This is an introductory astronomy survey class that covers our understanding of the physical universe and its major constituents, including planetary systems, stars, galaxies, black holes, quasars, larger structures, and the universe as a whole.
Interstellar Medium: General Properties
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Del curso dictado por Caltech
The Evolving Universe
369 calificaciones
De la lección
Stars and Planets
Conoce a los instructores
S. George DjorgovskiProfessor
Astronomy
Let's first talk about the interstellar medium in our galaxy,
and here is one of the pretty pictures from Hubble that shows
a reasonably typical combination of interstellar clouds.
So simply it is the gas and dust between stars, yeah.
And it is generally mostly concentrated in the galactic disc, but not entirely.
And it's stuff from which stars are made, or galaxies for that matter.
All of the baryons in the universe, protons,
neutrons, and electrons that go along with them, were originally in form of a gas.
And now we think that, in fact, maybe 90% of all ordinary matter
in the universe is in form of gas, not stars.
So stars are in sort of an ecological equilibrium with interstellar medium.
They form from interstellar medium, from gas clouds that condense.
We'll talk about that in a moment.
They live their lives, then some of them explode, others lose their envelopes and
thus, they contribute back to interstellar medium.
But the material that comes out of them was enriched by
heavier chemical elements that are cooked up in stars and then new stars form.
Stars also interact with interstellar medium.
They can change it, they can ionize it, they can be mechanical
effects of shock waves and so it is a fairly complex system.
There isn't a continuum of properties,
but it does fall into several different categories that I'll define in a moment.
So there are three basic forms of interstellar gas
that are associated at least with the galactic disc.
First, young stars emit lots of UV radiation, and that means
they will pump up internal energy levels of atoms or ions to higher energies,
which occasionally they will lose electrons and they will recombine.
And when they do this, they shine an emission light.
You'll see the red color tends to go with these.
And anybody have a guess what is the spectroscopic line that dominates this?
Let's try this way.
What chemical element is it likely to be from?
>> Hydrogen.
>> Yes, hydrogen, yeah.
So anybody cares to guess what's the spectroscopic line?
Which Lyman series of hydrogen is invisible part of the spectrum?
>> Balmer series. >> Balmer series, that's right.
And the strongest of those will be the first one, alpha.
So this is H-alpha, as it's called.
There are others of course.
But that's what tends to carry most of the energy in these recombination nebula,
at least invisible part of the spectrum.
And that's what gives them this reddish color.
What about the blue stuff?
You think that's also ionized gas?
>> [INAUDIBLE] >> Well, sometimes a little bit, but
mostly that's just starlight reflected from interstellar dust.
Now you don't think of dust as a mirror or a lot of little dust grains, but
they will reflect some fraction of photons that come upon them.
And the reason why it tends to look blue is that younger stars,
young stars, the most luminous ones are the hottest ones.
And thus, most of the starlight in the vicinity of star-forming
regions tend to be dominated by very blue continuum light so
you see a reflection of it off the dust clouds.
And then there are dust clouds,
which usually appear as shadows on the optical picture, hiding stuff behind them.
But if you were to take a look in infrared,
you would see them shining bright in thermal infrared.
They absorb visible light from starlight, then they get heated up to temperatures
of tens, sometimes couple hundred degrees Kelvin, but usually it's tens.
And, they emit mid to far infrared.
You probably remember Wien's Law,
which connects temperature with the peak wavelength.
So for solar type radiation, temperature of
sun in 6,000 degrees roughly speaking, where does the spectrum peak?
Around which wavelength?
You have eyes that see in the visible part of
the spectrum and so what could it possibly be?
>> [INAUDIBLE] >> Yeah.
>> Well, yeah, very smart.
Not where exactly.
>> [INAUDIBLE] >> Well, kind of in the middle.
It's more like yellowish, like there's about 5,000, 5,500 angstroms.
Okay, so sun is 6,000 degrees, and
lets say interstellar dust cloud is 60 degrees Kelvin.
What would be the peak wavelength of that?
Starting with say 500 nanometers.
Well, I'll let you figure this one out for yourselves, but it would be far-infrared,
maybe even submillimeter regime.
So I've said there are several different components.
Two of them were captured in an epic share of cold and the warm gas.
Cold gas and dust tend to be of these temperatures of some tens of Kelvin,
molecules tend to be well mixed with dust grains, and only small fraction
of all volume, but maybe a lot of mass is contained inside these cold clouds.
They are all exclusively in the thin disc of the Milky Way and
that's where stars are formed.
They're obviously not well ionized because they're cold, and
their primary importance is that this is what stars are made from.
Stars are made exclusively from cold interstellar gas and dust.
Warm is the one that makes pretty pictures, is the ionized gas,
mostly hydrogen, has temperatures of some thousands of degrees,
typically maybe around 10,000 degrees Kelvin.
And a lot of it is ionized, not necessarily all, and
it shines in these nice, recombination lights.
So, that tends to fill most of the volume around clouds of the cold gas.
And then there is a hot component that you didn't see on previous picture because it
doesn't shine much in visible light.
It is a gas that skeeted through may be million degree scaling and
therefore a chance in X-rays.
That gas is filling up the galactic halo.
It's not a dark matter halo.
It's regular matter mixed in, but it's no longer confined to the disc.
Can you guess how did it get there, and why did it get hot?
If it's hot, what does that mean in terms of the kinetic energy?
Low kinetic energy or high kinetic energy?
What's the relationship between kinetic energy and temperature for a gas?
>> [INAUDIBLE] >> Well, that's right.
It's proportion between kinetic energy and temperature.
So if this gas is high temperature, that means those atoms or
ions have received a lot of kinetic energy from somewhere.
And to spare you the agony of having to answer the question,
they got there largely due to supernova explosions,
which obviously impart a lot of kinetic energy into interstellar medium.
At same time, they can heat up the gas.
So because the gas has a lot of kinetic energy, flies high above a galactic disc,
and just like any gravitational system would work.
Okay, so where is the gas?
This is actual picture of the Milky Way from here, and we are in disc and
this is mosaic of near infrared imagery from the Two Micron Sky Survey.
And almost all of the gas is concentrated in this very thin disc, and
then there is this corona which has some of the hot gas,
which really is negligible component by mass, but it's interesting physically.
So in studying interstellar medium, you may recall there
is this hyper-fine structure line of neutral hydrogen
that happens when the spin of electron relative to the proton flips.
And that tends to happen once every 10 million years or
so per hydrogen atom, but there are a lot of hydrogen atoms.
And so it tends to be the dominant radiation from the cold gas.
Now if this hydrogen wasn't cold, if it wasn't the temperature of tens of
degrees Kelvin, sometimes its barely more than microwave background, a few Kelvin.
Do you think that this would be an important find?
Let's say with a gas this makes those nice, shiny nebulae,
also shining 21 centimeter line.
Well, yes, I'm asking the question.
The answer is obviously no, because that gas would be first ionized,
by and large, and second even if it's not,
the energy levels that are populated will be way higher than these.
So all this can happen at many different energy levels.
So the main advantage of observing interstellar hydrogen using this radio
emission line is that radiowaves zip
through the dust clouds as if they didn't exist.
And that way, we can actually see throughout our Milky Way Galaxy, and
same thing, other galaxies.
So we can study parts of the Milky Way that are hidden from view,
invisible light.
That unfortunately does not include protostellar clouds and
protostellar course.
The gas there is, actually,
the emission is dominated by molecular lines, but that's fine.
We can study those as well.
So, this is picture of the Milky Way.
Again, from here, in 21 centimeter line.
You can see that most of it really is concentrated in the Galactic Plane,
but there is hydrogen at high galactic latitudes as well.
Some of it is really near us, and so it's no longer we can see it up,
but other parts of it got there in some interesting fashion.
We can see there are kind of arches, almost bubbles.
Anybody have an idea where do those come from?
>> [INAUDIBLE] >> You
can see something probably kind of spherical up there.
>> [INAUDIBLE] >> Well,
they too must come from supernova explosions, and
the shockwave of a supernova will push the interstellar medium.
Even when it's not ionizing, but you'll still have kinetic energy.
It'll make these shells of hydrogen to just expand for
awhile before they dissolve and fall back.
All right, so it's interesting to look
how different components of interstellar medium correlate among each other.
And the top is side picture of the Milky Way invisible light.
There is obviously big stellar discs in the bulge, but
there are shadows in front and those are the dust clouds.
Now if you look in millimeter wavelengths, the carbon monoxide,
you find out that molecular gas, which you cannot see invisible light one way or
the other, goes more or less exactly where the dust grains are.
So molecular gas clouds and dust clouds tend to be well mixed together.
Also, it turns out that there is a reasonably good
correlation between neutral hydrogen,
atomic cold gas, and dust emission as well.
And the reason for this is, well, just simply gravity.
That you have denser spots,
say giant molecular clouds that would attract hydrogen as well.
And so there will be some correlation broadly speaking, but not a perfect one.
The molecular clouds are colder,
therefore they tend to be more condensed than just generic hydrogen clouds.
But in terms of gravity, doesn't matter.
And one last portrait of the interstellar medium.
This one, Is a large scale picture of most, not entire,
the Galactic Plane as seen in the light of ionized hydrogen, the H-alpha line.
And you can easily see that there are these bubbles that were produced
by supernova explosions and there are some spots it's hotter,
those are the regions where there's some star formation that ionizes the gas.
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