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In this lecture we obtain the energy and momentum conservation equations for the radiation field. Starting from those, we discuss radiative equilibrium and flux (or luminosity) constancy, optically thin radiative cooling, radiation force, and the vacuum wave equation limit. Relevant examples: Simplest way to justify Eddington-Barbier limb darkening (L5b). Temperature structure in atmospheres of stars and accretion discs. Radiative cooling in galaxy formation and solar corona. Force and Eddington limit of stars (more later in course). Radiation equilibrium 'sound speed' c/sqrt(3). Course: Radiation Processes in Astronomy Lecturer: Prof. Jon Sundqvist Programme: KU Leuven Bachelor Physics & Master Astronomy & Astrophysics #astrophysics #astronomy #education I record lectures live and place them here un-edited, in the hope that it will provide a more authentic feeling of the sort: "we're doing the actual work here and now". So like I keep telling students in the classroom: whenever you discover me doing some error let me know directly; for this channel this means make a comment on the videos. Then we can have a look at it, and thereby learn nicely from each other as we continue to develop our knowledge. You find all lectures under: https://www.youtube.com/playlist?list=PLrGAIWCGSKlDXALWS_6R4Bv3D1vEk85NX If you're interested more in my group's research, here're two links for that: https://fys.kuleuven.be/ster/research-projects/equation-folder/equation-home https://www.youtube.com/@JonSundqvist
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