Abstract
Pushed by the rapid rise of gravitational wave astronomy, the study of compact binary mergers has made significant progress over the last 5 years. Multiple binary black hole and binary neutron star systems have been detected, and while we are still waiting for the first confirmed observation of a mixed black hole-neutron star (BHNS) merger, a number of candidate events have been announced over the last observing run of the LIGO-Virgo Collaboration. BHNS mergers have many of the same advantages as neutron star mergers, including their potential to help us constrain the properties of dense nuclear matter and their ability to power bright electromagnetic counterparts and produce heavy r-process elements. There are however important differences between BHNS and binary neutron star mergers that significantly impact what we can hope to accomplish from their observation. In this chapter, we will review the basic physics of BHNS mergers and the properties of the observable gravitational wave and electromagnetic signals that they power. We will also discuss the current status of theoretical and numerical models of these signals, their successes, limitations, and likely future areas of improvements. Finally, we will consider the role that these models play in the robust interpretation of BHNS observations and how current model limitations impact what we can learn from multi-messenger observations of BHNS binaries.
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Foucart, F. (2022). Black Hole-Neutron Star Mergers. In: Bambi, C., Katsanevas, S., Kokkotas, K.D. (eds) Handbook of Gravitational Wave Astronomy. Springer, Singapore. https://doi.org/10.1007/978-981-16-4306-4_14
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