Lecture 4 - Astro Pas Rochester

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Some dimensional analysis Pressure P Force/area g cm s -2 cm -2 Energy/volume g cm 2 s -2 cm -3 = g s -2 cm -1 Combine M G R to make a pressure unit GM/R cm 2 s -2 velocity has s -2 GM 2 /R 4 g cm -1 s -2 expected scaling for P <strong>Astro</strong>nomy 142 10
The Sun’s interior, on the average Since we know its distance (from radar), mass (from Earth’s orbital period) and radius (from angular size and known distance): we know the average mass density (mass per unit volume): <strong>Astro</strong>nomy 142 11
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: Another way to derive this, using E
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

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