The common envelope phase of binary star evolution plays an essential role in the formation of short period systems containing a compact object. In this process, significant mass and angular momentum are lost, transforming a wide progenitor system into a close remnant binary. The pathways leading to this phase and the outcomes are described. Emphasis is placed on the conditions that are required for survival of the binary according to the results of three-dimensional hydrodynamics calculations. The evolution of high-mass systems containing neutron stars is discussed, including double neutron stars, binary pulsars, Thorne-Zytkow objects, and high- and low-mass X-ray binaries.


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  • Article Type: Review Article
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