| Issue |
A&A
Volume 460, Number 1, December II 2006
|
|
|---|---|---|
| Page(s) | 317 - 322 | |
| Section | Planets and planetary systems | |
| DOI | https://doi.org/10.1051/0004-6361:20065353 | |
| Published online | 12 September 2006 | |
A magnetic communication scenario for hot Jupiters
1
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany e-mail: preusse@steinbeis-europa.de;buechner@mps.mpg.de
2
Theoretische Physik IV, Ruhr-Universität Bochum, 44780 Bochum, Germany e-mail: ak@tp4.rub.de
3
Institut für Theoretische Physik, Technische Universität Braunschweig, Mendelssohnstrasse 3, 38106 Braunschweig, Germany e-mail: u.motschmann@tu-bs.de
Received:
3
April
2006
Accepted:
31
August
2006
The observations of enhanced chromospheric activity on HD 179949 as
well as on υ And with the same periods as their close-in planets seem
to indicate some kind of magnetic interaction between star and planet. A
constraint to any possible model are the large phase angles of 
and
, respectively. We present a simple model, which is based on the
propagation of Alfvén waves within the stellar wind flow relative to the
planet and which can meet this restriction. In the solar system such a model
is successfully used to explain the current system between Io and Jupiter.
Key words: planets and satellites: general / stars: magnetic fields / stars: winds, outflows / stars: activity
© ESO, 2006
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