Magnetic activity as an explanation for exoplanet signatures in post-common-envelope binaries. Schleicher, D., Navarrete, F., Käpylä, P., & Ortiz, C. In pages 275, July, 2023. ![Magnetic activity as an explanation for exoplanet signatures in post-common-envelope binaries [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex Eclipsing time variations in post-common-enevelope binaries have given risen to the suggestion that massive gas-rich planets are orbiting these systems on wide orbits, which would explain the planetary orbits via the light travel time effect. The planetary systems required to explain the data are however not always dynamically stable. An alternative explanation that is frequently discussed in the literature concerns modulations of the orbital period via magnetic activity, either via the Applegate or Lanza mechanism. The first of these requires a time-dependent quadrupole moment, which causes the eclipsing time variations via a time-dependent gravitational force, while in the second case a constant quadrupole moment is required giving rise to spin-orbit coupling. In this talk, we present 3D magneto-hydrodynamical simulations performed with the Pencil code, where we were modeling both solar mass stars and fully convective M-dwarf stars for a larger range of rotation rates. We quantify both the time-dependent as well as the constant component of the quadrupole moment as a result of magnetic activity, and compare it with the predictions of the Applegate and Lanza models. We expect that in principle both mechanisms may operate in real stars, though the Lanza mechanism is energetically more efficienet and may give rise to potentially larger variations.
@inproceedings{schleicher_magnetic_2023,
title = {Magnetic activity as an explanation for exoplanet signatures in post-common-envelope binaries},
url = {https://ui.adsabs.harvard.edu/abs/2023eas..conf..275S},
abstract = {Eclipsing time variations in post-common-enevelope binaries have given risen to the suggestion that massive gas-rich planets are orbiting these systems on wide orbits, which would explain the planetary orbits via the light travel time effect. The planetary systems required to explain the data are however not always dynamically stable. An alternative explanation that is frequently discussed in the literature concerns modulations of the orbital period via magnetic activity, either via the Applegate or Lanza mechanism. The first of these requires a time-dependent quadrupole moment, which causes the eclipsing time variations via a time-dependent gravitational force, while in the second case a constant quadrupole moment is required giving rise to spin-orbit coupling. In this talk, we present 3D magneto-hydrodynamical simulations performed with the Pencil code, where we were modeling both solar mass stars and fully convective M-dwarf stars for a larger range of rotation rates. We quantify both the time-dependent as well as the constant component of the quadrupole moment as a result of magnetic activity, and compare it with the predictions of the Applegate and Lanza models. We expect that in principle both mechanisms may operate in real stars, though the Lanza mechanism is energetically more efficienet and may give rise to potentially larger variations.},
author = {Schleicher, Dominik and Navarrete, Felipe and Käpylä, Petri and Ortiz, Carolina},
month = jul,
year = {2023},
pages = {275},
}
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