1997/12/31 by Alice C. Quillen, A. C. Quillen, David E. Trilling +1 · 1 citation
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Exoplanet #Jovian #Jupiter mass #Meteorology #Outflow #Physics #Planet #Planetary mass #Protoplanetary disk #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/306421
published as Astrophys.J. 508 (1998) 707 · AAS Latex, accepted for ApJ
arxiv created 1998/06/15 · openalex publication_date 1998/12/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We discuss the possibility that gaseous giant planets drive strong outflows during early phases of their formation. We consider the range of parameters appropriate for magneto-centrifugally driven stellar and disk outflow models and find that, if the proto-Jovian planet or accretion disk had a magnetic field of ≳10 G and moderate mass-inflow accretion rates through the disk of less than ~10 -7 M J yr -1 , it is possible to drive an outflow. Estimates based both on scaling from empirical laws observed in protostellar outflows and the magneto-centrifugal disk and stellar plus disk wind models suggest that winds with mass-outflow rates of order 10 -8 M J yr -1 and velocities of order ~20 km s -1 could be driven from proto-Jovian planets. Prospects for detection and some implications for the formation of the solar system are briefly discussed.