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Most massive stars are found in binaries (and higher multiplicity systems) that interact over the course of their evolution. Mass transfer plays a key role in understanding phenomena as diverse as supernovae, X-ray binaries, gamma ray bursts, kilonovae, tidal disruption events, novae, intermediate luminosity optical transients, and gravitational-wave mergers. I will discuss recent 3-d (hydrodynamics), 1-d (spherical stellar models), and 0-d (rapid binary population synthesis) efforts to explore mass transfer, including common-envelope evolution, and constrain it with observations. |
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