LOCAL STUDY OF ACCRETION DISKS WITH A STRONG VERTICAL MAGNETIC FIELD: MAGNETOROTATIONAL INSTABILITY AND DISK OUTFLOW
By Xue-Ning Bai, James M. Stone. 2012
173 citations recorded by the source corpus.
We perform three-dimensional, vertically-stratified, local shearing-box ideal MHD simulations of the magnetorotational instability (MRI) that include a net vertical magnetic flux, which is characterized by midplane plasma β0 (ratio of gas to magnetic pressure). We have considered β0 = 102, 103, and 104, and in the first two cases the most unstable linear MRI modes are well resolved in the simulations. We find that the behavior of the MRI turbulence strongly depends on β0: the radial transport of angular momentum increases with net vertical flux, achieving α ∼ 0.08 for β = 104 and α ≳ 1.0 for β0 = 100, where α is the height-integrated and mass-weighted Shakura–Sunyaev parameter. A critical value lies at β0 ∼ 103: for β0 ≳ 103, the disk consists of a gas pressure dominated midplane and a magnetically dominated corona. The turbulent strength increases with net flux, and angular momentum transport is dominated by turbulent fluctuations. The magnetic dynamo that leads to cyclic flips of large-scale fields still exists, but becomes more sporadic as net flux increases. For β0 ≲ 103, the entire disk becomes magnetically dominated. The turbulent strength saturates, and the magnetic dynamo is fully quenched. Stronger large-scale fields are generated with increasing net flux, which dominates angular momentum transport. A strong outflow is launched from the disk by the magnetocentrifugal mechanism, and the mass flux increases linearly with net vertical flux and shows sign of saturation at β0 ≲ 102. However, the outflow is unlikely to be directly connected to a global wind: for β0 ≳ 103, the large-scale field has no permanent bending direction due to dynamo activities, while for β0 ≲ 103, the outflows from the top and bottom sides of the disk bend towards opposite directions, inconsistent with a physical disk wind geometry. Global simulations are needed to address the fate of the outflow.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/7b42480b483ba0be2c06dfb72713dfb3d2bb47db
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In Astronomy and Astrophysics
Citations in the corpus
- Non-thermal particle acceleration in collisionless relativistic electron-proton reconnection (2016, background): “…dominated coronae in accretion disc models with vertical stratification is well documented in local (shearing box) simulations (Miller & Stone 2000; Bai & Stone 2013; Salvesen et al. 2016), suggesting that reconnection is the dominant dissipation and particle acceleration mechanism (Galeev et al.…”
- How to form planetesimals from mm-sized chondrules and chondrule aggregates (2015, background): “The second way to increase Z is to remove gas from the disk, either through late-stage photoevaporation (e.g., Alexander et al. 2006a,b) or through disk winds (Bai & Stone 2013; Suzuki & Inutsuka 2009).”
- Accretion onto Pre-Main-Sequence Stars (2016, methodology): “Simulations by Bai & Stone (2013) and Gressel et al. (2015) of disks with AD show the development of strong disk winds over a range of radii between ∼1 and 10 AU, with angular momentum transport driven by wind coupling.”
- Thanatology in protoplanetary discs - The combined influence of Ohmic, Hall, and ambipolar diffusion on dead zones (2014, methodology): “To circumvent this problem, we following Bai & Stone (2013b) by introducing a capping procedure on the magnetic diffusivities ηO,H,A.”
- Hot Accretion Flows Around Black Holes (2014, background): “Some shearing box simulations even find α values larger than unity (e.g., Bai & Stone 2013).”
- WIND-DRIVEN ACCRETION IN PROTOPLANETARY DISKS. I. SUPPRESSION OF THE MAGNETOROTATIONAL INSTABILITY AND LAUNCHING OF THE MAGNETOCENTRIFUGAL WIND (2013, methodology): “We note that the mass outflow rate is not a well-characterized quantity in shearing-box (Bai & Stone 2013), these measurements should only be taken as a reference.”