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.

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From the course by Caltech

The Evolving Universe

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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.

From the lesson

Introduction and Some Basics

- S. George DjorgovskiProfessor

Astronomy

Let's now talk about what was essentially first scientific thing in astronomy and

Â where does it come from, which is Kepler's Laws.

Â The strange contraption on the left here is Kepler's model of

Â nested Platonic solids.

Â Who knows what are Platonic solids?

Â These are volumes that can be composed out of equilateral

Â polygons and tetrahedron and cube and so on.

Â And so when Kepler figure out using Tycho Brahe's data,

Â how far are the planets relative to the sun?

Â He also sorted out that if you can take combinations of these platonic solids

Â sitting inside the spheres and

Â put spheres inside of them, you can find a combination that kinda

Â approximates the actual relatives sizes of orbits of planets in solar system.

Â Which is totally mystical and complete nonsense actually,

Â but Kepler was a mystic.

Â And an alchemist, and also court astrologer.

Â And this was perfectly normal thing to be that.

Â Isaac Newton spent most of his life doing alchemy.

Â He did this whole stuff that he's famous for a few years, he was a young guy,

Â and then later on he was just messing with alchemy, and

Â then he was master of mint, and stuff like that.

Â Anyway, back to Kepler.

Â So Tycho Brahe's data were best at the time.

Â But, even so, we're talking about positions of planets seen in the sky,

Â they move around.

Â And so things are all rotating.

Â The Earth's rotating, going around the sun.

Â Planets are going a different speed than the sun.

Â So it gets to be pretty messy, and yet from that set of data,

Â Kepler managed to deduce these three laws.

Â First that the orbits are elliptical and the sun is at the center.

Â So this was like, first real proof of the Copernican system.

Â You can say Galileo pretty much demonstrated, but

Â this was a good thing to add.

Â And it's the ellipses and not collections of epicycles,

Â circles rolling on other circles.

Â The Sun sits in focus of those.

Â Then something that's truly amazing that he can figure out is that

Â Radius vector, from Sun to the planet, rotates around,

Â and it doesn't rotate with the same angular speed,

Â it rotates faster when the planet's closer and slower when the planet is further out.

Â But in such a way that the distance and speed together match and

Â the area of the little triangle swept by this radius per unit time is the same.

Â This is a completely unnatural thing if you start from nothing, and it's correct.

Â It's just amazing that he figured this one out.

Â He also found this proportion,

Â that the squares of periods are proportional to the cubes of orbits.

Â So this was empirical data.

Â There was no theoretical understanding.

Â He had Copernican system as a geometrical framework if you will.

Â But nobody knew why this is.

Â Kepler did this just like a few years after Galileo's initial discoveries.

Â They're pretty much contemporaries.

Â So it's the early 17th century when science really started.

Â Now all these are explained by Newton who is justly famous, and there he is.

Â Then in 1676 or something like that.

Â Let's see, the Greek number is 1687.

Â Sorry.

Â Drawing a blank.

Â He published the famous book, The Mathematical Principals of

Â Natural Philosophy, where he put forward his four laws,

Â the three famous ones and the fourth law of gravity, which for

Â some reason never gets numbered, as well as calculus.

Â He was pushed into this by the news that Leibnitz,

Â who apparently independently discovered calculus, was about to publish his ideas,

Â and some of the ideas of Newton's may had been actually put forward by others,

Â by Hook for example.

Â Anyway you know the three Newton's Laws.

Â The law of inertia, and then orce is defined as product of mass and

Â acceleration, and action equals reaction.

Â Now the first two can be actually related to what's then

Â became really understood in 19th century the conservation laws of energy,

Â linear momentum, and angular momentum.

Â And we'll make heavy use of those.

Â Now as far as the third one that you have much of the forces,

Â if you have, say, a mass moving in a gravitational field off another mass,

Â then its centrifugal force is mass times velocity squared divided by the radius.

Â And that has to be matched by the gravitational force, which is the unnamed

Â fourth Newton's law of gravity, an amazing achievement in of itself.

Â And that is something we will be using very heavily as well.

Â The law of gravity there is this legend about apple falling from tree on

Â Newton's head and then figuring out it's same as moon going around the earth.

Â That's probably just urban legend from 17th century.

Â But, one way or the other he was able to connect simple

Â observations right here on planet Earth and motion of the moon and

Â so on and deduce what looks like a pretty natural formula.

Â If you think there is some kind of attraction force and

Â acts between different masses, well it's kinda reasonable be proportional to each

Â of the masses and some sense that it's effect will be diluted as a square

Â of the radius because of the surface of the sphere in which it elites, okay?

Â So it's a reasonable guess for a formula and it turns out to be correct.

Â There is a constant they can measure, front, and

Â this worked fine, they even, well it was superseded by theory of Relativity,

Â but for the most part we can use Newton's gravity for just about anything.

Â And the conservation of energy is the that the total energy's combination of two

Â parts, kinetic and potential, for minus sign for

Â a potential energy, and for gravitational field, it's proportional to the masses,

Â and proportional to the radius.

Â And the last quantity is angular momentum, which for a point mass

Â going in rotation around some center for whatever reason,

Â say gravity, is proportionate to mass, velocity, and radius.

Â And if you have solid body, you integrate over all mass points and you get that.

Â All right, keep this in mind.

Â So Newton, as a part of Principia, figured out that if you have two mass points,

Â moving under influence of each other's gravity,

Â their orbits, let's call them orbits, whether or

Â not they actually stay together, are always conic sections.

Â Conic sections are curves you get when you take a plane and

Â slice a cone If you do it obliquely, you'll get an ellipse.

Â Circle is a special case of an ellipse.

Â If you do it parallel to the angle of the cone, you'll get the parabola,

Â and if you do it vertical along the cone's axis, you get the hyperbola.

Â There is some tedious proof of this using polar coordinates.

Â But the important point was that

Â this major shape of the orbit is directly related to the total energy of the system.

Â If the two mass points are such that potential energy overcomes the kinetic

Â energy, they are bound, they just have to go around each other, so

Â the orbits are ellipses.

Â If the net energy is positive, there is more kinetic than potential,

Â they'll fly apart according to a hyperbola.

Â And the boundary condition between the two wings exactly kinetic equal potential,

Â it's a parabola.

Â So you can think of parabola as an ellipse with an infinitely long semi major axis.

Â Okay, so he immediately explained Kepler's first law,

Â which up until then was very mysterious, why ellipses and not something else.

Â Well, you can find in books, tedious derivation in polar coordinates,

Â there is as well all manner of angles which you'll never need in your life,

Â but here is a very simple intuitive way to think about it, right.

Â So as, say a planet goes around the Sun in ellipse, you can decompose its

Â velocity into radial component and a tangential component, right.

Â And so the motion will be sum of the two.

Â Now think of a simple harmonic oscillator like pendulum.

Â Probably know that the period of the pendulum would not depend

Â on the amplitude, it only depends on the length.

Â So if you give it initial momentum in two different directions,

Â the pendulum is not going to go according to just a slice of a circle,

Â it's going to make a little ellipse, right?

Â So exactly same thing happens here.

Â In some sense, you can think of it as a planet going around the sun and

Â also going in and out, in and out.

Â And it has to be exact same period because we're talking about same system, and so

Â that kind of gives you an ellipse.

Â Now this is not exactly right analogy, but

Â it kinda gives good intuitive idea where it comes from, okay.

Â Well, all right, so we have orbits.

Â We'll just talk about closed orbits, those that keep things together.

Â And there size will depend on the energy.

Â If a planet, let's say the planets and Sun can go through each other for

Â simplicity sake, right.

Â Physicists love to make this kind of assumptions,

Â like the famous case of spherically symmetric homogeneous chicken, all right.

Â And say there is a center of attraction mass one.

Â There is mass two.

Â Mass two has no kinetic energy whatsoever.

Â It just sits there in the middle because that's the center of attraction.

Â Now, if you give it some energy it's going to move away.

Â How far will we go?

Â It depends on the amount of kinetic energy you have.

Â If you throw a rock up,

Â the height is going to depend on how much energy you give it.

Â Well, same thing applies here.

Â So the higher the net energy of planet or

Â system, Sun and planet, the larger orbit you're going to get.

Â And when the kinetic energy is equal to the potential one, the flat part, bye bye.

Â The planet goes in parabolic orbit, or a hyperbolic, axis kinetic energy.

Â Okay, so the size of the orbit in some sense depends on the edge.

Â The shape of a closed orbit turns out depends on angular momentum.

Â So there is a fixed amount of energy whatever it is and

Â that defined the semi-major axis or radius of the Earth.

Â Now, the minimum angular momentum you can have is zero.

Â So the planet can just turn out and come back,

Â on a linear trajectory, which is maximum, so that's infinitely thin ellipse.

Â So that's the zero angular momentum.

Â Pure radial orbit.

Â The other extreme is pure circular orbit.

Â And for a circular orbit,

Â there is a maximum value that angular momentum can have,

Â because, you remember, kinetic energy is mv squared over 2.

Â And angular momentum is mv divided by r.

Â R was given because of total energy, so because there is, the energy's conserved,

Â sorry, energy's fixed, angular momentum has to be fixed too.

Â And so there is certain critical amount of angular momentum.

Â Planet can not go on an orbit that's more circular than circular, right.

Â It can only have less angular momentum than that.

Â If it is none, it's in a linear orbit.

Â If it has the maximum, it's in circular orbit.

Â And orbits of planets in the solar system,

Â our solar system at least, are pretty close to circular.

Â This ellipse business is very subtle actually.

Â And the reason for this, the reason why there are circular orbits

Â in disks in astrophysics and all different kinds of phenomena.

Â Planetary systems, accretion disc for quasars, and so on and so

Â forth, is that many of these systems are made by dissipating edge.

Â It can radiate energy away and so on, but you cannot radiate angular momentum.

Â There are no photons of angular momentum.

Â And so, things like planet, or comets, or what have you,

Â settle along the orbit that has the lowest possible energy for

Â the amount of angular momentum they got, which is a circle.

Â And so, this is why their disc galaxies and planetary systems in accretion discs.

Â Okay, so that's as far as the Kepler's first law, what about the second one?

Â So, this turns out to be a beautiful little derivation, right.

Â So, there is angular momentum and here assuming the Sun is much

Â heavier than planets or the Sun doesn't centralize and so the angular momentum

Â is mass of a planet times velocity times the radius at any given time.

Â So, in case of elliptical orbit radius changes.

Â So, because mass is fixed, product of velocity and radius is fixed.

Â This also known as the adiabatic invariant.

Â Now if you look at the tiny little angle, element of angle,

Â that's what per unit time, all right.

Â It's the length of the arch is

Â proportional to the velocity of a given element of time.

Â And so we multiply that by the radius and divided by two, you have the area.

Â And therefore, the product is independent of mass.

Â And so therefore,

Â the Kepler's second law, that planets moving elliptical orbits in stride

Â elements of equal area per unit time, moving slower into the third airway.

Â Obviously gonna move slower and further away because distance is larger,

Â gravitational pull is smaller, therefore centrifugal force has to be smaller,

Â velocity has to be smaller.

Â This is a Simple and direct consequence of the consideration of angular momentum.

Â Kepler had no idea about thing called angular momentum,

Â he just empirically found this is the case.

Â What about the third one?

Â Well, we can know that too.

Â So the centripetal force is given by the law of gravity

Â adding up semi major axis of the planet and the sun.

Â They're actually both moving around common center of the mass which is so

Â close to the center of the sun that it doesn't really matter, so

Â you can just use the semi major axis of the planetary orbit, okay?

Â Now, centrifugal force is given by a product of mass,

Â square of velocity, divided by the second major axis.

Â And velocity is circumference of the orbit divided by the period.

Â So this is how I transform.

Â Centrifugal force is proportional to mass.

Â Semimajor axis and inverse loop proportional to square root period, right?

Â Make them equal, and what?

Â You get the 4 pi squared cube of the semi major axis is equal,

Â G mass to the sun, because mass of the planet cancels,

Â times period square, and so that's exactly Kepler's third law.

Â So it's a simple consequence of conservation of energy.

Â You can go about this in different ways, like you can do an energy way

Â as opposed to the centrifugal centripetal force, but you still get the same result.

Â Now this actually tends to carry on in many other situations,

Â including even pulsating stars.

Â So that's how Newtonian physics, simple mechanics, and

Â Newtonian gravity explained motion in inside solar system.

Â Well, all right.

Â It actually things are a little more complicated because it's

Â not a whole bunch of two bodies, it's those many planets and other stuff.

Â And turns out, that there are no analytical

Â solutions for gravitational motion when there's more than two bodies.

Â The two body problems solve half a page, add third mass point,

Â there is no analytical solution in closed form.

Â Poincare has proven this in 19th century and it still holds, but

Â since masses of planets are pretty small relative to the mass of the Sun,

Â you can use gravitational pull of the other planets just as a small

Â perturbation on the orbit that's governed by the big mass, the Sun.

Â And there is whole theory called perturbation theory that you can

Â integrate as far as you want in different number of terms and

Â get approximations which can be very close.

Â I think, actually, this is not so difficult to do,

Â and this is how Neptune was discovered.

Â The two astronomers, Adams and Leverrier, looked at

Â orbit of Uranus, which was discovered empirically by Herschel, and found out

Â that Uranus is not moving exactly as you'd expect, according to Kepler's laws.

Â But if there was another massive planet behind, then its gravitational

Â pull could explain variations in the orbit of Uranus.

Â And then computing this backward,

Â they figured out where this new planet should be.

Â And an astronomer named Galilei as founded, and

Â so this was a fantastic prediction of Newtonian mechanics.

Â The new planet was discovered as a direct prediction of simple Newtonian.

Â More recently, also we see things like impacts of comets on Jupiter, or Earth for

Â that matter.

Â Jupiter is the only other mass in solar system that really matters when it

Â comes to these things, and can deflect orbits of comets and asteroids.

Â We've now seen at least three different cases of a comet being redirected from

Â its unperturbed orbit and making an impact into Jupiter, and

Â so when that happens on planet Earth, bad things happen depending on the size of it.

Â So this how astronomy can actually kill you.

Â It's one of the few ways.

Â Now it can also measure things really precisely.

Â It can find out that there are effects cannot be explained through Newtonian

Â gravity no matter how good perturbation theory is, and

Â those are due to the theory of relativity which

Â is a better approximation of physical reality than the Newton's physics was.

Â And in fact, this was the first significant evidence for

Â the theory of relativity is correct.

Â But for many years, until early 20th century, astronomers found out that

Â orbit of Mercury doesn't stay the same, that the ellipse itself rotates.

Â That's called the advance of the perihelion.

Â And there was no way to explain why this is the case, but Einstein explained it and

Â predicted it, and it was first reason why people started paying attention.

Â Things actually can get interesting in just good old Newtonian mechanics.

Â Now there are different systems, like Saturn's rings, that consist of gazillions

Â of particles orbiting the planet, and they form the rings,

Â and rings are not solid, there a whole bunch of little, thin ringlets.

Â And the gaps between them are all governed by the gravitational pull

Â of Saturn's satellites.

Â So you have a very complex multi body dynamics that produces this sort of LP

Â record look of Saturn's rings, and

Â astrophysicists including Peter have explained why this happens.

Â An even more interesting question is so called dynamical chaos.

Â Now, we tend to kind of indoctrinate you how once you know all these laws and

Â initial conditions, you can compute everything to infinite future.

Â And Laplace in the 19th century even invented a thing called the Laplace demon,

Â Which is a hypothetical, theoretical physicist who knows positions,

Â and masses, and velocities of every single mass in the universe, and

Â therefore can compute exactly what's going to happen to infinite future.

Â Turns out that's not the case.

Â That in mechanical systems,

Â you can have genuine chaotic motions past certain threshold of complexity,

Â and the solar system, which looked like a nice little

Â clockwork mechanism, according to Kepler's laws, Newton's laws.

Â It only looks that way now, but if you integrate through billions of years,

Â some of the members of the solar system may not actually stay with us.

Â These perturbations keep jiggering them, and sooner or

Â later it can kick a planet out.

Â This probably happens to comets and asteroids quite a bit.

Â So solar system need not be stable in long term, and

Â that actually is not too much of a problem for our solar system, pretty stable.

Â But now that we have planetary systems around other stars,

Â some of those are definitely not stable.

Â And so there is some interesting

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