Global simulations of protoplanetary disks with net magnetic flux: I. Non-ideal MHD case
By W. B'ethune, G. Lesur, J. Ferreira. 2016
157 citations recorded by the source corpus.
The planet-forming region of protoplanetary disks is cold, dense, and therefore weakly ionized. For this reason, magnetohydrodynamic (MHD) turbulence is thought to be mostly absent, and another mechanism has to be found to explain gas accretion. It has been proposed that magnetized winds, launched from the ionized disk surface, could drive accretion in the presence of a large-scale magnetic field. The efficiency and the impact of these surface winds on the disk structure is still highly uncertain. We present the first global simulations of a weakly ionized disk that exhibits large-scale magnetized winds. We also study the impact of self-organization, which was previously demonstrated only in non-stratified models. We perform numerical simulations of stratified disks with the PLUTO code. We compute the ionization fraction dynamically, and account for all three non-ideal MHD effects: ohmic and ambipolar diffusions, and the Hall drift. Simplified heating and cooling due to non-thermal radiation is also taken into account in the disk atmosphere. We find that disks can be accreting or not, depending on the configuration of the large-scale magnetic field. Magnetothermal winds, driven both by magnetic acceleration and heating of the atmosphere, are obtained in the accreting case. In some cases, these winds are asymmetric, ejecting predominantly on one side of the disk. The wind mass loss rate depends primarily on the average ratio of magnetic to thermal pressure in the disk midplane. The non-accreting case is characterized by a meridional circulation, with accretion layers at the disk surface and decretion in the midplane. Finally, we observe self-organization, resulting in axisymmetric rings of density and associated pressure "bumps". The underlying mechanism and its impact on observable structures are discussed.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/6e6992ea4bef83f1532e3b98731377529c0038a9
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In Astronomy and Astrophysics
Citations in the corpus
- The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “…dust, and magnetic fields are coupled (e.g., Dzyurkevich et al. 2013; Bai & Stone 2014; Flock et al. 2015; Lyra et al. 2015; Dipierro et al. 2015; Béthune et al. 2017; Dullemond & Penzlin 2018; Suriano et al. 2018) or by strong gradients in material properties (e.g., Okuzumi et al. 2012;…”
- Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “…coupled disk wind systems in the presence of a poloidal magnetic field (Suriano et al. 2018), disk self-organization due to nonideal MHD effects (Béthune et al. 2017), suppressed grain growth with the effect of sintering (Okuzumi et al. 2016), large-scale instabilities due to dust settling…”
- Global Simulations of the Inner Regions of Protoplanetary Disks with Comprehensive Disk Microphysics (2017, methodology): “Another exception is the very recent work of Béthune et al. (2017), which we will discuss in more detail in Section 8.2.”
- The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, background): “…et al. 2009; Bai & Stone 2014; Simon & Armitage 2014), surface density enhancements at the edges of dead zones (e.g., Lyra et al. 2015; Flock et al. 2015; Ruge et al. 2016), and the spontaneous concentration of magnetic flux (e.g., Bai & Stone 2014; Béthune et al. 2017; Suriano et al. 2018).”