Centrifugally driven winds from protostellar accretion discs – I. Formulation and initial results

Article


Nolan, C. A., Salmeron, R., Federrath, C., Bicknell, G. V. and Sutherland, R. S.. 2017. "Centrifugally driven winds from protostellar accretion discs – I. Formulation and initial results." Monthly Notices of the Royal Astronomical Society. 471 (2), pp. 1488-1505. https://doi.org/10.1093/mnras/stx1642
Article Title

Centrifugally driven winds from protostellar accretion discs – I. Formulation and initial results

ERA Journal ID1074
Article CategoryArticle
AuthorsNolan, C. A. (Author), Salmeron, R. (Author), Federrath, C. (Author), Bicknell, G. V. (Author) and Sutherland, R. S. (Author)
Journal TitleMonthly Notices of the Royal Astronomical Society
Journal Citation471 (2), pp. 1488-1505
Number of Pages18
Year2017
PublisherOxford University Press
Place of PublicationUnited Kingdom
ISSN0035-8711
1365-2966
Digital Object Identifier (DOI)https://doi.org/10.1093/mnras/stx1642
Web Address (URL)https://academic.oup.com/mnras/article/471/2/1488/3906601
Abstract

Protostellar discs play an important role in star formation, acting as the primary mass reservoir for accretion on to young stars and regulating the extent to which angular momentum and gas is released back into stellar nurseries through the launching of powerful disc winds. In this study, we explore how disc structure relates to the properties of the wind-launching region, mapping out the regions of protostellar discs where wind launching could be viable. We combine a series of 1.5D semi-analytic, steady-state, vertical disc-wind solutions into a radially extended 1+1.5D model, incorporating all three diffusion mechanisms (Ohm, Hall and ambipolar). We observe that the majority of mass outflow via disc winds occurs over a radial width of a fraction of an astronomical unit, with outflow rates attenuating rapidly on either side. We also find that the mass accretion rate, magnetic field strength and surface density profile each have significant effects on both the location of the wind-launching region and the ejection/accretion ratio. M-out/M-in. Increasing either the accretion rate or the magnetic field strength corresponds to a shift of the wind-launching region to smaller radii and a decrease in. M-out/M-in, while increasing the surface density corresponds to launching regions at larger radii with increased. M-out/M-in. Finally, we discover a class of disc winds containing an ineffective launching configuration at intermediate radii, leading to two radially separated regions of wind launching and diminished. M-out/M-in. We find that the wind locations and ejection/accretion ratio are consistent with current observational and theoretical estimates.

Keywordsaccretion, accretion discs; stars - formation; jets and outflows
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 ©: 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Byline AffiliationsAustralian National University
Institution of OriginUniversity of Southern Queensland
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