Lecture 4 - Astro Pas Rochester

More documents

Recommendations

Info

Central density and temperature of the Sun Central pressure is a little more than a factor of 100 larger than average pressure. Guess: central density 100 times higher than average? (That’s equivalent to guessing that the internal temperature does not vary much with radius.) ! For the Sun, that’s not bad; the central density turns out to be 110 times the average density, Since ! As we will see later, the average gas-particle mass in the center of the Sun, considering its composition and the fact that the center is completely ionized, is . <strong>Astro</strong>nomy 142 16
Central density and temperature of the Sun (continued) ! But the material is still an ideal gas, so ! We can make a scaling relation out of this as well, to use in extrapolating to stars similar to the Sun but having different masses, sizes and composition: <strong>Astro</strong>nomy 142 17
Page 1 and 2: Today in Astronomy 142: stellar str
Page 3 and 4: Principles of stellar structure (co
Page 5 and 6: These equations can be derived from
Page 7 and 8: Hydrostatic equilibrium Consider a
Page 9 and 10: Another way to derive this, using E
Page 11 and 12: The Sun’s interior, on the averag
Page 13 and 14: Central pressure in a star (continu
Page 15: For the Sun: Central pressure in a
Page 19 and 20: Diffusion of energy to the surface
Page 21 and 22: Opacity and luminosity in stars (co
Page 23 and 24: Diffusive approximations @f(x, t) @
Page 25: Summary ! Using hydrostatic equilib

Lecture 4 - Astro Pas Rochester

Create successful ePaper yourself

Delete template?

Save as template?