When dark matter assembles into large composites, the binding energy has to go somewhere. In a secluded dark sector it goes into the scalar field that holds the composites together, and that leftover field can show up in the CMB.

Almost everything you have ever touched is a bound state. What if dark matter is too? A walk from dark atoms to dark nuggets heavier than a bacterium, and why a detector a meter across might see only one a year.

A path-integral and diagrammatic proof that any correlation function of an odd number of photon fields vanishes exactly — the photon is C-odd, the vacuum is C-even, and QED conserves C — plus the three places the proof most often goes wrong.

Spending Furry's theorem: no photon tadpole, no three-photon vertex, why Euler–Heisenberg has only even powers of F, whole classes of Feynman diagrams deleted for free, why light doesn't scatter off light until fourth order, and where the theorem breaks near a magnetar.

How perturbation theory actually computes the field strength renormalization Z and the shift from bare mass m₀ to physical mass m, by resumming all 1PI insertions into the full propagator i/(p² − m₀² − M²(p²)).

A non-perturbative derivation showing that the analytic structure of the interacting two-point function forces field strength renormalization Z and a physical mass m ≠ m₀ — long before any loops or infinities appear.

A practical companion to a video I made in collaboration with STARGAZER on beginning the MSc Physics program at Heidelberg University — covering courses, research groups, admin, and life in the city.

Exploring the Poincaré group, its Casimir operators, and Wigner's classification of elementary particles by mass and spin/helicity.