive procedures?

  • Yeah?

  • AUDIENCE: Because they're very targeted.

  • MICHAEL SHORT: They are targeted,

  • and so they could give a lot of dose to certain organs.

  • But the amount of dose isn't necessarily

  • why we don't count medical procedures.

  • Anyone have any idea?

  • Yeah.

  • AUDIENCE: Was it because usually you wear a lead vest

  • if you're getting an X-ray?

  • MICHAEL SHORT: In some cases, like if you go to the dentist,

  • you'll get a lead X-ray.

  • But let's say you get a chest X-ray.

  • Why don't we care that a chest X-ray is way more than you get?

  • Because these things tend to save lives.

  • So you're absolutely willing to get extra radiation exposure

  • that may have a delayed effect if the immediate effect is

  • to save your life.

  • You had a question?

  • Or no.

  • OK.

  • Yeah, so we don't count medical things

  • because chances are you're doing them to improve or save

  • your life.

  • So what's a little bit of radiation

  • compared to let's say finding the blood clot or the aneurysm

  • or whatever it would take?

  • And then how much is enough?

  • AUDIENCE: Yeah, that's the table.

  • MICHAEL SHORT: This is the table that you're familiar with?

  • Yeah.

  • They actually talk about the lens of the eye.

  • And that's a heftier dose.

  • But also, the lens of the eye is not a very massive organ.

  • So this would mean do not stick remaining eye in neutron beam,

  • right?

  • Or you've seen that sticker, do not

  • stare into a laser with remaining eye.

  • Yeah, the same goes for the neutron beam ports coming out

  • of the reactor.

  • But the lens of the eye can take a fair bit more dose per unit

  • mass than the whole body.

  • The lens of the eye is not a particularly fast developing

  • tissue.

  • It can cloud up with an insane amount of radiation exposure.

  • That would take a lot more than 150 millisieverts to do,

  • though.

  • And then things like 500 millisieverts

  • for skin, hands, feet.

  • Pretty much just groups of muscle, bone, and dead skin

  • that not much is going on biologically.

  • Blood's flowing through it, but that's about it.

  • And notice that the regulations do differ a little bit,

  • but on the whole, they're fairly similar.

  • Same for the eye, same for the feet, same for the year.

  • Cumulative is a little different.

  • This says 10 millisieverts times age.

  • This allows you a little bit more.

  • Whichever recommendations you follow,

  • they're all pretty similar.

  • And our knowledge of how much dose

  • leads to how much risk hasn't changed

  • a ton in the last decade or so.

  • There's been all sorts of arguments for or against it.

  • Has anyone heard of this LNT or Linear No Threshold

  • model of dose versus risk?

  • This is something we'll talk a lot

  • about on the last day of class.

  • This is the theory that the amount

  • of risk versus the amount of dose is linear.

  • And no threshold means that every little bit of dose

  • gives you additional risk.

  • This is not supported very much by science.

  • I'd say it's not supported by science.

  • The converse argument is also not supported by science.

  • We just don't have the statistics at super low doses

  • to say what happens.

  • But the official recommendation is that there is a unit of dose

  • that we define as nothing, and it's 0.01 millisieverts--

  • about 100 bananas-- per event, let's say--

  • yeah, where does it say-- yeah, per source or practice.

  • So eating 100 bananas in one sitting

  • is considered to give you zero additional risk according

  • to the official guidelines.

  • So the guidelines put in place do not

  • follow the linear no threshold model.

  • But anyone that would claim that one or the other model

  • is absolutely correct has either got a huge sample

  • size of people that we don't know about,

  • or is probably extrapolating beyond what

  • the data will tell them.

  • So you'll see this argument flaring up quite a bit.

  • For the last day of class we'll have you read some arguments

  • for and against the linear no threshold model that

  • aren't just blogs on the internet,

  • but they're actual published articles

  • that have passed peer review.

  • And it's really hard to tell exactly what's

  • going on at low doses.

  • But meanwhile, let's focus on what you do

  • get that we can measure.

  • The actual contribution from background levels is about 50%

  • radon.

  • This is a natural decay product of radium.

  • It's just everywhere.

  • It's here right now.

  • It's all through the atmosphere.

  • This is why you want your basement

  • to be rather well ventilated, because it's

  • a heavy noble gas that accumulates down

  • in unventilated basements.

  • So you don't actually want your house

  • to be sealed up super tight, because you

  • can have radon accumulation.

  • Especially if you happen to live near a granite deposit

  • or on granite bedrock-- which everyone in New Hampshire

  • does--

  • radon levels are a little higher.

  • There's actually a story about a guy

  • that used to work at a nuclear plant somewhere

  • in Pennsylvania.

  • I don't know where, but he lived on top of a pretty good granite

  • deposit that was a few parts per million radium more.

  • So the radon levels in his house or in his basement

  • were much, much higher than would normally

  • be allowed for background.

  • And this guy used to set off the radiation

  • alarms coming into work.

  • Then he would breathe the nice clean radiation

  • free air in the plant and go out without setting off the alarm.

  • Eventually something had to be done.

  • I don't actually know what was done, but if any of you

  • can find that original story, that would be pretty cool.

  • Cosmic rays, another source that you can't shield from,

  • is about another 10%.

  • And we'll talk a lot about where these things come from.

  • Terrestrial radiation, well we'll count that as stuff

  • in the soil, stuff in the cinder block.

  • Wood happens to be a fairly radioactive substance

  • pound for pound, but it's not very dense compared

  • to things like brick or--

  • well, banana ashes is probably about the same as wood.

  • Internal, coming from you.

  • You'll have this on problems at number eight.

  • Because you all now know your internal radioactivity thanks

  • to going to environmental health and safety.

  • Did anyone see anything disconcerting in your spectra,

  • other than a tiny little potassium peak?

  • Anyone?

  • I'd say, ah, it's too bad.

  • But that's great, especially for you guys that work

  • at the reactor.

  • Medical X-rays.

  • It's assumed that everyone gets a couple of these a year.

  • You all go to the dentist and look for cavities.

  • You break something, you may get an X-ray of your hand or foot.

  • And this is let's say an average amount of medical X-rays.

  • Then a little bit of stuff leftover, consumer products.

  • This isn't counting things like Fiestaware,

  • those orange glazed plates and bowls

  • that were painted with a uranium based neon orange paint.

  • So we also don't tend to drink from Revigators anymore.

  • Has anyone ever seen or heard of a Revigator?

  • AUDIENCE: Yeah, was this in the '50s or '60s?

  • MICHAEL SHORT: Or even earlier, yeah.

  • So back in the '20s, people would

  • put radium ore in these containers and pour water in it

  • and say, natural radioactivity gets in.

  • It cures croup or the Jimmy legs or astigmatoid rheumatism,

  • or whatever other quack diseases there were in the '20s.

  • You can still find them on eBay, and that's not

  • accounted for in today's consumer products.

  • But this all accumulates the amount of dose

  • that you tend to get on your own.

  • You might get a couple of millisieverts a year of dose

  • just from background, especially depending on where you are.

  • And the big one--

  • whose spectrum I think you're all familiar with by now--

  • is that of radon.

  • Because we saw most of these peaks in the bananas.

  • Anyone have any idea why you would find so many radon decay

  • products in bananas?

  • Given that radon's everywhere, we

  • did notice elevated levels of specifically bismuth 214

  • and actinium I think 228 was the isotope we saw.

  • Where would those come from?

  • The what?

  • AUDIENCE: The soil.

  • MICHAEL SHORT: Absolutely, yeah.

  • Whatever radium's coming out from the bedrock,

  • that radon has to come up through the soil.

  • If that happens to decay in the soil,

  • it makes lead, bismuth, polonium,

  • other heavy metals that are taken by the plant's tissues.

  • In addition, radon daughter products

  • can plate out on the leaves themselves.

  • So this is one of those reasons that smoking

  • is such a bad thing to do.

  • Aside from the chemical effects, you

  • have giant fields of high surface area tobacco

  • that you then concentrate and dry up

  • into these tiny little sticks.

  • You have an enormous amount of leaf surface area

  • and dry vegetation that has taken all these radon daughter

  • products.

  • So most the dose you get from smoking

  • is lead, bismuth, polonium, actinium, radium.

  • Alpha emitters.

  • As we saw last time, to remind you

  • guys of the quality factor for alpha particles,

  • it's as big as it gets.

  • Anyone remember why that is?

  • Why are alphas so damaging if they get into your tissues?

  • AUDIENCE: Because they're big.

  • MICHAEL SHORT: They are big, so they have high mass.

  • And?

  • AUDIENCE: Short range.

  • MICHAEL SHORT: Short range coming

  • from their high relative charge.

  • They have quite high stopping power.

  • And they will deposit a lot of energy

  • very close to where they are emitted.

  • So their range is very small.

  • So that armor piercing bullet analogy

  • comes to just an armor piercing bullet that explodes right

  • out of the barrel of the gun.

  • And they do quite a bit of radiation damage.

  • We jump back to the right slide without inducing a seizure.

  • I think we've looked before at the radon decay chain.

  • This is a simplified version, because there

  • are different branches or different possibilities

  • for decay, but some of them have extremely low percentages.

  • So this one's simplified quite a bit.

  • But it is whenever radon decays, it gives off

  • a bunch of alpha and beta emitters

  • that last anywhere from minutes or seconds to days and so.

  • For every radon atom that you absorb,

  • you end up getting four or five alphas and betas,

  • depending on how long it stays into your system.

  • And then mapping out radon in the US.

  • You have quite different amount of radon dose

  • depending on where you are.

  • And I wanted to skip ahead and overlay

  • a couple of maps of the US.

  • So this is a terrestrial--

  • oh, I'm sorry, that's the wrong one.

  • Let's just look at this one, yeah.

  • Anyone notice any patterns here?

  • Where do you tend to get the most radon?

  • What sort of features would one live near when

  • you get a lot of radon dose?

  • AUDIENCE: Mountains.

  • MICHAEL SHORT: Mountains, which tend to be made of?

  • AUDIENCE: Rocks.

  • MICHAEL SHORT: Rocks, which tend to contain a lot of radium.

  • Especially granite and other such rocks.

  • The Conway granite, named after up in Conway, New Hampshire,

  • is about 52 parts per million uranium or radium.

  • So it's a fairly toasty rock.

  • You can actually tell there with your Geiger counter,

  • if its count long enough, that there

  • is a little bit of radioactive ore in that Conway granite.

  • Not nearly enough to matter at all,

  • and certainly not enough to stop you from making fancy kitchen

  • countertops.

  • But I wonder if folks would buy those

  • if they knew that there was 52 parts per million of something

  • with a half life of 9 billion years.

  • I somehow think it would matter to people,

  • but it really doesn't.

  • AUDIENCE: They put the radiation symbol on it [INAUDIBLE]

  • MICHAEL SHORT: Yes, engrave that.

  • If they made the radiation symbol a little induction

  • stove, that would be pretty slick.

  • Yeah.

  • And then in terms of relative radon risk,

  • how much actually matters?

  • I like this graph.

  • Despite being difficult to read, it actually

  • shows how much the average indoor level

  • compares to all the different things you could do.

  • Like getting 2,000 chest X-rays per year versus 100 times

  • the average indoor level.

  • That's about what I heard that fellow in Pennsylvania

  • had is like 100 or 80 times the normal radon

  • levels from living underground on this giant granite deposit.

  • It's like getting 2,000 chest X-rays per year,

  • or something like smoking four packs a day.

  • I know some people that do this.

  • They don't tend to be that afraid of the radiation

  • that they're taking in from smoking.

  • But yeah, it's pretty insane how much radiation you get.

  • People are afraid to get one chest X-ray, which is not even

  • on this map.

  • One chest X-ray worth of radiation

  • gives you much, much less than living for a year in a house,

  • which we all tend to do.

  • Then if you live in a brick or cinder block house,

  • you actually get a fair bit more radiation,

  • because these are fairly radioactive building materials.

  • And I'll show you those activity levels in just a sec.

  • As far as exposure sources, again,

  • to look at the relative amount of terrestrial gamma ray

  • exposure, you can correlate that pretty well

  • with not green regions on a topological map.

  • So look at the really low levels down here,

  • correlates with low lying vegetative areas around here.

  • Colors are a little more extreme on my screen,

  • but you can see this is all low lying right here.

  • From Louisiana, Florida, up the east coast,

  • until you get to the Appalachian Mountains and such.

  • So pretty striking correlations there.

  • And it all comes from what we call the primordial nuclides.

  • These are unstable nuclides that have such long half

  • lives that they still exist, despite the universe

  • being 15 billion years old, or whatever supernova

  • formed our solar system being five plus billion years old.

  • Things that we've already studied almost to death,

  • like potassium-40.

  • And you can see that's about 0.011% of all potassium

  • is radioactive potassium-40.

  • About 10% of which gives off gammas in--

  • what is it, 90/10?

  • I forget the split.

  • But can give off either betas and then a gamma,

  • or positrons and then a gamma.

  • Then things like rubidium, in the same column

  • as sodium, potassium, and cesium, so it behaves kind

  • of like a salt-like element.

  • There should be some for-- are there any for chlorine too?

  • Some of the other important ones to note, oh, platinum.

  • Does anyone has any platinum jewelry?

  • Does anyone have any platinum jewelry?

  • Good answer, yeah.

  • I don't either.

  • I teach at a college.

  • Also, I don't like wearing jewelry.

  • But there'll be all sorts of these primordial nuclides

  • that you can't really do anything about.

  • They're just there.

  • Note that the half lives are really, really long.

  • And as you know now, the half life

  • is going to be inversely proportional to the activity.

  • Despite almost all indium--

  • look at that, 95% of the indium that you'll find emits betas.

  • Doesn't stop people from using it as these awesome glass

  • to metal seals for vacuum components.

  • Because once in a while it might emit a beta ray,

  • like a whole gasket might emit a beta once

  • every millennium or so.

  • But these half lives actually are measurable.

  • And that begs the question, are there elements

  • with longer half lives that are just too long to measure?

  • You think what does it mean to have a half life of 10

  • to the 15 years, given that the universe is on the order of 10

  • to the 10 years old?

  • Is it possible that all nuclei will

  • decay till the end of time?

  • I've seen some documentary such things

  • and don't call this a science that say, oh 10 to the 40 years

  • from now, the last protons decay,

  • or the last whatever elements decay

  • into all protons and neutrons.

  • Don't know if that's true, but it

  • does make me wonder, are some of the other so-called stable

  • elements just have ridiculously long half lives?

  • It's something to think about.

  • So let's take a look at the building materials,

  • and see what's in the typical things around us right now.

  • You can see how much granite, radioactive thorium,

  • and potassium are in these building materials.

  • And how many usually is measured in picocuries per gram.

  • A picocurie is already less than a becquerel per gram.

  • Because a curie is what, 3.7 times 10 to the 10 becquerels.

  • And a pico is a 10 to the minus 12.

  • So things on the order of a few picocuries per gram,

  • a gram of that material might emit

  • one disintegration per second.

  • Not a lot of radiation.

  • But take a look at how much potassium there is in granite.

  • Nanocuries per gram, that's getting into the integers

  • worth of becquerels.

  • If you look at wood, check that out.

  • Anyone heard of potash before?

  • It's one of the ways we get potassium.

  • So if you take wood based things and you burn them in a fire,

  • you drive off all the carbon in the water,

  • you're left with these kind of whitened salt and pepper ashes.

  • That's potash.

  • That's the ashes left over in the pot

  • after you burn stuff in a fire.

  • They're quite potassium rich.

  • So I think what we'll do next year,

  • instead of burning a bunch of food,

  • is just burn a bunch of wood.

  • We'll have a nice bonfire, collect the ashes.

  • And we can see how much potassium there is in wood.

  • Which pound for pound, if you see on this list,

  • is the most radioactive building material there is.

  • Just that wood happens to be pretty inexpensive,

  • and consists mostly of water, lignin, and other carboniferous

  • materials.

  • They don't have carbon-14 on this list,

  • but let's take a look at some of the other ones.

  • So sandstone cement has a pretty toasty signature to it.

  • Gypsum drywall.

  • What is it, 13 parts per million uranium in all the drywall

  • you tend to find.

  • Anyone scared yet?

  • Because you shouldn't be.

  • It's like I mentioned before, this

  • is the slide I want to show to most folks

  • in the general public.

  • There is such a dose as nothing.

  • And that's pretty much what you get from,

  • let's say, a day's worth of being around these building

  • materials.

  • It's just about nothing.

  • It's after the building materials.

  • There we go.

  • Seawater is another great source of radioactivity.

  • Enough so that people have actually

  • proposed harvesting uranium from seawater.

  • So the total amount of activity in the ocean,

  • there's something like 11 exabecquerels

  • of radiation contained in the uranium in the seawater.

  • Which means you should be able to have a gigantic trawler

  • flying out around in the ocean, and just floating

  • through the seawater, picking up atoms of uranium

  • here and there.

  • Because technically, there's enough to power

  • the world for like 2,000 years.

  • The problem is the ocean is big.

  • It doesn't stop people from actually working on it.

  • So it's neat to think that there's

  • a whole lot of carbon-14 and tritium

  • and uranium in seawater.

  • 300 picocuries per liter.

  • Anyone have any idea why there's so much more potassium activity

  • than anything else in seawater?

  • It's because it's salty, yeah.

  • And potassium's just like sodium.

  • So there'll be a fair bit of potassium

  • in the seawater, 0.0117% of which is potassium-40.

  • And so last year, people asked, what, uranium from seawater?

  • How is that even possible?

  • So this is the part in the course where

  • I'm going to pull out a lot more recent papers

  • to show you some of the cooler innovations going on.

  • So you could use this adsorbent.

  • And adsorbent.

  • Does anyone know what adsorption means, not absorption?

  • Adsorption is when something sticks

  • to the surface of something.

  • Absorption with a B is when it actually gets

  • incorporated into the bulk.

  • So folks are thinking about making high surface area

  • materials that can adsorb selectively atoms of uranium.

  • So you send out this huge braided net, or a huge stack

  • of adsorbing material with a D, and just go around

  • in the ocean.

  • Attach them to tankers or cargo ships,

  • and just have them pull in product

  • as they go from coast to coast.

  • And by actually changing around the chemistry and the geometry

  • of this, you can enhance things specifically for uranium

  • by about a factor of three.

  • And this yellowcake right here next to an actual ruler--

  • that's 50 millimeters right there--

  • that was obtained directly from seawater.

  • So you can actually pull yellowcake out of the ocean.

  • Just not very much of it.

  • And the way these work is there are interesting compounds that

  • selectively absorb uranium into their structure,

  • not by direct chemical bonding, but by getting something close.

  • For example, my wife tends to study metals bonding

  • to proteins.

  • And it's not necessarily always a full chemical bond

  • like you might think, but the protein

  • can kind of wrap around a metal ion, transport it places.

  • Similar thing going here.

  • I'm not going to pontificate anymore

  • on it because the title has the word organic in it,

  • and I am definitely not an organic chemist.

  • Don't want to tell you anything wrong,

  • but I do want to tell you you can actually see this paper

  • to find out what sort of compounds

  • selectively grab onto uranium.

  • And if there's a seawater floating through,

  • and uranium happens to flow nearby, it can bond to it.

  • You can then somehow squeeze out or burn off that adsorbent,

  • and there you get uranium.

  • Now let's talk about what's in the body

  • and interpreting the spectra that you got from EHS,

  • your full body spectra.

  • If you take a look at how much uranium

  • there is in the body, wow, there's some.

  • Every one of you is got about a becquerel of uranium

  • in the body.

  • But if you look at the relative amounts, rate it was at.

  • The only things that really matter a ton,

  • potassium-40, about 4.4 kilobecquerels per human.

  • So each of you is giving off 4,400 potassium gammas

  • per second.

  • Most of them just flow right through all the other people.

  • And then carbon-14, about 3.7 kilobecquerels.

  • Pretty interesting to know just how much radioactive stuff

  • you have in your own body.

  • You will need this table for homework number eight

  • when I ask you a pretty fun question.

  • Then there's all the various medical procedures.

  • The ones that aren't counted in your annual dose because they

  • tend to save people.

  • But now let's look at the dose in millirem

  • So if you want to figure out what this is in sieverts,

  • just divide by 100.

  • So a regular old chest X-ray, 0.1--

  • let's see, how does it go?

  • 100 rem in a sievert.

  • Yeah, so about 0.1 millisieverts, or 1,000 banana

  • equivalent dose.

  • Not terrible.

  • Which is why if we go back to that chart of all

  • those relative risks, if you look

  • at the average indoor level, it's like getting-- well,

  • I would have to guess maybe 40 chest X-rays per year

  • based on this rather crude scale.

  • And you're allowed to get around a millisievert

  • or a few millisieverts of radiation per year.

  • That sounds like it checks out mathematically.

  • Let's look at some of the other crazier ones.

  • Dental bitewing.

  • Yeah.

  • So anyone ever bite down on something

  • where you have to get an X-ray through the side of your mouth?

  • Quite negligible amount of dose, yet they still

  • put the lead apron on you.

  • I'm guessing that's mostly for show, because that's

  • very, very little dose.

  • It's well beyond the 0.1 microsieverts of something

  • that counts as nothing.

  • But there's not a lot of dose going into these things.

  • Let's see what really does give you a whole lot of dose.

  • 10 millisieverts for a CT scan, or a whole body CT screening.

  • That's a pretty hefty amount of dose.

  • Right there with one procedure you

  • may get more than your normal annual background dose.

  • But if you're going in to look for stuff,

  • chances are you need to find whatever you're looking for.

  • So we don't count it.

  • And it may give you a slightly higher chance

  • of developing cancer much later down the line

  • when that cell that gets mutated divides.

  • But it's probably going to save your life in the next hour,

  • or the next day.

  • So definitely worth it.

  • Let's see, the worst--

  • what's the worst procedure we can find?

  • Noncardiac embolization.

  • I don't know enough biology words

  • know exactly what that means.

  • AUDIENCE: I know what noncardiac means.

  • MICHAEL SHORT: Yeah, I think we all know what noncardiac means.

  • Good.

  • This isn't 7012.

  • Nonmedical procedures-- or more medical procedures, I'm sorry.

  • Where's the techneitum scan?

  • Yeah, notice how many of these things

  • have technetium imaging where you'll inject technetium

  • into a certain organ or a certain vascular or lymph

  • or whatever system.

  • Some of these things can give you a fair bit of dose.

  • Like again, maybe a heart stress rest test

  • can give you double or triple your normal background dose.

  • This is why you have to declare to airports

  • if you've just had a medical imaging procedure,

  • because this is well more than enough to pick up

  • on any sort of airport radiation monitor.

  • So again, if you ever get a medical procedure

  • with any sort of radiation, anything,

  • do declare it, because it's quite measurable.

  • Then there's radiation from altitude.

  • I may have mentioned already that the reason that pilots

  • can't fly for a certain number of hours is not fatigue,

  • but it's radiation exposure.

  • When you start to look at how many

  • microsieverts you get per hour on the ground, 0.03.

  • Right about down at that-- hanging around for an hour

  • is a negligible dose.

  • You go up to international air travel,

  • that goes up by a factor of little more than 100.

  • And so you get a fair bit of radiation exposure.

  • If you take your annual allowable occupational

  • limit of 50 millisieverts, divide by 3.7 microsieverts,

  • you're getting close to 86--

  • what is it?

  • How many hours in a year?

  • Let's see.

  • There's three times 10 of the seven seconds in a year.

  • So divide that by 3,600.

  • That's getting on the realm of 10,000.

  • That's about the conversion factor.

  • So you can't spend your life in the air,

  • because you'd get too much radiation according

  • to the occupational risks.

  • And so actually in addition to some interesting measurements

  • that have been published in papers,

  • we've actually had students go out

  • and build radiation altimeters based on the MIT Geiger

  • counter--

  • removing the speaker, of course, because you

  • don't want to clicking Geiger counter on a plane.

  • That'd be kind of a stressful situation.

  • Let me show you one example of these.

  • Are also published from a paper, but we have pretty similar data

  • from-- if you want, to go talk to Max Carlson,

  • one of my graduate students who hooked up his Geiger counter

  • to an alarm clock--

  • the case that had [INAUDIBLE] in it.

  • I think this was a poor choice of case for a plane

  • because it looks kind of like a time bomb.

  • But luckily nobody found it, and he was able to get the data.

  • But you can see just how much more data you get.

  • And you can correlate the height that you're at with the dose--

  • in this case, microroentgens per hour or microrad depending on--

  • what is it-- ambiguous unit definition right there.

  • But it's quite noticeable.

  • So for those of you who have built Geiger counters

  • and have cell phones, and don't want to have a fake time bomb,

  • you can actually hook in your Geiger counter

  • to the microphone port of your cell phone.

  • And with a few available radiation apps,

  • you can actually monitor your dose in microsieverts.

  • Assuming that it all comes from gamma rays, which

  • is most of what a lot of cosmic rays will produce.

  • So it's a pretty safe approximation

  • that your dose in gray flying on the plane

  • is also your dose in sieverts, because it's

  • whole body, and its gammas.

  • So I'd say try this at home, kids.

  • This is one of those things I recommend you try out.

  • Speaking of these cosmic rays, where did they come from?

  • Well, this is a question that's been under debate,

  • and was more completely answered just a few years ago.

  • They come from very high energy particles from somewhere.

  • It had been argued, do they come mostly from solar flares,

  • or did they come from elsewhere in the galaxy?

  • Mostly we're talking about things like high energy protons

  • or other charged particles.

  • We're also talking neutrinos.

  • Anyone know about how many neutrinos

  • are theorized to pass through you every second?

  • Trillions.

  • Yeah, something like that.

  • But they basically don't interact with matter.

  • As I showed you guys near the beginning,

  • it takes a gigantic salt mine full of water and exploding

  • photomultiplier tubes in order to catch two or three neutrinos

  • a day if you're lucky.

  • So let's say those don't really matter

  • in terms of background dose.

  • But when those high energy particles interact

  • with the oxygen and nitrogen up here in the atmosphere,

  • they produce a shower and cascade

  • of additional ionization and high energy particles.

  • So it's been said that solar flares and such will accelerate

  • charged particles from the plasma

  • in the sun towards Earth.

  • They're deflected somewhat by the magnetic field

  • of the Earth, but they tend to enter right here

  • at the-- what is it?

  • At the poles.

  • I'm sorry, that's the simple word I was looking for.

  • Until recently in 2001, they were looking specifically

  • at the evidence for or against the idea that coronal mass

  • ejections-- which means large ejections of mass from

  • the outer layers, these sparcer layers of the sun--

  • was responsible for most charged particles and cosmic rays.

  • Skipping the stuff that's not in bold,

  • it appears to be that the CME bow shock

  • scenario has been overvalued.

  • So for a while, folks were saying

  • most cosmic rays come from the sun-- that's our nearest star.

  • By making really, really careful measurements of the energy

  • and lifetime of these cosmic rays,

  • this has actually been somewhat disproven

  • that this is the major source of cosmic rays, which

  • is pretty cool.

  • But let's talk about where they actually come from.

  • Reactions that you can probably understand.

  • So extremely high protons enter the atmosphere.

  • They all start as high energy protons.

  • And when protons are high enough energy--

  • and like I do probably in every class ever,

  • I'm going to pull up Janis to show you something.

  • They can undergo what's called spallation.

  • It's the same principle that the Spallation Neutron

  • Source at Oak Ridge National Lab works on

  • is shoot in extremely high energy protons,

  • out come neutrons.

  • So as usual, it didn't clone the screen right.

  • So just bear with me for a sec.

  • I'd like to, for probably the first time in this course,

  • switch databases to the incident proton data.

  • Is that actually working?

  • OK, good.

  • So we'll leave the incident neutron data,

  • we'll go to the incident proton data.

  • We'll stick with the same library.

  • Let's see how much they have.

  • Not much, but enough to matter, because there's

  • a lot of nitrogen-14 up in the air.

  • Let's see what happens when protons hit nitrogen-14

  • all the way at high energy.

  • So don't quite know what a negative cross-section refers

  • to.

  • But at high energies, this is definitely a possible event.

  • And let's see, there's not a lot of cross-sections

  • to look at here.

  • Let's try oxygen-16.

  • Not much.

  • We'll stick to the slides then.

  • So when a high energy proton strikes a nucleus,

  • it can eject neutrons.

  • And those neutrons can then cause activation reactions,

  • and then emit things like proton or tritium, leading to--

  • that's where your carbon-14 comes from.

  • Comes from nitrogen-14.

  • So in comes a high energy proton, releases a neutron.

  • That neutron hits nitrogen-14, releases a proton,

  • out comes carbon-14.

  • So this is why it's being constantly generated

  • in the atmosphere.

  • It's not like there's a certain amount that

  • was there at the beginning of the universe and decays,

  • because its half life is only 5,700 years.

  • So this is part of why radiocarbon dating works,

  • because we have cosmic rays.

  • It's kind of a neat connection to make.

  • If there weren't cosmic rays, all of the carbon-14

  • would decay pretty quickly in the universe time scale.

  • And we wouldn't have this form of radiocarbon dating.

  • And then same thing for tritium production in the atmosphere.

  • This is where some of that tritium naturally comes from,

  • is it makes carbon-12-- which is the normal form of carbon--

  • but out come tritium, which there is going

  • to be some constant isotopic fraction of tritium in all

  • the world's hydrogen. Some of it's being

  • generated in real time.

  • And we do have these spallation sources on Earth.

  • Like I mentioned, the Spallation Neutron Source

  • has a gigantic synchrotron.

  • We've seen these before, which just injects in this case

  • protons, which circle around and around and around, accelerating

  • until some of them are extracted and fire onto things

  • like a liquid mercury target, some neutron rich liquid metal.

  • So you want something that's very neutron rich.

  • You want something that's very dense.

  • You want something that's fluid so you can cool it better.

  • And you want something with high thermal conductivity.

  • That's where the metal comes in.

  • So a liquid metal you can keep cool really well.

  • Because when you're firing lots of 800 MeV protons into it,

  • you generate a tremendous amount of heat.

  • And this is what the actual thing looks like.

  • You can get tours of this down in Tennessee

  • at the Oak Ridge National Lab.

  • Actually, I've driven up here before.

  • I recognize this from the map.

  • That's pretty cool.

  • So where the actual neutron science stuff

  • happens, where all the scientists sit

  • with their targets, there's quite a bit of stuff

  • going on behind it.

  • So there is a gigantic--

  • you can see that's a parking lot for scale.

  • There's a gigantic linear accelerator

  • shooting into the synchrotron ring, which

  • then fires the protons here into the target

  • into one of any number of end stations, which creates a not

  • quite push button, but turn on-able pulsed neutron

  • source, which is pretty slick.

  • And again, parking lot for scale.

  • Takes a lot of magnets to bend an 800 MeV proton.

  • That's what it actually looks like.

  • Has anyone ever seen one of these synchrotrons?

  • Like at Brookhaven or at Oak Ridge or at anywhere?

  • They're quite interesting things.

  • The closest one to us is the NSLS,

  • or the National Synchrotron Light Source version

  • two at Brookhaven National Lab.

  • It's like a 2 and 1/2 hour drive down in Long Island.

  • I don't know if they're doing tours yet,

  • but it's about a kilometer around.

  • And I was told they did bike races around it

  • to see who could beat the protons, which

  • of course everybody loses.

  • But they are pretty insane collections

  • of magnets, vacuum equipment.

  • And once in a while a proton will pass through.

  • And then there's the spallation source itself.

  • So this is what the target looks like.

  • There's going to have to be liquid metal cooled in.

  • And then out of here come lots and lots and lots of neutrons.

  • Enough neutrons that you still need

  • hot cells to deal with things.

  • They're still quite radioactive, inactivated.

  • But it's not a reactor.

  • Other ways of making neutrons.

  • Speaking of, has anybody seen the pulsed fusion source

  • that we have down in Northwest 13?

  • No?

  • We have a pulse neutron source that you

  • can come take a look at.

  • It's an electrostatic fusion pulsed machine.

  • There's a whole bunch of tritium and deuterium

  • in this palladium sponge, what happens to hold hydrogen

  • and its isotopes very well.

  • And with a very quick pulse, you can have a tiny pulse fusion

  • and generate about 10 to the 8th neutrons that actually is

  • a push button neutron source.

  • So if you want to see a neutron source beyond reactors,

  • go down to the vault in Northwest 13

  • and ask to see that.

  • We did a quick experiment before trying

  • to activate cell phones to see what was in them.

  • We did not generate enough neutrons to do so.

  • But this cell phone has definitely seen a few fusion

  • neutron pulses.

  • And we checked later, it's not giving off

  • any residual radioactivity.

  • At least we can measure.

  • That was a fun failed experiment.

  • And then comes the craziness.

  • Since it's about five of, I want to get

  • into things that will definitely not be on the exam.

  • So just sit back and enjoy and stop taking notes.

  • Complete insanity can happen with super high energy

  • electrons.

  • We've already talked about Bremsstrahlung.

  • We have talked about synchrotron radiation, where

  • you have a charged particle going along a magnetic field

  • line.

  • It changes direction and gives off X-rays.

  • We haven't talked about inverse Compton scattering.

  • Interesting process here.

  • In comes a low energy photon, hits an electron,

  • out comes a higher energy photon.

  • Compton scatterings usually think of as the other way

  • around, where a high energy photon comes in, scatters off

  • an electron, loses energy.

  • In this case, a high energy electron

  • colliding with a low energy photon

  • can impart energy to the photon.

  • And you can actually calculate-- or in this case,

  • I've just taken from a paper--

  • the energy gain from inverse Compton scattering,

  • as well as whatever cross-section there is.

  • And even though this is a very infrequent process--

  • well, the universe is pretty big,

  • and contains a lot of things that

  • have magnetic fields like stars and black--

  • whatever else happens to have magnetic fields.

  • And you can identify radio sources

  • by looking for these inverse Compton scattered X-rays.

  • So the Chandra X-ray map, I believe a piece of which

  • or a receiver for which is up in the building in Porter Square.

  • If you guys go down three stops on the red line,

  • you'll see this little area full of Japanese noodle

  • shops, Lesley University, a bunch of galleries.

  • And in a little--

  • I think it's still there-- and a little sign that says, oh,

  • and there's the Chandra X-ray Observatory.

  • Whatever.

  • They may or may not have moved, but I

  • recommend you check it out.

  • And then what happens to those electrons?

  • Well, they can actually decay.

  • Pretty interesting things.

  • And so some of this inverse Compton scattering

  • has gone into the evidence for or against where

  • cosmic rays come from, because you should

  • see electrons of a certain energy

  • after undergoing this process.

  • I think I will skip ahead.

  • Oh, I won't skip ahead.

  • And so what these cosmic rays can produce

  • is what's called positive, negative, or neutral pions.

  • Other subatomic particles with masses somewhere

  • between protons and electrons that themselves

  • can undergo different reactions or different decays into muons.

  • And don't worry, muons and pions and such

  • are not part of the topic of this course.

  • But they do have known lifetimes,

  • they do have known masses and charges,

  • they do have known stopping powers.

  • We should be able to measure them.

  • And there is a cosmic muon detector at Boston University.

  • Or rather, it's a pair of detectors

  • that looks for this coincidence of one muon

  • scattering off one detector, or interacting,

  • and another particle being sensed directly beneath.

  • So we can actually sense these muons to confirm or refute

  • the theories about where they come

  • from in terms of cosmic rays.

  • And these neutral pions are what end

  • up creating these gamma rays.

  • I think they were around the 70 something MeV range.

  • So if these theories about them are correct,

  • we should be able to sense these gamma rays,

  • and sense how many of them there are as a function of energy.

  • That's not what I wanted to do.

  • Let me recreate presentation mode,

  • because this is definitely delving into the kind of stuff

  • that, well, I'm not an expert in.

  • So a quick detour into subatomic physics.

  • You guys probably have heard of that protons and neutrons are

  • not the smallest building blocks of matter.

  • They themselves can be composed of quarks and antiquarks

  • with different charges and different masses.

  • They're given different flavors.

  • I don't know who came up with this terminology,

  • but it's kind of fun.

  • Things get kind of whimsical when

  • you get into subatomic physics.

  • And these quarks and the gluons between them

  • are what composes protons, neutrons, in their antimatter

  • counterparts.

  • And these sorts of things can also undergo their own decay

  • and reactions.

  • So when beta decay occurs, it's actually

  • one of these up quarks turning into a down quark

  • and releasing an electron and an antineutrino.

  • But again, we're not going to delve even deeper into this.

  • There are other particles composed of other arrangements

  • of quarks.

  • So if you have just an up and a down, you have a positive pion.

  • Which should have a charge--

  • I think one's 2/3 of one's minus 1/3.

  • Yep, that is correct.

  • So a plus pion should have a charge of 1/3

  • the charge of an electron.

  • So if you know the mass of some particle

  • because you know the number of quarks,

  • and you know the charge of it, you

  • should be able to calculate its own stopping power.

  • And figure out how many should get

  • through the atmosphere and such, or how many

  • get absorbed in your detector.

  • And so when a very high energy proton collides

  • with an atmospheric molecule, it creates neutrons,

  • creates a shower of pions.

  • These neutral pions-- much like electron positron interaction--

  • can produce their own gammas.

  • So they can spontaneously decay from particles

  • that are mass into gamma rays of pure energy.

  • Which then go on to create their own shower of electrons

  • and positrons by pair production.

  • Because as we saw, the higher in energy you go for photons,

  • the more likely pair production becomes.

  • And there you have it.

  • This is part of the 22.01 stuff, but taken to the nth degree.

  • And then the evidence for pion decay

  • comes from extremely fine measurements

  • of the number of these pions as a function of energy.

  • Or in this case, look at that.

  • They're-- what is it-- ergs per centimeter squared per second.

  • What does that unit physically mean?

  • Not going to get into that.

  • But at any rate, there are different models

  • for how many of these pions or their high energy gamma

  • decay products should be observed.

  • And by looking at those very carefully,

  • you can tell where they came from.

  • Should they have come from coronal mass discharges,

  • so we should know what energy those protons should be,

  • or some other source

  • But I am going to stop there, because it is five of.

  • So after that crazy detour, give you guys 10 minutes to degas

  • and absorb some neutral pion gamma decay products.

  • We'll meet upstairs in 10 minutes for an exam review.

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