Draw atomic nuclei

Look at the nuclei.

You add the droplet to the system.

You have on your left an olive oil droplet, and this olive oil droplet gets attacked by enzymes.

Nuclei and nuclear reactions, of course.

And we call them active galactic nuclei.

Connection between life and radioactive nuclei is straightforward.

The Big Bang nucleosynthesis predicts abundances of light nuclei.

These two nuclei, when they're far apart, are charged.

You have fissile nuclei. That means this is a nucleus.

For this fish, it's actually whole cells with nuclei and membranes.

Stars are fueled by how the nuclei in those atoms react together.

Now let's go and grab all of the nuclei from a typical car.

The strong force, the strong nuclear force, which sticks nuclei together, gets weaker.

For example, here is a lovely yellow droplet of milk on the left, there is nothing on the right.

Those are the active galactic nuclei, which we will discuss in more detail later in class.

There's too many condensation nuclei, so the water droplets do not combine and fall as rain.

Because that is the way to suppress the energetic phenomena that we see in active galactic nuclei.

Obviously, the heavier nuclei have higher charges and there is a higher Coulomb barrier to be overcome.

What we do is we accelerate protons so, hydrogen nuclei around 99.999999 percent the speed of light.

The super massive black hole paradigm for active galactic nuclei quasars and such is now very well established.

The different bands correspond to abundances of different nuclei at the end as a function of the baryon density.

One is the super massive black holes and their nuclei and the other one is the dwarf family of galaxies.

The covalent radius in chemistry corresponds to half of the distance between two identical atomic nuclei, bound by a covalent bond.

But small atoms want to join together, small nuclei want to join together to make bigger ones to go towards iron.

The nuclei in the cell on the left is in the animal, the one on the right is in a dish.

Charged particles don't want to get near each other. Bare nuclei are both charged, positive charged, they want to avoid each other.

So before they can be combined with protons into helium or other like nuclei, the decay destroys about 24, 25 of them.

Oil droplet forms through self assembly, has a chemical metabolism inside so it can use energy, and it uses that energy to move itself around in its environment.

By the time temperature drops to a billion degrees, neutrons and protons can combine to form nuclei of helium according to these reactions.

And then we took the dead nucleus from the dead tissue of the extinct frog and we inserted those nuclei into that egg.

The quarks, these pink things, are the things that make up protons and neutrons that make up the atomic nuclei in your body.

At this point, the neutron to proton ratio has dropped to 0.14 and these neutrons end up in the like nuclei that they're produced.

How many cars' nuclei would you have to put into the box to have your one foot box have the same density of the nucleus?

What we see are, first of all, a very active culture, a lot of divisions, and then very clear nuclei once the cells have separated.

In this protocell model, it's just an oil droplet, but a chemical metabolism inside that allows this protocell to use energy to do something, to actually become dynamic, as we'll see here.

The frame and radii of this web is made up of one type of silk, while the capture spiral is a composite of two different silks the filament and the sticky droplet.

But this symmetry has to be broken, electrons are lighter than muons, the top quark is much much heavier than the quarks that make up everyday nuclei.

A few seconds after the Big Bang, it was hotter still, hot enough to overpower the forces that usually hold protons and neutrons together in atomic nuclei.

So in this way, the intrinsic mass difference between protons and neutrons, something that comes out of particle physics, determines the abundances of light nuclei created in the

That the reason the reactions don't proceed beyond lithium or beryilium, beryilium or so is the universe expands and becomes insufficiently hot and dense to create heavier nuclei.

In 1940's Carl Seyfert wrote his PhD thesis, observed bright nuclei nearby spiral galaxies and found to have these somewhat unusual spectra with very broad emission lines.

Today, things are largely made up of atoms, but hundreds of seconds after the Big Bang, it was too hot for electrons to join atomic nuclei to make atoms.

Basically in the X ray sky, you see point sources which would be active nuclei or maybe stars of some sort and extended sources which are clusters of galaxies.

Some of those newly made nuclei of helium are then dissociated by residual photons, but as the universe expands, they cool it off and so no more association can occur.