Magnetic field buoyancy in accretion disks of young stars

Abstract

Buoyancy of the fossil magnetic field in the accretion disks of young stars is investigated. It is assumed that the Parker instability leads to the formation of slender flux tubes of toroidal magnetic field in the regions of effective magnetic field generation. Stationary solution of the induction equation is written in the form in which buoyancy is treated as the additional mechanism of the magnetic flux escape. We calculate the fossil magnetic field intensity in the accretion disks of young T Tauri stars for the cases when radius of the magnetic flux tubes $a_{\mathrm{mft}}=0.1H$, $0.5H$ or $1H$, where $H$ is the accretion disk height scale. Calculations show that the buoyancy limits toroidal magnetic field growth, so that its strength is comparable with the vertical magnetic field strength for the case $a_{\mathrm{mft}}=0.1H$.

published in PEPAN Letters

References in corpus (4)

• The Magnetic Fields of Classical T Tauri Stars
• Spatially Resolved Magnetic Field Structure in the Disk of a T Tauri Star
• Fossil magnetic field of accretion disks of young stars
• Theory of fossil magnetic field

Cited by in corpus (2)

• Dynamics of magnetic flux tubes in accretion discs of T Tauri stars
• Influence of Ohmic and ambipolar heating on thermal structure of accretion discs