Issue |
A&A
Volume 411, Number 3, December I 2003
|
|
---|---|---|
Page(s) | 623 - 635 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361:20034154 | |
Published online | 17 November 2003 |
Magnetically driven outflows from Jovian circum-planetary accretion disks
Institut für Physik, Universität Potsdam, Am Neuen Palais 10, 14469 Potsdam, Germany
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
Corresponding author: cfendt@aip.de
Received:
1
August
2003
Accepted:
6
October
2003
We discuss the possibility to launch an outflow from the close vicinity
of a protoplanetary core considering a model scenario where the protoplanet
surrounded by a circum-planetary accretion disk is located in a
circum-stellar disk.
For the circum-planetary disk accretion rate we assume
implying peak disk temperatures of about 2000 K.
The estimated disk ionization degree and Reynolds number allow for a
sufficient coupling between the disk matter and the magnetic field.
We find that the surface magnetic field strength of the protoplanet is
probably not more than 10 G,
indicating that the global planetary magnetosphere
is dominated by the circum-planetary disk magnetic field of
50 G.
The existence of a gap between circum-planetary disk and planet
seems to be unlikely.
The estimated field strength and mass flow rates allow for asymptotic
outflow velocities of
.
The overall outflow geometry will be governed by the orbital radius,
resembling a hollow tube or cone perpendicular the disk.
The length of the outflow built up during one orbital period is
about 100 AU, depending on the outflow velocity.
Outflows from circum-planetary disks may be visible in shock excited
emission lines along a tube of diameter of the orbital radius and
thickness of about 100 protoplanetary radii.
We derive particle densities of 3000
in this
layer.
Energetically, protoplanetary outflows cannot survive the interaction
with a protostellar outflow.
Due to the efficient angular momentum removal by the outflow,
we expect the protoplanetary outflow to influence the early planet
angular momentum evolution.
If this is true,
planets which have produced an outflow in earlier times will rotate
slower at later times.
The mass evolution of the planet is, however,
hardly affected as the outflow mass loss rate will be small compared
to the mass accumulated by the protoplanetary core.
Key words: ISM: jets and outflows / stars: planetary systems: formation / stars: planetary systems: protoplanetary disks
© ESO, 2003
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