HALL-EFFECT-CONTROLLED GAS DYNAMICS IN PROTOPLANETARY DISKS. I. WIND SOLUTIONS AT THE INNER DISK

The gas dynamics of protoplanetary disks (PPDs) is largely controlled by non-ideal magnetohydrodynamic (MHD) effects including Ohmic resistivity, the Hall effect, and ambipolar diffusion. In this series, we have included, for the first time, all three non-ideal MHD effects in a self-consistent manne...

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Bibliographic Details
Published inThe Astrophysical journal Vol. 791; no. 2; pp. 137 - 22
Main Author Bai, Xue-Ning
Format Journal Article
LanguageEnglish
Published United States 20.08.2014
Subjects
Accretion disks
AMBIPOLAR DIFFUSION
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Gas dynamics
HALL EFFECT
INSTABILITY
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MATHEMATICAL SOLUTIONS
MHD
Planet formation
PROTOPLANETS
SIMULATION
Stellar winds
STRESSES
TURBULENCE
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Summary:The gas dynamics of protoplanetary disks (PPDs) is largely controlled by non-ideal magnetohydrodynamic (MHD) effects including Ohmic resistivity, the Hall effect, and ambipolar diffusion. In this series, we have included, for the first time, all three non-ideal MHD effects in a self-consistent manner to investigate the role of the Hall effect on PPD gas dynamics using local shearing-box simulations. In this first paper, we focus on the inner region of PPDs, where previous studies (Bai & Stone 2013; Bai 2013) excluding the Hall effect have revealed that the inner disk up to ~10 AU is largely laminar, with accretion driven by a magnetocentrifugal wind. We confirm this basic picture and show that the Hall effect modifies the wind solutions depending on the polarity of the large-scale poloidal magnetic field B sub(0) threading the disk. Scaling relations for the wind properties, especially the wind-driven accretion rate, are provided for aligned and anti-aligned field geometries.
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ISSN:1538-4357
0004-637X
1538-4357
DOI:10.1088/0004-637X/791/2/137