Near-critical magnetic fields in Kepler red giants
Abstract
Context. The recent seismic detection of magnetic fields in the cores of red giants has provided the opportunity to characterize these fields, potentially allowing access to information about their origin and their role in the internal transport of angular momentum. Aims. We detected strong deviations from the regular pattern of g -mode periods in eight Kepler red giants showing l = 1 doublets. In three of these stars, the modes show partial suppression. We investigated the magnetic origin of these features and determined the characteristics of the core fields that can produce such signatures (strength, topology). Methods. We needed to invoke strong near-critical fields. Assessing the effects of such fields on the mixed mode frequencies requires a non-perturbative approach. We used and adapted a formalism that was recently proposed following a similar development as the traditional approximation for rotation. We then computed asymptotic expressions of mixed mode frequencies including magnetic effects and attempted to reproduce the observed oscillation spectra. Results. We show that for near-critical fields, information can be obtained about the radial profile of the radial field B r , as opposed to weaker fields for which only a weighted average of B r 2 can be measured. For the eight targets, we found that the l = 1 doublets cannot be identified as the m = ±1 components. Instead, we show that very good fits to all the observations can be obtained by identifying the two components as m = 0 and m = 1. These solutions correspond to fields with intensities ranging from 100 to 700 kG that are confined well below the H-burning shell. Our best-fit models for the eight stars have low masses (1.1–1.2 M ⊙ ), and the maximal size of their convective core during the main sequence approximately corresponds to the radial extent of the measured magnetic fields. The detected fields therefore could have been generated by dynamo action in the main-sequence convective core.
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BibTeX
@article{deheuvels2026nearcritical,
title = {{Near-critical magnetic fields in Kepler red giants}},
author = {S. Deheuvels and J. Ballot and F. Lignières and Gang Li and M. Villate},
journal = {Astronomy \& Astrophysics - A\&A},
year = {2026},
month = may,
doi = {10.1051/0004-6361/202659344},
eprint = {2604.09901},
archivePrefix = {arXiv},
url = {https://hal.science/hal-05790247v1},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Near-critical magnetic fields in Kepler red giants
AU - S. Deheuvels
AU - J. Ballot
AU - F. Lignières
AU - Gang Li
AU - M. Villate
PY - 2026
DA - 2026/05/19
JO - Astronomy & Astrophysics - A&A
DO - 10.1051/0004-6361/202659344
UR - https://hal.science/hal-05790247v1
AB - Context. The recent seismic detection of magnetic fields in the cores of red giants has provided the opportunity to characterize these fields, potentially allowing access to information about their origin and their role in the internal transport of angular momentum. Aims. We detected strong deviations from the regular pattern of g -mode periods in eight Kepler red giants showing l = 1 doublets. In three of these stars, the modes show partial suppression. We investigated the magnetic origin of these features and determined the characteristics of the core fields that can produce such signatures (strength, topology). Methods. We needed to invoke strong near-critical fields. Assessing the effects of such fields on the mixed mode frequencies requires a non-perturbative approach. We used and adapted a formalism that was recently proposed following a similar development as the traditional approximation for rotation. We then computed asymptotic expressions of mixed mode frequencies including magnetic effects and attempted to reproduce the observed oscillation spectra. Results. We show that for near-critical fields, information can be obtained about the radial profile of the radial field B r , as opposed to weaker fields for which only a weighted average of B r 2 can be measured. For the eight targets, we found that the l = 1 doublets cannot be identified as the m = ±1 components. Instead, we show that very good fits to all the observations can be obtained by identifying the two components as m = 0 and m = 1. These solutions correspond to fields with intensities ranging from 100 to 700 kG that are confined well below the H-burning shell. Our best-fit models for the eight stars have low masses (1.1–1.2 M ⊙ ), and the maximal size of their convective core during the main sequence approximately corresponds to the radial extent of the measured magnetic fields. The detected fields therefore could have been generated by dynamo action in the main-sequence convective core.
SN - 0004-6361
SN - 1432-0746
ER -