Abstract
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 ∼10-7Mj 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 10-8M, 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.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 707-713 |
| Number of pages | 7 |
| Journal | Astrophysical Journal |
| Volume | 508 |
| Issue number | 2 PART II |
| DOIs | |
| State | Published - 1998 |
Keywords
- ISM: jets and outflows
- MHD
- Planetary systems
- Stars: mass loss
- Stars: pre-main-sequence
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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