2008/08/14 by Fabio De Colle, José Gracia, Jose Gracia +1 · 6 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Jet (fluid) #Magnetic declination #Magnetic field #Mechanics #Physics #Protostar #RADIUS #Star formation #Stars #Stellar, planetary, and galactic studies #Variation (astronomy) #astro-ph
paper · pdf · doi:10.1086/592494
published in The Astrophysical Journal 688(2), 1137-1141 (IOP Publishing) · 5 pages, 3 figures, accepted for publication in ApJ
arxiv created 2008/08/14 · openalex publication_date 2008/11/17 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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 produces 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.