The gamma-ray binaries LS 5039, LS I +61 303 and PSR B1259-63
Abstract
Three binaries are now established sources of emission at very high energies (>1e11 eV). They are composed of a massive star and a compact object. The emission can be due to the interaction of the relativistic wind from a young ms pulsar with the stellar wind of the companion, by which rotation-power ends up as non-thermal flux. Variations at VHE energies are explained as due to gamma-gamma absorption and/or changes in shock location along the orbit. Resolved radio emission is due to cooling particles trailing the pulsar.
Turn this paper into a full lesson
ArcXiv compiles a staged curriculum from this paper: 8-12 lessons across beginner → advanced, synthesised section guides, visuals, flashcards, a quiz, exercises, and on-demand deep dives per section. Grounded in the abstract, never invented.