[{"publication_status":"published","type":"journal_article","publisher":"IOP Publishing","doi":"10.3847/1538-4357/ae7a3c","oa":1,"quality_controlled":"1","article_processing_charge":"Yes","date_published":"2026-07-10T00:00:00Z","citation":{"short":"N.B. De Vries, A. Le Saux, I. Baraffe, T. Guillet, R.H.D. Townsend, A. Leclerc, A. Morison, The Astrophysical Journal 1005 (2026).","ista":"De Vries NB, Le Saux A, Baraffe I, Guillet T, Townsend RHD, Leclerc A, Morison A. 2026. Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. The Astrophysical Journal. 1005(2), 154.","chicago":"De Vries, Nils B., Arthur Le Saux, Isabelle Baraffe, Thomas Guillet, Richard H.D. Townsend, Armand Leclerc, and Adrien Morison. “Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">https://doi.org/10.3847/1538-4357/ae7a3c</a>.","apa":"De Vries, N. B., Le Saux, A., Baraffe, I., Guillet, T., Townsend, R. H. D., Leclerc, A., &#38; Morison, A. (2026). Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">https://doi.org/10.3847/1538-4357/ae7a3c</a>","ieee":"N. B. De Vries <i>et al.</i>, “Revealing mixed modes in compressible hydrodynamical simulations of red giant stars,” <i>The Astrophysical Journal</i>, vol. 1005, no. 2. IOP Publishing, 2026.","ama":"De Vries NB, Le Saux A, Baraffe I, et al. Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. <i>The Astrophysical Journal</i>. 2026;1005(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">10.3847/1538-4357/ae7a3c</a>","mla":"De Vries, Nils B., et al. “Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars.” <i>The Astrophysical Journal</i>, vol. 1005, no. 2, 154, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">10.3847/1538-4357/ae7a3c</a>."},"article_type":"original","keyword":["Stellar physics","Stellar interiors","Asteroseismology","Stellar oscillations","Hydrodynamical simulations"],"file_date_updated":"2026-07-13T08:14:01Z","abstract":[{"lang":"eng","text":"Mixed modes are observed in many low-mass evolved stars. They provide information about core rotation rates of these stars, which are lower than predicted by stellar evolution models. The mixed modes themselves have been invoked as an angular momentum (AM) transport mechanism, but estimating their transport efficiency requires knowledge of their amplitudes. We constrain, for the first time, the mixed-mode amplitudes in 2D hydrodynamical simulations of a 1.3M⊙ red giant using the code MUSIC. We perform two simulations with outer radial truncations at fractional radii ro/r⋆ = 0.90 and 0.98. We compare the modes in the simulation with those found using both GYRE and a Dedalus eigenvalue solver. Excellent frequency agreement is found for all p-dominated modes, with minor discrepancies for g-dominated modes, especially in the frequency range [60, 240] μHz. We find excellent eigenfunction agreement for all modes except those in this frequency range. According to empirical predictions, the largest kinetic energies are located around Vmax= 312.μHz, but in both simulations, the modes with frequencies of ν < 50 μHz have the largest kinetic energies. In the simulation with r/r⋆ = 0.98, the simulated modes have extrapolated surface velocities comparable to the empirical predictions, with the highest surface velocities in a bell-shaped curve peaking around ν = 700 μHz. The extrapolated surface velocities of the low-frequency modes are small and thus hard to observe, but their large kinetic energies deeper in the interior could significantly impact AM transport, which has not yet been investigated."}],"_id":"22262","project":[{"name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","grant_number":"101165631"}],"date_created":"2026-07-12T22:02:17Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","author":[{"full_name":"De Vries, Nils B.","first_name":"Nils B.","last_name":"De Vries"},{"last_name":"Le Saux","first_name":"Arthur","full_name":"Le Saux, Arthur"},{"first_name":"Isabelle","last_name":"Baraffe","full_name":"Baraffe, Isabelle"},{"full_name":"Guillet, Thomas","first_name":"Thomas","last_name":"Guillet"},{"full_name":"Townsend, Richard H.D.","first_name":"Richard H.D.","last_name":"Townsend"},{"id":"2a1fb1fc-f373-11ef-901a-87cee43a1217","full_name":"Leclerc, Armand","first_name":"Armand","last_name":"Leclerc"},{"first_name":"Adrien","last_name":"Morison","full_name":"Morison, Adrien"}],"OA_type":"gold","title":"Revealing mixed modes in compressible hydrodynamical simulations of red giant stars","OA_place":"publisher","file":[{"date_updated":"2026-07-13T08:14:01Z","access_level":"open_access","relation":"main_file","date_created":"2026-07-13T08:14:01Z","file_id":"22275","creator":"dernst","content_type":"application/pdf","file_size":14866194,"checksum":"d32061d2341bac3adeb404975c6bd59e","success":1,"file_name":"2026_AstrophysicalJour_deVries.pdf"}],"intvolume":"      1005","external_id":{"arxiv":["2606.07125"]},"ddc":["520"],"article_number":"154","has_accepted_license":"1","department":[{"_id":"LiBu"}],"scopus_import":"1","oa_version":"Published Version","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"day":"10","DOAJ_listed":"1","researchdata_availability":"yes","year":"2026","das_tickbox":"1","supplementarymaterial":"yes","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"date_updated":"2026-07-13T08:16:25Z","volume":1005,"dataavailabilitystatement":"The kinetic energies and surface velocities shown in Figure 4, as well as the underlying spectral data of this work, can be found in a Zenodo repository at doi:10.5281/zenodo.18661976.","arxiv":1,"month":"07","acknowledgement":"We would like to thank the referee for their careful reading of the manuscript and their constructive comments that helped improve the paper. N.B.V. would like to thank K. Belkacem and J. Philidet for helpful discussions. N.B.V. is supported by STFC grant ST/Y002164/1. A.L.S. acknowledges support from the European Research Council (ERC) under the Horizon Europe program (Synergy grant agreement 101071505: 4D-STAR) from the CNES SOHO-GOLF and PLATO grants at CEA-DAp, and from ATPS (CNRS/INSU). Part of this work was supported by the ERC grant No. 787361-COBOM. R.H.D.T. acknowledges support from NASA grants 80NSSC24K0895 and 80NSSC23K1517, and NSF grant 2407636. A.L. is supported by ERC Starting Grant 101165631 (“Calcifer”). The authors would like to acknowledge the use of the University of Exeter High-Performance Computing (HPC) facility, ISCA, in carrying out this work. This work used the DiRAC Memory Intensive service (Cosma8) at Durham University, managed by the Institute for Computational Cosmology, and the DiRAC Data Intensive service (DIaL3) at the University of Leicester, managed by the University of Leicester Research Computing Service. These facilities are managed on behalf of the STFC DiRAC HPC (www.dirac.ac.uk). The DiRAC services at Durham and Leicester were funded by BEIS, UKRI, and STFC capital funding, and STFC operations grants. The service at Durham received funding from Durham University. DiRAC is part of the UKRI Digital Research Infrastructure.","status":"public","PlanS_conform":"1"}]