J/MNRAS/412/1162 Wind-driving protostellar accretion discs (Salmeron+, 2011)
Wind-driving protostellar accretion discs.
II. Numerical method and illustrative solutions.
Salmeron R., Konigl A., Wardle M.
<Mon. Not. R. Astron. Soc., 412, 1162-1180 (2011)>
=2011MNRAS.412.1162S 2011MNRAS.412.1162S
ADC_Keywords: Accretion ; Models
Keywords: accretion, accretion discs - MHD - stars: formation -
ISM: jets and outflows
Abstract:
We continue our study of weakly ionized protostellar accretion discs
that are threaded by a large-scale magnetic field and power a
centrifugally driven wind. It has been argued that there is already
evidence in several protostellar systems that such a wind transports a
significant fraction of the angular momentum from at least some part
of the disc. We model this situation by considering a radially
localized disc model in which the matter is everywhere well coupled to
the field and the wind is the main repository of excess angular
momentum. We consider stationary configurations in which magnetic
diffusivity counters the shearing and advection of the magnetic field
lines. In Wardle & Koenigl (1997, ASP Conf. Ser., 121, 561) we
analysed the disc structure in the hydrostatic approximation (vertical
motions neglected inside the disc) and presented exact disc/wind
solutions for the ambipolar diffusivity regime. In Koenigl, Salmeron &
Wardle (Paper I, 2010MNRAS.401..479K 2010MNRAS.401..479K) we generalized the hydrostatic
analysis to the Hall and Ohm diffusivity domains and used it to
identify the disc parameter sub-regimes in which viable solutions with
distinct physical properties can be expected to occur. In this paper
we test the results of Paper I by deriving full numerical solutions
(integrated through the sonic critical surface) of the disc equations
in the Hall domain.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 39 20501 Global, self-similar (BP82-type) wind solutions
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 9 E9.4 --- kappa Normalized mass-to-magnetic flux ratio, κ
11- 19 E9.4 --- lambda Normalized total specific angular momentum, λ
21- 29 E9.4 --- xi'b Inclination of the magnetic field lines at the base
of the wind, ξ'b
31- 39 E9.4 --- chiA Normalized height of the Alfven point, χA
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History:
From electronic version of the journal
References:
Konigl et al., Paper I 2010MNRAS.401..479K 2010MNRAS.401..479K
(End) Patricia Vannier [CDS] 17-Oct-2011