Strong surface outflows on accretion discs

Abstract

In order to provide an explanation for the unexpected radial brightness distribution of the steady accretion discs seen in nova-like variables, Nixon & Pringle (2019) proposed that the accretion energy is redistributed outwards by means of strong, magnetically driven, surface flows. In this paper we note that the "powerful, rotating disc winds" observed in the soft states of black hole X-ray binaries, and also in the disc around a magnetized neutron star in Her X-1, have the properties of the outflows postulated by Nixon & Pringle to exist in the nova-like variable accretion discs around white dwarfs. The relevant properties are that the flows are not winds, but are, instead, bound flows (traveling at less than the escape velocity) and that the mass fluxes in the flows are a substantial fraction of the accretion rate in the disc.

4 pages, 2 figures, accepted for publication in Astronomy & Astrophysics

References in corpus (4)

• Accretion disc viscosity: how big is alpha?
• The magnetic nature of disk accretion onto black holes
• A Comprehensive Chandra Study of the Disk Wind in the Black Hole Candidate 4U 1630-472
• An ionised accretion disc wind in Hercules X-1

Cited by in corpus (4)

• Vertical wind structure in an X-ray binary revealed by a precessing accretion disk
• The peculiar spectral evolution of the new X-ray transient MAXI J0637-430
• X-ray Spectra and Light Curves of Cooling Novae and a Nova-Like
• Do the periodic activities of repeating fast radio bursts represent the spins of neutron stars?