Volume 460, Number 1, December II 2006
|Page(s)||317 - 322|
|Section||Planets and planetary systems|
|Published online||12 September 2006|
A magnetic communication scenario for hot Jupiters
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany e-mail: email@example.com;firstname.lastname@example.org
2 Theoretische Physik IV, Ruhr-Universität Bochum, 44780 Bochum, Germany e-mail: email@example.com
3 Institut für Theoretische Physik, Technische Universität Braunschweig, Mendelssohnstrasse 3, 38106 Braunschweig, Germany e-mail: firstname.lastname@example.org
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.