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.
Galaxy Interactions and Mergers
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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 talk about one of the most important formation processes for
galaxies, which is merging.
And these are pictures from Hubble Space Telescope of different galaxy pairs and
different stages of merging.
Mergers take a couple of billion years to accomplish, and so what we can do is find
them in different stages, and if we can assemble them in a correct
temporal order, that gives us the movie of how galaxies would merge.
So on the basis of different models, this is sort of order to help people think it.
Two spirals, they don't know much about each other.
They get closer to each other.
They distort each other with their own neutral gravity making these title tales
and bridges, orbit for a while, and smush together and
make just one amorphous galaxy that incidentally settles into an elliptical.
Few percent of galaxies today are involved in some sort of strong interaction
like this.
And that was certainly much more the case in the past.
Because, first of all, they were closer together,
the universe expands, and there were more galaxies around.
Since then some have merged in.
Now in the early days, people did not know what to make of this.
So these things look like nothing else on Hubble sequence, so
they were called peculiar galaxies.
And now we know that there's nothing peculiar with them.
They just happen to be caught in the act of merging with another galaxy somewhere.
And there are a number of famous examples.
This one is called antennae.
And the superpose the knot is imaging from Hubble Space Telescope.
There's a great deal of star formation going on in the mergers of galaxies.
And the same process must have happened in the early days,
when galaxies were first assembled.
Here is a Rogues Gallery of a number of different types of galaxy mergers and
we're pretty sure that's what's going on as we can
recover some of these by dynamical modeling.
And notice that there is always, in the early stages at least,
there is this strange distortion going on.
Not spiral arms, but more like a long,
long tails of stars that have been kicked out.
And, this is an intriguing thing because if you think in terms of Kepler's law,
Newton's gravity, clockwork, planets go around suns, point masses.
But if you now have couple 100 billion mass points interacting together,
suddenly gravity turns out to be much more interesting.
It creates these collective effects of tails and what have you,
which you just couldn't possibly predict just knowing Newton's gravity law.
And that's all there is going here, just normal values.
So sometimes you see an elliptical galaxy that has dust in it like this, this is
the biggest galaxy in the Fornax cluster, and that's just remains of its last meal.
It gobbled up this galaxy, and some of the dust clouds are still remaining.
Eventually, those will dissipate.
But Hubble actually noticed some of the dust lines and didn't know what to do with
them, kind of ignored them, and now we know that this is a normal part
of a life of a big galaxy, that it'll be just consuming its neighbors.
Now, why do galaxies merge?
And that is due to the process called dynamical friction.
You are familiar with the regular friction that really comes from
atomic forces of materials, two objects rub against each other.
This is different, but it works like viscosity works, but for
different reasons.
So imagine there is a large mass, say a galaxy,
that's moving through a big sea of stars, say going through another galaxy.
It will be attracting those stars towards itself, and then it moves on, and
those things are still kinda piling up behind it, in a kinda wake wave.
And if it expands some of the kinetic energy
in accelerating those stars stores itself.
So, in that way, the bulk kinetic energy of a galaxy or
two galaxies gets to be translated into the internal degrees of freedom.
The kinetic energy has been repackaged to be more within the galaxies themselves.
And because of that, if you have two galaxies approaching each other and
they're on parabolic orbit there is not very gravitationally bound, maybe even
slightly hyperbolic orbit, they will lose enough energy that they'll actually become
gravitationally bound, and that will keep going on until they spiral and merge.
So simulations of this have been done for many years now and this is for
example what stars might do in a merger of two spirals.
So first there is this dance of lows spectacular splatter of stars around.
Eventually, it settles into something like elliptical galaxy where now most of
the kinetic energy's in random motions, that's the kinetic energy that's being
soaked up from the orbital kinetic energy, the two progenitors.
An interesting thing happens when you compare gas to stars.
Turns out, that the gas loses energy much faster.
Stars are mass points, they just get rearranged, but
gas can actually dissipate energy and because of that,
it settles to the middle of the merger product sometimes in a very dense way.
What that will do is it will ignite burst of star formation or
there's a big black hole, it will feed it and provide fuel for emission.
And so now we have plenty of examples that show that galaxies that seem
to be recent mergers or mergers in progress do tend to have very luminous
bursts of star formation in their middle and/or also active nuclei.
So this dynamical of the evolution process then explains a number of other observed
facts which have to do with star formation as well as with presence of active nuclei.
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