10.5281/zenodo.3818245
https://zenodo.org/records/3818245
oai:zenodo.org:3818245
Van Beeck, Jordan
Jordan
Van Beeck
0000-0002-5082-3887
Institute of Astronomy, KU Leuven
Prat, Vincent
Vincent
Prat
0000-0002-5335-4991
AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot
Van Reeth, Timothy
Timothy
Van Reeth
0000-0003-2771-1745
Institute of Astronomy, KU Leuven
Mathis, Stéphane
Stéphane
Mathis
0000-0001-9491-8012
AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot; LESIA, Observatoire de Paris, PSL University, CNRS, Sorbonne Université, Univ. Paris Diderot
Bowman, Dominic M.
Dominic M.
Bowman
0000-0001-7402-3852
Institute of Astronomy, KU Leuven
Neiner, Coralie
Coralie
Neiner
0000-0003-1978-9809
LESIA, Observatoire de Paris, PSL University, CNRS, Sorbonne Université, Univ. Paris Diderot,
Aerts, Conny
Conny
Aerts
0000-0003-1822-7126
Institute of Astronomy, KU Leuven; Dept. of Astrophysics, IMAPP, Radboud University Nijmegen; Max Planck Institute for Astronomy, Heidelberg
Detecting axisymmetric magnetic fields using gravity modes in intermediate-mass stars
Zenodo
2020
Michielsen, Mathias
Mathias
Michielsen
0000-0001-9097-3655
Institute of Astronomy, KU Leuven
Pedersen, May G.
May G.
Pedersen
0000-0002-7950-0061
Institute of Astronomy, KU Leuven
Johnston, C.
C.
Johnston
0000-0002-3054-4135
Institute of Astronomy, KU Leuven
2020-05-05
eng
arXiv:2005.02411
10.1051/0004-6361/201937363
10.5281/zenodo.3818210
https://zenodo.org/communities/eu
https://zenodo.org/communities/mesa
Creative Commons Attribution 4.0 International
Typical MESA and GYRE inlists associated with Van Beeck et al. (2020). MESA version 10398 and GYRE version 5.2.
Context: Angular momentum (AM) transport models of stellar interiors require improvements to explain the strong extraction of AM from stellar cores that is observed with asteroseismology. One of the often invoked mediators of AM transport are internal magnetic fields, even though their properties, observational signatures and influence on stellar evolution are largely unknown.
Aims: We study how a fossil, axisymmetric internal magnetic field affects period spacing patterns of dipolar gravity mode oscillations in main-sequence stars with masses of 1.3, 2.0 and 3.0 \(\mathrm{M}_{\odot}\) . We assess the influence of fundamental stellar parameters on the magnitude of pulsation mode frequency shifts.
Methods: We compute dipolar gravity mode frequency shifts due to a fossil, axisymmetric poloidal-toroidal internal magnetic field for a grid of stellar evolution models, varying stellar fundamental parameters. Rigid rotation is taken into account using the traditional approximation of rotation and the influence of the magnetic field is computed using a perturbative approach.
Results: We find magnetic signatures for dipolar gravity mode oscillations in terminal-age main-sequence stars that are measurable for a near-core field strength larger than 105 G. The predicted signatures differ appreciably from those due to rotation.
Conclusions: Our formalism demonstrates the potential for the future detection and characterization of strong fossil, axisymmetric internal magnetic fields in gravity-mode pulsators near the end of core-hydrogen burning from Kepler photometry, if such fields exist.
The publication date is the date of acceptance.
J. Van Beeck would like to thank researchers M. Michielsen, C. Johnston, and dr. M. G. Pedersen for their valuable input in the MESA and GYRE computations.
European Commission
10.13039/501100000780
647383
Stars: dynamical Processes driving tidal Interactions, Rotation and Evolution
European Commission
10.13039/501100000780
670519
Mixing and Angular Momentum tranSport of massIvE stars