Astronomy 162:
Introduction to Stellar, Galactic, & Extragalactic Astronomy

Lecture 13: Energy Generation in Stars


Key Ideas:


Putting Stars Together

Physics needed to describe stars:

Hydrostatic Equilibrium

Balance between Pressure & Gravity.

Sets up a Core-Envelope Structure:


Energy Generation

Stars shine because they are hot.

To stay hot stars must make up for the energy lost by shining.

Energy sources available:


Main-Sequence Stars

Generate energy by fusion of 4 1H into 1 4He.

There are two nuclear reaction paths by which a star might accomplish this fusion:

Proton-Proton Chain:

CNO Cycle:


Proton-Proton Chain:

Note that you use 6 protons in all, and end up with 1 4He nucleus and 2 protons at the end, for a net conversion of 4 protons into 1 Helium, with the release of energy as gamma-ray photons, neutrinos, and postirons.


CNO Cycle:

Note that you start with one 12C nucleus in step one, and add 4 protons during steps 1, 3, 4, and 6, ending up with the 12C nucleus back at the end with the 4He nucleus.

The result is a net conversion of 4 protons into 1 Helium nucleus, with a release of energy in the form of gamma-ray photons, neutrinos, and positrons.

Because 12C is not consumed by this process (it goes in & comes out at the end), we say that it acts as a catalyst for the nuclear reaction.

Because Carbon and Nitrogen have 6 and 7 protons, respectively, in order to overcome the repulsion of all these positive charges the protons must be moving fairly fast. This is why the CNO cycle occurs at higher temperatures than the P-P chain.


Controlled Nuclear Fusion

Fusion reactions are Temperature sensitive:

BUT,

So why doesn't it runaway and blow up like a Hydrogen Bomb?


Hydrostatic Thermostat

If fusion reactions run too fast:

If fusion reactions run too slow:


Summary:

Energy generation in stars: