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Tayler Instability Revisited
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DOI：10.3847/1538-4357/ad71c8.png)
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摘要
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Tayler instability of toroidal magnetic fields B phi is broadly invoked as a trigger for turbulence and angular momentum transport in stars. This paper presents a systematic revision of the linear stability analysis for a rotating, magnetized, and stably stratified star. For plausible configurations of B phi , instability requires diffusive processes: viscosity, magnetic diffusivity, or thermal/compositional diffusion. Our results reveal a new physical picture, demonstrating how different diffusive effects independently trigger instability of two types of waves in the rotating star: magnetostrophic waves and inertial waves. It develops via overstability of the waves, whose growth rate sharply peaks at some characteristic wavenumbers. We determine instability conditions for each wave branch and find the characteristic wavenumbers. The results are qualitatively different for stars with magnetic Prandtl number Pm << 1 (e.g., the Sun) and Pm >> 1 (e.g., protoneutron stars). The parameter dependence of unstable modes suggests a nonuniversal scaling of the possible Tayler-Spruit dynamo.
Keyword:
ANGULAR-MOMENTUM TRANSPORT
TOROIDAL MAGNETIC-FIELDS
MAGNETOROTATIONAL INSTABILITY
DIFFERENTIAL ROTATION
DYNAMO ACTION
ADIABATIC STABILITY
STELLAR INTERIORS
MAIN-SEQUENCE
STARS
EVOLUTION
期刊
IF:
5.4
论文数:
8.3W
被引数:
32.0W
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