Instructor notes: EOS Lab: Pressure Support in Stars

What this demo is for, how long it takes, and what misconception it targets.

• Stellar pressure support is only thermal gas pressure.
• Radiation pressure always follows aT^4/3 without assumption checks.

Suggested flow (edit as needed):

1. Students write a prediction before touching controls.
2. Students run the play steps in pairs and record evidence.
3. Whole-class debrief: claim + evidence, then model limitations.

• 1–2 sentence explanation aligned to the “Explain” prompt.
• One claim + one piece of evidence from the demo.

• Gas pressure uses P_gas = rho k_B T/(mu m_u) with fully ionized mixture approximations for mu and mu_e.
• Radiation pressure uses an LTE-like closure with explicit caution framing for low-density/high-temperature cases.
• Finite-temperature electron pressure uses Fermi-Dirac EOS (nonrelativistic branch first, relativistic branch at larger x_F).
• Displayed degeneracy channel is P_deg,e = max(P_e,FD - n_e k_B T, 0), so classical electron pressure is not double-counted.

• Add a proper instructor content collection for richer notes.
• Improve station card parameter table to be demo-driven.
• Add export-results scaffolding once runtime lands.