Bondi accretion is a theoretical model describing how a massive body, such as a star or a black hole, can collapse matter from its surroundings in a steady, spherically symmetric manner. The concept was introduced by Hermann Bondi in 1952 as a way to understand how celestial objects gather material from their environment in the context of gravitational forces.
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Bondi accretion is steady spherical accretion from a uniform gas reservoir onto a compact gravitating object. In its adiabatic form, compression raises internal energy without providing the irreversible shear heating of a radiatively efficient disk.