Abstract
A solution is presented for the nearly force-free magnetic field in the inner region of an accretion disc wind, well inside the Alfven surface. This is matched to a dynamo-generated disc field and the consequences for the disc and wind structures are investigated. The radial and vertical structures of the disc are found, together with the essential properties of the wind flow. Solutions result for which the wind angular momentum loss is at least comparable to the viscous radial advection of angular momentum.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
