Lecture 4 - Astro Pas Rochester

More documents

Recommendations

Info

Hydrostatic equilibrium (continued) If the star is in hydrostatic equilibrium the weight is balanced by the pressure difference across the shell: This differential equation, one of the equations of stellar structure, can be solved easily under certain assumptions. <strong>Astro</strong>nomy 142 8
Another way to derive this, using Euler’s equation Euler’s equation for a fluid We assume time independent so that Assume that the velocities are zero (in equilibrium) Gravitational potential Sub in and get <strong>Astro</strong>nomy 142 9
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: Hydrostatic equilibrium Consider a
Page 11 and 12: The Sun’s interior, on the averag
Page 13 and 14: Central pressure in a star (continu
Page 15 and 16: For the Sun: Central pressure in a
Page 17 and 18: Central density and temperature of
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?