Skip to main content Accessibility help
×
Home
Hostname: page-component-888d5979f-zxcqg Total loading time: 0.145 Render date: 2021-10-25T12:12:29.424Z Has data issue: true Feature Flags: { "shouldUseShareProductTool": true, "shouldUseHypothesis": true, "isUnsiloEnabled": true, "metricsAbstractViews": false, "figures": true, "newCiteModal": false, "newCitedByModal": true, "newEcommerce": true, "newUsageEvents": true }

Effect of Advected Fields on Accretion Disk Dynamos

Published online by Cambridge University Press:  12 April 2016

Arun V. Mangalam
Affiliation:
Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30303-3083
K. Subramanian
Affiliation:
National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune, India
Rights & Permissions[Opens in a new window]

Abstract

HTML view is not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present calculations of favored dynamo modes when advection of ambient magnetic fields onto accretion disks is important. These models are relevant for compact binary systems and young stellar objects and can be extended to active galactic nuclei (AGNs). The dynamo equation, including the standard α-effect, is modified to take into account advected magnetic fields. Vacuum boundary conditions are assumed outside the disk and the dynamo number switches sign across the equatorial plane. For the local steady state problem, critical dynamo numbers for various modes are obtained analytically. Our motivation is to investigate whether the dominant dynamo generation of quadrupolar magnetic fields and accretion of dipolar magnetic fields is likely to lead to particle acceleration in the form of jets. The results shown here are for a particular choice of boundary conditions and geometry of the advected field. Besides examining other choices, we shall calculate growth rates for different modes, and the influence of the initial seed field configuration on the evolution of the magnetic fields in subsequent work.

Subject headings: acceleration of particles — accretion, accretion disks — binaries: close — galaxies: nuclei — MHD — stars: pre-main-sequence

Type
Poster Papers
Copyright
Copyright © The American Astronomical Society 1994

References

Blandford, R.D. 1989, in Theory of Accretion Disks, ed. Meyer, F. et al. (Dordrecht: Kluwer), 35 CrossRefGoogle Scholar
Blandford, R.D., & Payne, D.G. 1982, MNRAS, 199, 883 CrossRefGoogle Scholar
Chandrashekar, S. 1956, ApJ, 124, 232 CrossRefGoogle Scholar
Krause, F., & Rädler, K.H. 1980, Mean-Field Magnetohydrodynamics and Dynamo Theory (Oxford: Pergamon)Google Scholar
Lovelace, R.V.E., Wang, J.C.L., & Sulkanen, M.E. 1987, ApJ, 315, 504 CrossRefGoogle Scholar
Mangalam, A.V., & Subramanian, K. 1994, in preparationGoogle Scholar
Mestel, L. 1961, MNRAS, 122, 473 CrossRefGoogle Scholar
Moffat, H.K. 1978, Magnetic Field Generation in Electrically Conducting Fluids (Cambridge Univ. Press)Google Scholar
Parker, E.N. 1955, ApJ, 122, 293 CrossRefGoogle Scholar
Parker, E.N. 1971, ApJ, 163, 255 CrossRefGoogle Scholar
Pelletier, G., & Pudritz, R.E., 1992, ApJ, 394, 117 CrossRefGoogle Scholar
Pudritz, R.E. 1981a, MNRAS, 195, 881 CrossRefGoogle Scholar
Pudritz, R.E. 1981b, MNRAS, 195, 897 CrossRefGoogle Scholar
Ruzmaikin, A.A., Shukurov, A.M., & Sokoloff, D.D. 1988, Magnetic Fields of Galaxies (Dordrecht: Kluwer)CrossRefGoogle Scholar
Ruzmaikin, A.A., & Sokoloff, D.D. 1979, A&A, 78, 1 Google Scholar
Zeldovich, Y.B., Ruzmaikin, A.A., & Sokoloff, D.D. 1983, Magnetic Fields in Astrophysics (New York: Gordon & Breach)Google Scholar
You have Access

Send article to Kindle

To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

Find out more about the Kindle Personal Document Service.

Effect of Advected Fields on Accretion Disk Dynamos
Available formats
×

Send article to Dropbox

To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

Effect of Advected Fields on Accretion Disk Dynamos
Available formats
×

Send article to Google Drive

To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

Effect of Advected Fields on Accretion Disk Dynamos
Available formats
×
×

Reply to: Submit a response

Please enter your response.

Your details

Please enter a valid email address.

Conflicting interests

Do you have any conflicting interests? *