Abstract
Accretion is a general phenomenon in the interaction of astrophysical objects with their environment. Accretion onto white dwarfs, neutron stars and black holes in particular may give rise to multi-wavelength continuous and transient emission. The most extreme accretion scenarios are envisioned following birth of compact objects in core-collapse of massive stars. Accretion is a complex process of mass flow. Quite generally, in fall of angular momentum rich matter gives rise to disks. Accretion may continue provided angular momentum diffuses outwards, perhaps by a combination of turbulent viscosity and outflows.
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Notes
- 1.
In the classical limit, ingoring evaporation. Black holes evaporate by photon emission one-by-one that, in preserving unitarity, involves an astronomical amount of computation [6]. Subject to the Margolus-Levitin bound on quantum computation (1998, Physica D, 120, 88), this process is slow, one photon every few thousand light crossing time scales [7].
- 2.
Historically, this problem was treated before Bondi’s spherical accretion.
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van Putten, M.H. (2017). Accretion Flows onto Black Holes. In: Introduction to Methods of Approximation in Physics and Astronomy. Undergraduate Lecture Notes in Physics. Springer, Singapore. https://doi.org/10.1007/978-981-10-2932-5_11
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