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3. (10 points) The most luminous/hottest stars are supported not by ideal-gas pressure but by radiation pressure - the interaction of photons with the atoms in the star provides the main pressure force, rather than the atom/atom collisions in an ideal gas. For blackbody radiation, radiation pressure obeys the equation of state: $P_{rad} = \frac{1}{3}aT^4 = \frac{1}{3}u$ where $u$ is the thermal energy density carried by the photons (see Maoz ch 3.6). Repeat the derivation of the virial relationships between $E_{gr}$, $E_{th}$, and $E_{total}$ for a star supported by radiation pressure (you can ignore the contribution of gas pressure for this calculation).

          3. (10 points) The most luminous/hottest stars are supported not by ideal-gas pressure but by radiation pressure - the interaction of photons with the atoms in the star provides the main pressure force, rather than the atom/atom collisions in an ideal gas. For blackbody radiation, radiation pressure obeys the equation of state:
$P_{rad} = \frac{1}{3}aT^4 = \frac{1}{3}u$
where $u$ is the thermal energy density carried by the photons (see Maoz ch 3.6). Repeat the derivation of the virial relationships between $E_{gr}$, $E_{th}$, and $E_{total}$ for a star supported by radiation pressure (you can ignore the contribution of gas pressure for this calculation).

3. (10 points) The most luminous/hottest stars are supported not by ideal-gas pressure but by radiation pressure - the interaction of photons with the atoms in the star provides the main pressure force, rather than the atom/atom collisions in an ideal gas. For blackbody radiation, radiation pressure obeys the equation of state:
Prad = (1)/(3)aT^4 = (1)/(3)u
where u is the thermal energy density carried by the photons (see Maoz ch 3.6). Repeat the derivation of the virial relationships between Egr, Eth, and Etotal for a star supported by radiation pressure (you can ignore the contribution of gas pressure for this calculation).

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