Impact of rotation on the amplitude of acoustic modes in solar-like stars: insights from hydrodynamical simulations
Abstract
In solar-like stars, acoustic modes provide the main way of probing their internal structure and dynamics. Although these modes are expected to be ubiquitous in stars with convective envelopes, Kepler observations reveal that a significant fraction of solar-like stars show no detectable acoustic modes, particularly among rapidly rotating and magnetically active stars. Recent theoretical work has proposed that rotation tends to inhibit convective motions, thereby reducing the power available for stochastic excitationof low degree acoustic modes. Here, we test this prediction using fully compressible hydrodynamical simulations of a solar-like star. We perform a series of 2.5D simulations, which consider longitudinal symmetry, using the music code spanning rotation rates from 0 to 8 Ω ⊙ . We find a clear and systematic decline of acoustic mode amplitudes with increasing rotation rate. In the most rapidly rotating models, mode damping rates are also enhanced. The combined reduction in excitation and increase in damping with increasing rotation rate provide a physical explanation for the observed decrease in mode detectability in rapidly rotating solar-like stars. Our results demonstrate that rotation can significantly modify oscillation properties and must be accounted for when interpreting asteroseismic observations.
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BibTeX
@article{saux2026impact,
title = {{Impact of rotation on the amplitude of acoustic modes in solar-like stars: insights from hydrodynamical simulations}},
author = {Arthur Le Saux and Leïla Bessila and Stéphane Mathis},
journal = {Monthly Notices of the Royal Astronomical Society},
year = {2026},
month = jun,
doi = {10.1093/mnras/stag870},
url = {https://hal.science/hal-05843994v1},
note = {CC BY},
}
RIS
TY - JOUR
TI - Impact of rotation on the amplitude of acoustic modes in solar-like stars: insights from hydrodynamical simulations
AU - Arthur Le Saux
AU - Leïla Bessila
AU - Stéphane Mathis
PY - 2026
DA - 2026/06/14
JO - Monthly Notices of the Royal Astronomical Society
DO - 10.1093/mnras/stag870
UR - https://hal.science/hal-05843994v1
AB - In solar-like stars, acoustic modes provide the main way of probing their internal structure and dynamics. Although these modes are expected to be ubiquitous in stars with convective envelopes, Kepler observations reveal that a significant fraction of solar-like stars show no detectable acoustic modes, particularly among rapidly rotating and magnetically active stars. Recent theoretical work has proposed that rotation tends to inhibit convective motions, thereby reducing the power available for stochastic excitationof low degree acoustic modes. Here, we test this prediction using fully compressible hydrodynamical simulations of a solar-like star. We perform a series of 2.5D simulations, which consider longitudinal symmetry, using the music code spanning rotation rates from 0 to 8 Ω _⊙ . We find a clear and systematic decline of acoustic mode amplitudes with increasing rotation rate. In the most rapidly rotating models, mode damping rates are also enhanced. The combined reduction in excitation and increase in damping with increasing rotation rate provide a physical explanation for the observed decrease in mode detectability in rapidly rotating solar-like stars. Our results demonstrate that rotation can significantly modify oscillation properties and must be accounted for when interpreting asteroseismic observations.
SN - 0035-8711
SN - 1365-2966
ER -