Wind-driving protostellar accretion discs – I. Formulation and parameter constraints

Article


Konigl, Arieh, Salmeron, Raquel and Wardle, Mark. 2009. "Wind-driving protostellar accretion discs – I. Formulation and parameter constraints." Monthly Notices of the Royal Astronomical Society. 401 (1), pp. 479-499. https://doi.org/10.1111/j.1365-2966.2009.15664.x
Article Title

Wind-driving protostellar accretion discs – I. Formulation and parameter constraints

ERA Journal ID1074
Article CategoryArticle
AuthorsKonigl, Arieh (Author), Salmeron, Raquel (Author) and Wardle, Mark (Author)
Journal TitleMonthly Notices of the Royal Astronomical Society
Journal Citation401 (1), pp. 479-499
Number of Pages21
Year2009
PublisherOxford University Press
Place of PublicationUnited Kingdom
ISSN0035-8711
1365-2966
Digital Object Identifier (DOI)https://doi.org/10.1111/j.1365-2966.2009.15664.x
Web Address (URL)https://academic.oup.com/mnras/article/401/1/479/1007793
Abstract

We study a model of weakly ionized, protostellar accretion discs that are threaded by a large-scale, ordered magnetic field and power a centrifugally driven wind. We consider the limiting case where the wind is the main repository of the excess disc angular momentum and generalize the radially localized disc model of Wardle & Königl, which focused on the ambipolar diffusion regime, to other field diffusivity regimes, notably Hall and Ohm. We present a general formulation of the problem for nearly Keplerian, vertically isothermal discs using both the conductivity-tensor and the multifluid approaches and simplify it to a normalized system of ordinary differential equations in the vertical space coordinate. We determine the relevant parameters of the problem and investigate, using the vertical-hydrostatic-equilibrium approximation and other simplifications, the parameter constraints on physically viable solutions for discs in which the neutral particles are dynamically well coupled to the field already at the mid-plane. When the charged particles constitute a two-component ion-electron plasma, one can identify four distinct sub-regimes in the parameter domain where the Hall diffusivity dominates and three sub-regimes in the Ohm-dominated domain. Two of the Hall sub-regimes can be characterized as being ambipolar diffusion-like and two as being Ohm-like: the properties of one member of the first pair of sub-regimes are identical to those of the ambipolar diffusion regime, whereas one member of the second pair has the same characteristics as one of the Ohm sub-regimes. All the Hall sub-regimes have Brb/|Bφb| (ratio of radial-to-azimuthal magnetic field amplitudes at the disc surface) >1, whereas in two Ohm sub-regimes this ratio is <1. When the two-component plasma consists, instead, of positively and negatively charged grains of equal mass, the entire Hall domain and one of the Ohm sub-regimes with Brb/|Bφb| < 1 disappear. All viable solutions require the mid-plane neutral-ion momentum exchange time to be shorter than the local orbital time. We also infer that vertical magnetic squeezing always dominates over gravitational tidal compression in this model. In a follow-up paper we will present exact solutions that test the results of this analysis in the Hall regime.

KeywordsAccretion, accretion discs; ISM: jets and outflows; MHD; Stars: formation
ANZSRC Field of Research 2020510109. Stellar astronomy and planetary systems
Public Notes

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2009 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Byline AffiliationsUniversity of Chicago, United States
Australian National University
Macquarie University
Institution of OriginUniversity of Southern Queensland
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