The effect of a stellar magnetic variation on the jet velocity
arXiv:0808.1949 · doi:10.1086/592494
Abstract
Stellar jets are normally constituted by chains of knots with some periodicity in their spatial distribution, corresponding to a variability of order of several years in the ejection from the protostar/disk system. A widely accepted theory for the presence of knots is related to the generation of internal working surfaces due to variations in the jet ejection velocity. In this paper we study the effect of variations in the inner disk-wind radius on the jet ejection velocity. We show that a small variation in the inner disk-wind radius produce a variation in the jet velocity large enough to generate the observed knots. We also show that the variation in the inner radius may be related to a variation of the stellar magnetic field.
arXiv comment5 pages, 3 figures, accepted for publication in ApJ
References in corpus (14)
- The Magnetic Fields of Classical T Tauri Stars
- Which jet launching mechanism(s) in TTauri stars?
- Spin-Up/Spin-Down of Magnetized Stars with Accretion Disks and Outflows
- Magnetic field generation in fully convective rotating spheres
- Large-scale alpha^2-dynamo in low-mass stars and brown dwarfs
- Results of the ROTOR-program. I. The long-term photometric variability of classical T Tauri stars
- MHD Stellar and Disk Winds: Application to Planetary Nebulae
- Systematic construction of exact MHD models for astrophysical winds and jets
- Proper motions and velocity asymmetries in the RW Aur jet
- Simulation-Based Investigation of a Model for the Interaction Between Stellar Magnetospheres and Circumstellar Accretion Disks
- Magnetic Interaction between Stars and Accretion Disks
- The Propagation of Magneto-Centrifugally Launched Jets: I
- Magnetic Field Effects on the Structure and Evolution of Overdense Radiatively Cooling Jets
- Magnetic cycles and photometric variability of T Tauri stars