The power plant of the Sun and stars. Nuclear Reactions in Stellar Interiors H + H 2 H + e + + nu H + 2 H 3 He + gamma 3 He + 3 He 4 He + H + H Net effect:

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Presentation transcript:

The power plant of the Sun and stars

Nuclear Reactions in Stellar Interiors H + H 2 H + e + + nu H + 2 H 3 He + gamma 3 He + 3 He 4 He + H + H Net effect: 4H 4 He Question: why does this occur exclusively in the core of a star? Demo

A small mass difference between Hydrogen and Helium 4 Hydrogen atoms: 6.693E-27 kg 1 Helium atom: 6.645E-27 kg Difference = 0.048E-27 kg Difference = 0.7 percent Why is this small difference important?

The Einstein Energy-Mass equivalence relation E=mc 2 c=speed of light You get a lot of bang for the buck: 6.3E+14 J/kg. This gives plenty of energy to power the Sun for 4.5 billion years plus

The Power Source of Main Sequence Stars MS stars fuse hydrogen into helium, releasing prodigious amounts of energy in the process. Their fuel source is the matter of which they are made

The Structure of Main Sequence Stars The Powerhouse

How can we tell if this is right? Detect neutrinos emitted from the center of the Sun.

The Neutrino Sun: A View into the Solar Interior

Nuclear reactions explain a lot about the Sun, but what is going on on the rest of the Main Sequence?

The fuel for a main sequence star is its own mass in the form of hydrogen. The total amount of fuel is proportional to the total mass of the star. What are the masses of stars?

How We Determine Masses of Stars Method:observation of binary stars (double stars)

Binary stars are numerous (e.g. Sirius )

We can see orbital motion of Sirius B around Sirius A

Masses of stars determine the gravitational force, and thus the acceleration of the stars

Binary Stars (Chapter 21 of book)

The Types of Binary Stars Visual Binaries Eclipsing Binaries Spectroscopic Binaries

Visual binaries…you can see them as two stars in a telescope Alpha Geminorum: Castor Like Albireo, Sirius, Nu Draconis

With visual binaries, if you know the distance, you know the orbital speed and orbital radius (actually the semi-major axis) Bright double stars…find them on your SC1 Chart and look at them in a telescope StarSeparation (arcseconds) Period (years) Alpha Herculis Epsilon Lyrae Beta Cygni34.5? Gamma Andromedae 9.6?

Visual binaries have wide separations and very long periods

Second class of binary…eclipsing binaries One star in a binary comes in front of The other and blocks its light

The classic example of an eclipsing binary…Algol, Beta Persei Period of Algol= Days; orbital Period much Shorter and Precisely known

Upcoming minima of Algol (Beta Persei) October 1, 0:39 AM October 3, 9:28 PM October 6, 6:17 PM Also check eclipsing binary Beta Lyrae, P= days

The final class of binary stars: spectroscopic binaries Basic physical process: the Doppler effect demo

Spectroscopic binaries (3rd class of binaries); known to be binaries only because of periodic variations in the spectrum

From periodic wobbling back and forth of the spectral lines of a (blended) binary, we can often determine the radius of the orbit, and orbital speeds, and thus the masses of the stars From observations of binaries, we have the masses Of a sample of stars, and can study how stellar Properties depend on mass.

The masses of stars (and their luminosities) Main Sequence stars