Sign on
ADS Classic will be deprecated in May 2019 and retired in October 2019. Please redirect your searches to the new ADS modern form or the classic form. More info can be found on our blog.

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (370) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
· Translate This Page
Hydromagnetic disk winds in young stellar objects and active galactic nuclei
Pelletier, Guy; Pudritz, Ralph E.
AA(Grenoble, Observatoire, France), AB(Grenoble, Observatoire, France; McMaster University, Hamilton, Canada)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 394, no. 1, July 20, 1992, p. 117-138. Research supported by NATO and NSERC. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Accretion Disks, Active Galactic Nuclei, Black Holes (Astronomy), Early Stars, Magnetohydrodynamic Flow, Stellar Winds, Angular Momentum, Computational Astrophysics, Hydrodynamic Equations, Interstellar Magnetic Fields, Stellar Mass Ejection
Astronomy Keywords:
galaxies: nuclei MHD stars: pre-main-sequence stars: mass loss
Bibliographic Code:


We present a general theory for the origin and collimation of centrifugally driven, hydromagnetic winds from the surfaces of Keplerian accretion disks that surround central objects such as young stellar objects (YSOs) or black holes. The theory is fully two-dimensional and makes no assumption about self-similarity of the flows. These winds efficiently extract disk angular momentum and convert the gravitational binding energy released in the accretion process into the mechanical energy of the wind. We investigate solutions under the very general assumption that the magnetic flux in the disk scales as a power law in disk radius r0 as psi0 ∝ r3/2a0. We find analytical solutions for many of the physical quantities in the outflow, such as the wind speed, mass-loss rate, thrust, density, Alfvén surface, etc. We demonstrate that the self-similar solutions of Blandford & Payne (a = 2) are a special case of our theory. We find that large classes of models have the generic property that they self-collimate due to the J x B pinching force arising from the toroidal magnetic field component in the outflow that dominates far from the surface of the accretion disk. We also find that flows that achieve modest values for fast magnetosonic Mach numbers recollimate toward the axis forming magnetic focal points.

We identify a unique non-self-similar solution (a = 3) that carries a constant current intensity everywhere (the toroidal field scales as Bphi ∝ r-1 - for this case) and is free of the divergences of self-similar models. We apply our results to both bipolar outflows in the vicinity of YSOs and black hole/accretion disk models for active galactic nuclei (AGNs). We find that modest magnetic field strengths (<= 104 G for AGNs, 10 G for YSOs) in the inner portions of these disks are sufficient to drive flows that match all the known observational constraints. In no case do the required magnetic energy densities exceed that of thermal pressure in these disks. An important new result in our theory is an intrinsic scale length to the disk outflow. The mass accretion rate is fundamentally connected to the wind mass-loss rate from the disk because it is the wind that carries off the disk angular momentum. We typically find that the ratio of the wind mass-loss rate to the accretion rate, MsW/Msa, is 10-1 for both the YSO and AGN models. Our results suggest that the highly collimated outflows seen in regions of star formation and in galactic nuclei share a simple physical mechanism that depends only upon the presence of magnetized gas with angular momentum, and the depth of the central gravitational potential well.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences

More Article Retrieval Options

HELP for Article Retrieval

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints