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.
Trends Along the Hubble Sequence and their Origins
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From the course by Caltech
The Evolving Universe
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From the lesson
The World of Galaxies
Meet the Instructors
S. George DjorgovskiProfessor
Astronomy
Let's now take a closer look as to how properties of galaxies change
as a function of their morphology, and where does it come from.
So here is another schematic representation of Hubble sequence with
actual real life example pictures to propose them in, and one thing to notice
about this classification is that it has some drawbacks.
First of all, it's completely subjective.
To some people, the galaxy may look like it's got really promised spiral arms,
and other people maybe not so much.
In any way it's based on which filter you take a picture.
Because if you use bluer filters you see more star formation,
if you're redder you see less.
It's all sort of beauty contest type of assignment.
A much better thing is if you can actually measure some numbers and use that.
As a means of assigning morphology which is now done in modern sky.
It also missed a very important difference between a large galaxy and a small ones.
Morph galaxies, which there's more then one family,
are not just a shrunken version of big galaxies.
They are very different kind of beast.
And there is different physical process that governs their formation.
But if you had eyes in different parts of the electromagnetic spectrum
galaxies would look very different.
And so it sort of quasi-historical-biological
accident that we do it in visible light.
But if we had eyes in sensitive and
far-infrared we will have a completely different kind of classification.
All right, that's the bad news.
The good news is there actually is some meaning to galaxy morphology because that
Is a product of the overall evolution.
And it's useful to think of big galaxies, those in Hubble sequence,
as a combination of two basic components, disks and bulges.
Ellipticals will have no disks, traditionally, and
the ratio bulge to disk, will define where a spiral is.
And then again this does not take into account invisible stuff,
dark matter, which totally dominates masses in dynamics of galaxies.
But it's very hard to classify morphology with invisible materials so
we stick with normal light.
So if you look for properties as they go from ellipticals, and
I smoosh all ellipticals into one group because, turns out the doesn't matter, and
then go along the spiral sequence.
And again, doesn't matter if they have bars or
not, a number of interesting things change.
Not just the way stars look, but the dynamics of it.
Ellipticals are supported entirely by random motions of stars
in their gravitational potential.
Spirals have most of their kinetic energy in orderly rotation of the disk.
90 odd percent, and
there is a dynamical change that corresponds to also gradual change in your
stellar populations, from no star formation to lot of star formation.
Therefore, from red colors of old stars like red giants,
to blue colors of blue ultraluminous of giants, and so on.
So somehow actual affirmative processes of galaxies know about all this
they correlate together stellar populations with the dynamics,
and that is what really poses the question, where does this come from?
And again, I'll note even though many things do correlate
with morphological types, many others don't.
For example, if I tell you what's Hubble type of some galaxy,
you have no idea of what luminosity it has, or what mass, or size.
And those are pretty important properties too.
So it is now generally agreed that as far as these
observed properties are concerned,
it can be all understood in terms of the different star formation histories.
Whereby ellipticals, or early types,
form most of their stars early on, whereas spirals continued at a more or
less uniform pace throughout the age of the universe.
And interestingly enough, if you add up all hydrogen that you see in spiral
galaxies, add up all star formation, and ask how much longer do they have to go?
How much more fuel do we have for making stars?
The answer is usually of the order of billion years.
So either we live in a very special time of the universe,
just before spirals run out of gas, or they somehow get the resupply of
hydrogen to build stars, and that's probably what's happening.
There is intergalactic hydrogen that is being created to the galaxies and
then serves as an additional fuel for star formation.
So this is sort of a cartoon version of what the difference might be, that for
elliptical galaxies, or bulges, you do a lot of early star formation.
You do it in place.
So you recycle all the supernova products to make next generation star and next.
And within billion years you might have already hundred generations of stars.
This is why these are all metal-rich stellar population, not all metal-poor.
Whereas to good approximation most these galaxies are more or
less constant in their star formation history through the universe.
So that's as far as stars are concerned, but
how do you connect this with dynamics of galaxies?
Well, here is the basic idea.
It all depends on when do you make stars versus when do
you assemble stuff, gas, into the bigger galaxy.
And if you make stars in small protogalactic pieces like dwarf galaxies,
and then merge them.
Those stars are mass points.
They conserve energy, momentum, angular momentum.
There's some other combinations of things.
And if there is no dissipation, they will just remain in that motion forever.
So they will respond to the global gravitational potential of the newly made
galaxy, but their motions will be random because they came from any odd direction.
So this is why you would have elliptical galaxies that are kinematically supported
by random motions, pressure of the stellar gas if you want, not by rotation.
Now on the other hand, if you first put the gas together,
it collapses, retains angular momentum,
settles into a disk because it doesn't know what to do with angular momentum.
Then you make stars.
Then those stars will remember that they were formed in a thin, cold,
rotating disk.
And that's exactly what happens.
So the sequence of formative events, mergers, and star formation, and
accretion of gas,
is what determines whether a galaxy will be mostly elliptical, or mostly disc.
And that accounts for a lot of these observed properties.
One other important thing is well, you make stars.
Big stars explode.
They release newly formed chemical elements.
What happens with that stuff?
Well, if you have a really massive galaxy.
The potential well is deep, the super nova shell might expand,
but then turn around and fall back.
Mix with the rest of the interstellar material used to make new stars.
On the other hand, if you have a dwarf galaxy, a supernova may put so much
kinetic energy in its expanding shell, that that material just leaves the galaxy.
And so the galaxy itself does not evolve chemically very much.
You expect then dwarfs will be more metal core, and in fact, they really are.
So this mechanism actually can explain a lot of their other properties.
By removal of the Baryonic material, there is less stuff left to make stars.
So in the end, you will end up with very low star density systems, not many stars
there, relative to the dark matter that is not affected by supernova shocks at all.
And because you're removing mass
altogether the thing will expand slowly, and assume even lower density.
So this combination of supernova
enrichment of the interstellar medium and kinetic energy actually can explain a lot
in terms of differences between big and small galaxies.
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