[{"article_processing_charge":"No","PlanS_conform":"1","intvolume":"       704","abstract":[{"lang":"eng","text":"Context. Asymmetries in the observed rotational splittings of a multiplet contain information about the star’s rotation profile and internal magnetic field. Moreover, the frequency regularities of multiplets can be used for mode identification. However, to exploit this information, highly accurate theoretical predictions are needed.\r\n\r\nAims. We aim to quantify the difference in the predicted mode asymmetries between a 1D perturbative method and a 2D method that includes a 2D stellar structure model, which takes rotation into account. We then place these differences between 1D and 2D methods in the context of asteroseismic measurements of internal magnetic fields. We only focus on the asymmetries and not on possible additional frequency peaks that can arise when the magnetic and rotation axis are misaligned.\r\n\r\nMethods. We coupled the 1D pulsation codes GYRE and StORM to the 2D stellar structure code ESTER and compared the oscillation predictions with the results from the 2D TOP pulsation code. We focused on zero-age main-sequence models representative of rotating β Cephei pulsators spinning at up to 20 per cent of the critical Keplerian rotation rate. Specifically, we investigated low-radial-order gravity and pressure modes.\r\n\r\nResults. We find a generally good agreement between the oscillation frequencies resulting from the 1D and 2D pulsation codes. We report differences in predicted mode multiplet asymmetries of mostly below 0.06 d−1. Since the magnetic asymmetries are small compared to the differences in the rotational asymmetries resulting from the 1D and 2D predictions, accurate measurements of the magnetic field are in most cases challenging.\r\n\r\nConclusions. Differences in the predicted mode asymmetries of a rotating star between 1D perturbative methods and 2D non-perturbative methods can greatly hinder accurate measurements of internal magnetic fields in main-sequence pulsators with low-order modes. Nevertheless, reasonably accurate measurements could be possible with npg ≥ 2 modes if the internal rotation is roughly below 10 per cent of the Keplerian critical rotation frequency for (aligned) magnetic fields of the order of a few hundred kilogauss. While the differences between the 1D and 2D frequency predictions are mostly too large for internal magnetic field detections, the rotational asymmetries predicted by StORM are in general accurate enough for asteroseismic modelling of the stellar rotation in main-sequence stars with identified low-order modes."}],"publication_status":"published","file":[{"creator":"dernst","file_id":"20937","access_level":"open_access","content_type":"application/pdf","success":1,"date_created":"2026-01-05T08:36:28Z","file_name":"2025_AstronomyAstrophysics_Mombarg.pdf","checksum":"d838b4783920c43b7cc866e9cf08b383","date_updated":"2026-01-05T08:36:28Z","relation":"main_file","file_size":2620909}],"status":"public","ec_funded":1,"OA_type":"diamond","arxiv":1,"article_number":"A336","volume":704,"department":[{"_id":"LiBu"}],"day":"19","publication":"Astronomy & Astrophysics","scopus_import":"1","year":"2025","has_accepted_license":"1","title":"Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields","_id":"20931","DOAJ_listed":"1","OA_place":"publisher","author":[{"full_name":"Mombarg, J. S.G.","first_name":"J. S.G.","last_name":"Mombarg"},{"last_name":"Vanlaer","full_name":"Vanlaer, V.","first_name":"V."},{"first_name":"Srijan B","full_name":"Das, Srijan B","last_name":"Das","orcid":"0000-0003-0896-7972","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149"},{"last_name":"Rieutord","full_name":"Rieutord, M.","first_name":"M."},{"full_name":"Aerts, C.","first_name":"C.","last_name":"Aerts"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"},{"last_name":"Mathis","full_name":"Mathis, S.","first_name":"S."},{"last_name":"Reese","first_name":"D. R.","full_name":"Reese, D. R."},{"last_name":"Ballot","full_name":"Ballot, J.","first_name":"J."}],"citation":{"ama":"Mombarg JSG, Vanlaer V, Das SB, et al. Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields. <i>Astronomy &#38; Astrophysics</i>. 2025;704. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557247\">10.1051/0004-6361/202557247</a>","ista":"Mombarg JSG, Vanlaer V, Das SB, Rieutord M, Aerts C, Bugnet LA, Mathis S, Reese DR, Ballot J. 2025. Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields. Astronomy &#38; Astrophysics. 704, A336.","chicago":"Mombarg, J. S.G., V. Vanlaer, Srijan B Das, M. Rieutord, C. Aerts, Lisa Annabelle Bugnet, S. Mathis, D. R. Reese, and J. Ballot. “Is a 1D Perturbative Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators? Implications for Measurements of Rotation and Internal Magnetic Fields.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202557247\">https://doi.org/10.1051/0004-6361/202557247</a>.","apa":"Mombarg, J. S. G., Vanlaer, V., Das, S. B., Rieutord, M., Aerts, C., Bugnet, L. A., … Ballot, J. (2025). Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557247\">https://doi.org/10.1051/0004-6361/202557247</a>","mla":"Mombarg, J. S. G., et al. “Is a 1D Perturbative Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators? Implications for Measurements of Rotation and Internal Magnetic Fields.” <i>Astronomy &#38; Astrophysics</i>, vol. 704, A336, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557247\">10.1051/0004-6361/202557247</a>.","short":"J.S.G. Mombarg, V. Vanlaer, S.B. Das, M. Rieutord, C. Aerts, L.A. Bugnet, S. Mathis, D.R. Reese, J. Ballot, Astronomy &#38; Astrophysics 704 (2025).","ieee":"J. S. G. Mombarg <i>et al.</i>, “Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields,” <i>Astronomy &#38; Astrophysics</i>, vol. 704. EDP Sciences, 2025."},"acknowledgement":"We thank the anonymous referee for their comments on the manuscript, Dario Fritzewski for providing the distribution of fractions of critical rotation for the β Cephei sample, and Zhao Guo for the discussions. The research leading to these results has received funding from the European Research Council (ERC) under the Horizon Europe programme (Synergy Grant agreement N°101071505: 4D-STAR). While partially funded by the European Union, views and opinions expressed are however those of the authors only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. V.V. acknowledges support from the Research Foundation Flanders (FWO) under grant agreement N°1156923N (PhD Fellowship). S.B.D. acknowledges funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement N°101034413. L.B. gratefully acknowledges support from the European Research Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement N°101165631). J.B., M.R., S.M. and J.S.G.M have been supported by CNES, focused on the preparation of the PLATO mission. Computations with ESTER and TOP have made use of the HPC resources from the CALMIP supercomputing centre (Grant 2023-P0107). This research made use of the numpy (Harris et al. 2020) and matplotlib (Hunter 2007) Python software packages.","article_type":"original","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_updated":"2026-02-16T12:14:36Z","oa":1,"quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_published":"2025-12-19T00:00:00Z","publisher":"EDP Sciences","related_material":{"record":[{"status":"public","id":"20936","relation":"research_data"}]},"language":[{"iso":"eng"}],"type":"journal_article","file_date_updated":"2026-01-05T08:36:28Z","doi":"10.1051/0004-6361/202557247","external_id":{"arxiv":["2511.09617"]},"ddc":["520"],"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"project":[{"_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413","call_identifier":"H2020"},{"grant_number":"101165631","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology"}],"month":"12","oa_version":"Published Version","date_created":"2026-01-04T23:01:35Z"},{"citation":{"mla":"Mombarg, Joey, et al. <i>Is a 1D Perturbative Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators?</i> Zenodo, 2025, doi:<a href=\"https://doi.org/10.5281/ZENODO.17580178\">10.5281/ZENODO.17580178</a>.","apa":"Mombarg, J., Vanlaer, V., Das, S. B., Rieutord, M., Aerts, C., Bugnet, L. A., … Ballot, J. (2025). Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Zenodo. <a href=\"https://doi.org/10.5281/ZENODO.17580178\">https://doi.org/10.5281/ZENODO.17580178</a>","ama":"Mombarg J, Vanlaer V, Das SB, et al. Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? 2025. doi:<a href=\"https://doi.org/10.5281/ZENODO.17580178\">10.5281/ZENODO.17580178</a>","chicago":"Mombarg, Joey, Vincent Vanlaer, Srijan B Das, Michel Rieutord, Conny Aerts, Lisa Annabelle Bugnet, Stephane Mathis, Daniel Reese, and Jerome Ballot. “Is a 1D Perturbative Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators?” Zenodo, 2025. <a href=\"https://doi.org/10.5281/ZENODO.17580178\">https://doi.org/10.5281/ZENODO.17580178</a>.","ista":"Mombarg J, Vanlaer V, Das SB, Rieutord M, Aerts C, Bugnet LA, Mathis S, Reese D, Ballot J. 2025. Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?, Zenodo, <a href=\"https://doi.org/10.5281/ZENODO.17580178\">10.5281/ZENODO.17580178</a>.","ieee":"J. Mombarg <i>et al.</i>, “Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?” Zenodo, 2025.","short":"J. Mombarg, V. Vanlaer, S.B. Das, M. Rieutord, C. Aerts, L.A. Bugnet, S. Mathis, D. Reese, J. Ballot, (2025)."},"author":[{"first_name":"Joey","full_name":"Mombarg, Joey","last_name":"Mombarg"},{"last_name":"Vanlaer","full_name":"Vanlaer, Vincent","first_name":"Vincent"},{"full_name":"Das, Srijan B","first_name":"Srijan B","last_name":"Das","orcid":"0000-0003-0896-7972","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149"},{"first_name":"Michel","full_name":"Rieutord, Michel","last_name":"Rieutord"},{"last_name":"Aerts","first_name":"Conny","full_name":"Aerts, Conny"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle"},{"last_name":"Mathis","full_name":"Mathis, Stephane","first_name":"Stephane"},{"full_name":"Reese, Daniel","first_name":"Daniel","last_name":"Reese"},{"last_name":"Ballot","first_name":"Jerome","full_name":"Ballot, Jerome"}],"article_processing_charge":"No","OA_place":"repository","_id":"20936","status":"public","abstract":[{"lang":"eng","text":"Supplementary material for Mombarg et al. (2025, A&A). Title: \"Is a 1D perturbative method sufficient for asteroseismic modelling of \r\n~Cephei pulsators? Implications for measurements of rotation and internal magnetic fields\"\r\n\r\nContent:\r\n- Non-rotating ESTER models and associated .GSM models. (Xini = 0.71, Zini = 0.014, vertical/horizonal viscosity 10^7 cm^2/s, vertical chemical diffusion 10^4 cm^2/s for evolution model. More details on the ESTER models can be found in the ESTER manual.\r\n\r\n- Rotational asymmetries computed with StORM and TOP in 1/d, and the central m=0 frequency from TOP in 1/d. (all_A*_new.pkl)\r\n\r\n- Magnetic asymmetries in 1/d for different obliquity angles between 0 and 90 deg for ZAMS and MAMS model, for B_0 = 75 kG. *_nu key gives unperturbed mode frequencies, *_npg the radial order (asym_dict.pkl, asym_dict_evol.pkl)"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_updated":"2026-02-16T12:14:36Z","oa":1,"type":"research_data_reference","doi":"10.5281/ZENODO.17580178","department":[{"_id":"LiBu"}],"main_file_link":[{"url":"https://doi.org/10.5281/zenodo.17580178","open_access":"1"}],"OA_type":"gold","related_material":{"record":[{"status":"public","relation":"used_in_publication","id":"20931"}]},"date_published":"2025-11-11T00:00:00Z","publisher":"Zenodo","title":"Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?","date_created":"2026-01-05T08:39:33Z","oa_version":"Submitted Version","month":"11","year":"2025","ddc":["520"],"day":"11"},{"article_processing_charge":"No","isi":1,"status":"public","abstract":[{"lang":"eng","text":"Context. Rotation plays an important role in stellar evolution. However, the mechanisms behind the transport of angular momentum in stars at various stages of their evolution are not well understood. To improve our understanding of these processes, it is necessary to measure and validate the internal rotation profiles of stars across different stages of evolution and mass regimes.\r\nAims. Our aim is to constrain the internal rotation profile of the 12-M⊙ β Cep pulsator HD 192575 from the observed pulsational multiplets and the asymmetries of their component frequencies.\r\nMethods. We updated the forward asteroseismic modelling of HD 192575 based on new TESS observations. We inverted the rotation profile from the symmetric part of the splittings and computed the multiplet asymmetries due to the Coriolis force and stellar deformation, which we treated perturbatively. We compared the computed asymmetries with the observed asymmetries.\r\nResults. Our new forward asteroseismic modelling is in agreement with previous results but with increased uncertainties, partially due to increased frequency precision, which required us to relax certain constraints. Ambiguity in the mode identification is the main source of the uncertainty, which also affects the inferred rotation profiles. Almost all acceptable rotation profiles occur in the regime below 0.4 d−1 and favour weak radial differential rotation, with a ratio of core to envelope rotation of less than 2. We find that the quality of the match between the observed and theoretically predicted mode asymmetries is strongly dependent on the mode identification and the internal structure of the star.\r\nConclusions. Our results offer the first detailed rotation inversion for a β Cep pulsator. They show that the rotation profile and the mode asymmetries provide a valuable tool for further constraining the evolutionary properties of HD 192575, and in particular the details of angular momentum transport in massive stars."}],"file":[{"creator":"dernst","file_id":"20354","access_level":"open_access","content_type":"application/pdf","success":1,"date_created":"2025-09-15T06:58:09Z","file_name":"2025_AstronomyAstrophysics_Vanlaer.pdf","checksum":"9ee9f34cf86305602d6cb3e07a1cc1a6","date_updated":"2025-09-15T06:58:09Z","relation":"main_file","file_size":3175077}],"publication_status":"published","PlanS_conform":"1","intvolume":"       701","department":[{"_id":"LiBu"}],"article_number":"A5","volume":701,"arxiv":1,"OA_type":"diamond","ec_funded":1,"title":"Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries","has_accepted_license":"1","year":"2025","scopus_import":"1","publication":"Astronomy & Astrophysics","day":"01","acknowledgement":"The authors appreciated the critical comments from the\r\nreferee, which encouraged V.V. to embark upon a new code development\r\nsprint. V.V. gratefully acknowledges support from the Research Foundation\r\nFlanders (FWO) under grant agreement N◦1156923N (PhD Fellowship) and\r\nN\r\n◦K233724N (Travel grant). D.M.B. gratefully acknowledges support from\r\nthe Research Foundation Flanders (FWO; grant number: 1286521N), and UK\r\nResearch and Innovation (UKRI) in the form of a Frontier Research grant under\r\nthe UK government’s ERC Horizon Europe funding guarantee (SYMPHONY;\r\ngrant number: EP/Y031059/1), and a Royal Society University Research Fellowship (URF; grant number: URF\\R1\\231631). S.B.D. acknowledges funding from\r\nthe European Union’s Horizon 2020 research and innovation programme under\r\nthe Marie Skłodowska-Curie grant agreement No 101034413. L.B. gratefully\r\nacknowledges support from the European Research Council (ERC) under the\r\nHorizon Europe programme (Calcifer; Starting Grant agreement N◦101165631).\r\nS.M. acknowledges support from the PLATO CNES grant at CEA/DAp.C.A.\r\nacknowledges financial support from the Research Foundation Flanders (FWO)\r\nunder grant K802922N (Sabbatical leave); she is grateful for the kind hospitality\r\noffered by CEA/Saclay during her sabbatical work visits in the spring of 2023.\r\nThe research leading to these results has received funding from the European\r\nResearch Council (ERC) under the Horizon Europe programme (Synergy Grant\r\nagreement N◦101071505: 4D-STAR). While funded by the European Union,\r\nviews and opinions expressed are however those of the author(s) only and do\r\nnot necessarily reflect those of the European Union or the European Research\r\nCouncil. Neither the European Union nor the granting authority can be held\r\nresponsible for them. The TESS data presented in this paper were obtained from\r\nthe Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for\r\nResearch in Astronomy, Inc., under NASA contract NAS5-26555. Support to\r\nMAST for these data is provided by the NASA Office of Space Science via grant\r\nNAG5-7584 and by other grants and contracts. Funding for the TESS mission\r\nwas provided by the NASA Explorer Program.","citation":{"mla":"Vanlaer, V., et al. “Interior Rotation Modelling of the β Cep Pulsator HD 192575 Including Multiplet Asymmetries.” <i>Astronomy &#38; Astrophysics</i>, vol. 701, A5, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202452885\">10.1051/0004-6361/202452885</a>.","apa":"Vanlaer, V., Bowman, D. M., Burssens, S., Das, S. B., Bugnet, L. A., Mathis, S., &#38; Aerts, C. (2025). Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452885\">https://doi.org/10.1051/0004-6361/202452885</a>","ista":"Vanlaer V, Bowman DM, Burssens S, Das SB, Bugnet LA, Mathis S, Aerts C. 2025. Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries. Astronomy &#38; Astrophysics. 701, A5.","ama":"Vanlaer V, Bowman DM, Burssens S, et al. Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries. <i>Astronomy &#38; Astrophysics</i>. 2025;701. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452885\">10.1051/0004-6361/202452885</a>","chicago":"Vanlaer, V., D. M. Bowman, S. Burssens, Srijan B Das, Lisa Annabelle Bugnet, S. Mathis, and C. Aerts. “Interior Rotation Modelling of the β Cep Pulsator HD 192575 Including Multiplet Asymmetries.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202452885\">https://doi.org/10.1051/0004-6361/202452885</a>.","ieee":"V. Vanlaer <i>et al.</i>, “Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries,” <i>Astronomy &#38; Astrophysics</i>, vol. 701. EDP Sciences, 2025.","short":"V. Vanlaer, D.M. Bowman, S. Burssens, S.B. Das, L.A. Bugnet, S. Mathis, C. Aerts, Astronomy &#38; Astrophysics 701 (2025)."},"author":[{"full_name":"Vanlaer, V.","first_name":"V.","last_name":"Vanlaer"},{"last_name":"Bowman","full_name":"Bowman, D. M.","first_name":"D. M."},{"last_name":"Burssens","first_name":"S.","full_name":"Burssens, S."},{"last_name":"Das","first_name":"Srijan B","full_name":"Das, Srijan B","orcid":"0000-0003-0896-7972","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149"},{"last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"Mathis","full_name":"Mathis, S.","first_name":"S."},{"last_name":"Aerts","full_name":"Aerts, C.","first_name":"C."}],"OA_place":"publisher","_id":"20350","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"article_type":"original","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_updated":"2026-02-16T12:12:53Z","doi":"10.1051/0004-6361/202452885","file_date_updated":"2025-09-15T06:58:09Z","type":"journal_article","language":[{"iso":"eng"}],"date_published":"2025-09-01T00:00:00Z","publisher":"EDP Sciences","oa_version":"Published Version","date_created":"2025-09-14T22:01:32Z","month":"09","project":[{"call_identifier":"H2020","grant_number":"101034413","name":"IST-BRIDGE: International postdoctoral program","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"},{"grant_number":"101165631","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"}],"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"ddc":["520"],"external_id":{"arxiv":["2506.19948"],"isi":["001561561200007"]}},{"_id":"17189","author":[{"first_name":"Chris S.","full_name":"Hanson, Chris S.","last_name":"Hanson"},{"id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","last_name":"Das","first_name":"Srijan B","full_name":"Das, Srijan B","orcid":"0000-0003-0896-7972"},{"first_name":"Prasad","full_name":"Mani, Prasad","last_name":"Mani"},{"full_name":"Hanasoge, Shravan","first_name":"Shravan","last_name":"Hanasoge"},{"last_name":"Sreenivasan","first_name":"Katepalli R.","full_name":"Sreenivasan, Katepalli R."}],"citation":{"short":"C.S. Hanson, S.B. Das, P. Mani, S. Hanasoge, K.R. Sreenivasan, Nature Astronomy 8 (2024) 1088–1101.","ieee":"C. S. Hanson, S. B. Das, P. Mani, S. Hanasoge, and K. R. Sreenivasan, “Supergranular-scale solar convection not explained by mixing-length theory,” <i>Nature Astronomy</i>, vol. 8. Springer Nature, pp. 1088–1101, 2024.","ama":"Hanson CS, Das SB, Mani P, Hanasoge S, Sreenivasan KR. Supergranular-scale solar convection not explained by mixing-length theory. <i>Nature Astronomy</i>. 2024;8:1088-1101. doi:<a href=\"https://doi.org/10.1038/s41550-024-02304-w\">10.1038/s41550-024-02304-w</a>","ista":"Hanson CS, Das SB, Mani P, Hanasoge S, Sreenivasan KR. 2024. Supergranular-scale solar convection not explained by mixing-length theory. Nature Astronomy. 8, 1088–1101.","chicago":"Hanson, Chris S., Srijan B Das, Prasad Mani, Shravan Hanasoge, and Katepalli R. Sreenivasan. “Supergranular-Scale Solar Convection Not Explained by Mixing-Length Theory.” <i>Nature Astronomy</i>. Springer Nature, 2024. <a href=\"https://doi.org/10.1038/s41550-024-02304-w\">https://doi.org/10.1038/s41550-024-02304-w</a>.","apa":"Hanson, C. S., Das, S. B., Mani, P., Hanasoge, S., &#38; Sreenivasan, K. R. (2024). Supergranular-scale solar convection not explained by mixing-length theory. <i>Nature Astronomy</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41550-024-02304-w\">https://doi.org/10.1038/s41550-024-02304-w</a>","mla":"Hanson, Chris S., et al. “Supergranular-Scale Solar Convection Not Explained by Mixing-Length Theory.” <i>Nature Astronomy</i>, vol. 8, Springer Nature, 2024, pp. 1088–101, doi:<a href=\"https://doi.org/10.1038/s41550-024-02304-w\">10.1038/s41550-024-02304-w</a>."},"acknowledgement":"We thank F. J. Simons for the codes for computing Slepian functions,\r\nM. Rempel and R. Cameron for their insights into solar convection, J.\r\nW. Lord for the numerical simulations and J. Naranjo for his help with\r\nthe NYUAD NetDRMS system. This research was carried out with the\r\nHigh Performance Computing resources at NYUAD. The datasets were\r\nprepared in the data centre at the Center for Space Science of NYUAD.\r\nThis research is based upon work supported by Tamkeen under the\r\nNYUAD Research Institute (Grant Nos G1502 and CASS to C.S.H,\r\nS.H. and K.R.S.). S.H. acknowledges funding from the Department\r\nof Atomic Energy, India. K.R.S. and S.H. acknowledge support from\r\nthe Ofice of Sponsored Research of King Abdullah University of\r\nScience and Technology (Award No. OSR-CRG2020-4342). S.B.D.\r\nacknowledges funding from the Elisabeth H. and F. A. Dahlen Award\r\n2022 by the Department of Geosciences, Princeton University. S.B.D.\r\nalso acknowledges funding from the European Union’s Horizon 2020\r\nresearch and innovation programme under a Marie Skłodowska-Curie\r\ngrant (Grant Agreement No. 101034413). Some data products were\r\nprocessed and downloaded from the German Data Center for SDO,\r\nwhich is funded by the German Aerospace Center (DLR Grant No.\r\n500L1701).","article_type":"original","date_updated":"2025-09-08T08:04:56Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","quality_controlled":"1","publisher":"Springer Nature","date_published":"2024-09-01T00:00:00Z","language":[{"iso":"eng"}],"doi":"10.1038/s41550-024-02304-w","type":"journal_article","external_id":{"isi":["001254181700001"]},"project":[{"name":"IST-BRIDGE: International postdoctoral program","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","call_identifier":"H2020","grant_number":"101034413"}],"publication_identifier":{"eissn":["2397-3366"]},"month":"09","oa_version":"None","date_created":"2024-06-30T22:01:05Z","page":"1088-1101","article_processing_charge":"No","intvolume":"         8","publication_status":"published","abstract":[{"lang":"eng","text":"Supergranules, which are solar flow features with a lateral scale of 30,000–40,000 km and a lifetime of ~24 h, form a prominent component of the Sun’s convective spectrum. However, their internal flows, which can be probed only by helioseismology, are not well understood. We analyse dopplergrams recorded by the Solar Dynamics Observatory satellite to identify and characterize ~23,000 supergranules. We find that the vertical flows peak at a depth of ~10,000 km, and remain invariant over the full range of lateral supergranular scales, contrary to numerical predictions. We also infer that, within the local seismic resolution (≳5,000 km), downflows are ~40% weaker than upflows, indicating an apparent mass-flux imbalance. This may imply that the descending flows also comprise plumes, which maintain the mass balance but are simply too small to be detected by seismic waves. These results challenge the widely used mixing-length description of solar convection."}],"isi":1,"status":"public","ec_funded":1,"OA_type":"closed access","volume":8,"department":[{"_id":"LiBu"}],"day":"01","publication":"Nature Astronomy","scopus_import":"1","year":"2024","title":"Supergranular-scale solar convection not explained by mixing-length theory"},{"tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_updated":"2025-09-08T08:42:20Z","article_type":"original","oa":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","quality_controlled":"1","_id":"17326","DOAJ_listed":"1","author":[{"first_name":"Shatanik","full_name":"Bhattacharya, Shatanik","last_name":"Bhattacharya"},{"orcid":"0000-0003-0896-7972","full_name":"Das, Srijan B","first_name":"Srijan B","last_name":"Das","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000"},{"last_name":"Panda","full_name":"Panda, Subrata","first_name":"Subrata"},{"last_name":"Hanasoge","first_name":"Shravan M.","full_name":"Hanasoge, Shravan M."}],"acknowledgement":"This project has received funding from the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101034413. S.\r\nB.D. acknowledges Prof. Jeroen Tromp at Princeton University for supporting a part of this work. S.M.H., S.B., and S.P. acknowledge support from the Department of Atomic Energy,\r\nGovernment of India, under Project Identification No. RTI 4002. The authors would like to thank the reviewer(s) and data editor for their constructive comments and suggestions. The\r\ngeneration of the stellar models was done using the Modules for Experiments in Stellar Astrophysics (MESA Paxton et al. 2011, 2013, 2015, 2018, 2019; we have used MESA version\r\nr22.05.1 for RG and r23.05.1 for SG models, MESA-SDK version x86_64-linux-22.6.1). The eigenfrequencies and eigenfunctions for this model were calculated using the GYRE\r\n(Townsend & Teitler 2013) code. The code to calculate the kernels and the splittings has been written completely in Python 3.8.16.","issue":"1","citation":{"ama":"Bhattacharya S, Das SB, Bugnet LA, Panda S, Hanasoge SM. Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars. <i>Astrophysical Journal</i>. 2024;970(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ad4708\">10.3847/1538-4357/ad4708</a>","chicago":"Bhattacharya, Shatanik, Srijan B Das, Lisa Annabelle Bugnet, Subrata Panda, and Shravan M. Hanasoge. “Detectability of Axisymmetric Magnetic Fields from the Core to the Surface of Oscillating Post-Main-Sequence Stars.” <i>Astrophysical Journal</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/1538-4357/ad4708\">https://doi.org/10.3847/1538-4357/ad4708</a>.","ista":"Bhattacharya S, Das SB, Bugnet LA, Panda S, Hanasoge SM. 2024. Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars. Astrophysical Journal. 970(1), 42.","mla":"Bhattacharya, Shatanik, et al. “Detectability of Axisymmetric Magnetic Fields from the Core to the Surface of Oscillating Post-Main-Sequence Stars.” <i>Astrophysical Journal</i>, vol. 970, no. 1, 42, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/1538-4357/ad4708\">10.3847/1538-4357/ad4708</a>.","apa":"Bhattacharya, S., Das, S. B., Bugnet, L. A., Panda, S., &#38; Hanasoge, S. M. (2024). Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars. <i>Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ad4708\">https://doi.org/10.3847/1538-4357/ad4708</a>","short":"S. Bhattacharya, S.B. Das, L.A. Bugnet, S. Panda, S.M. Hanasoge, Astrophysical Journal 970 (2024).","ieee":"S. Bhattacharya, S. B. Das, L. A. Bugnet, S. Panda, and S. M. Hanasoge, “Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars,” <i>Astrophysical Journal</i>, vol. 970, no. 1. IOP Publishing, 2024."},"external_id":{"isi":["001270972500001"],"arxiv":["2404.17167"]},"ddc":["520"],"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"project":[{"call_identifier":"H2020","grant_number":"101034413","name":"IST-BRIDGE: International postdoctoral program","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"}],"month":"07","date_created":"2024-07-28T22:01:09Z","oa_version":"Published Version","date_published":"2024-07-15T00:00:00Z","publisher":"IOP Publishing","language":[{"iso":"eng"}],"type":"journal_article","doi":"10.3847/1538-4357/ad4708","file_date_updated":"2024-07-29T11:02:48Z","intvolume":"       970","abstract":[{"lang":"eng","text":"Magnetic fields in the stellar interiors are key candidates to explain observed core rotation rates inside solar-like stars along their evolution. Recently, asteroseismic estimates of radial magnetic field amplitudes near the hydrogen-burning shell (H-shell) inside about 24 red giants (RGs) have been obtained by measuring frequency splittings from their power spectra. Using general Lorentz-stress (magnetic) kernels, we investigated the potential for detectability of near-surface magnetism in a 1.3 M⊙ star of supersolar metallicity as it evolves from a mid subgiant to a late subgiant into an RG. Based on these sensitivity kernels, we decompose an RG into three zones—deep core, H-shell, and near-surface. The subgiants instead required decomposition into an inner core, an outer core, and a near-surface layer. Additionally, we find that for a low-frequency g-dominated dipolar mode in the presence of a typical stable magnetic field, ∼25% of the frequency shift comes from the H-shell and the remaining from deeper layers. The ratio of the subsurface tangential field to the radial field in the H-burning shell decides if subsurface fields may be potentially detectable. For p-dominated dipole modes close to vmax, this ratio is around two orders of magnitude smaller in subgiant phases than the corresponding RG. Further, with the availability of magnetic kernels, we propose lower limits of field strengths in crucial layers in our stellar model during its evolutionary phases. The theoretical prescription outlined here provides the first formal way to devise inverse problems for stellar magnetism and can be seamlessly employed for slow rotators."}],"publication_status":"published","file":[{"access_level":"open_access","creator":"dernst","file_id":"17340","checksum":"acb42a87deecbc9228fbbe6a48a37ec6","relation":"main_file","date_updated":"2024-07-29T11:02:48Z","file_size":3912290,"success":1,"content_type":"application/pdf","date_created":"2024-07-29T11:02:48Z","file_name":"2024_AstrophysicalJourn_Bhattacharya.pdf"}],"isi":1,"status":"public","article_processing_charge":"Yes","day":"15","publication":"Astrophysical Journal","year":"2024","scopus_import":"1","has_accepted_license":"1","title":"Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars","ec_funded":1,"arxiv":1,"article_number":"42","volume":970,"department":[{"_id":"LiBu"}]},{"day":"01","publication":"Astronomy & Astrophysics","year":"2024","scopus_import":"1","has_accepted_license":"1","title":"Unveiling complex magnetic field configurations in red giant stars","ec_funded":1,"arxiv":1,"OA_type":"hybrid","volume":690,"article_number":"A217","department":[{"_id":"LiBu"}],"intvolume":"       690","das_tickbox":"1","publication_status":"published","abstract":[{"text":"The recent measurement of magnetic field strength inside the radiative interior of red giant stars has opened the way toward full 3D characterization of the geometry of stable large-scale magnetic fields. However, current measurements, which are limited to dipolar (ℓ = 1) mixed modes, do not properly constrain the topology of magnetic fields due to degeneracies on the observed magnetic field signature on such ℓ = 1 mode frequencies. Efforts focused toward unambiguous detections of magnetic field configurations are now key to better understand angular momentum transport in stars. We investigated the detectability of complex magnetic field topologies (such as the ones observed at the surface of stars with a radiative envelope with spectropolarimetry) inside the radiative interior of red giants. We focused on a field composed of a combination of a dipole and a quadrupole (quadrudipole) and on an offset field. We explored the potential of probing such magnetic field topologies from a combined measurement of magnetic signatures on ℓ = 1 and quadrupolar (ℓ = 2) mixed mode oscillation frequencies. We first derived the asymptotic theoretical formalism for computing the asymmetric signature in the frequency pattern for ℓ = 2 modes due to a quadrudipole magnetic field. To access asymmetry parameters for more complex magnetic field topologies, we numerically performed a grid search over the parameter space to map the degeneracy of the signatures of given topologies. We demonstrate the crucial role played by ℓ = 2 mixed modes in accessing internal magnetic fields with a quadrupolar component. The degeneracy of the quadrudipole compared to pure dipolar fields is lifted when considering magnetic asymmetries in both ℓ = 1 and ℓ = 2 mode frequencies. In addition to the analytical derivation for the quadrudipole, we present the prospect for complex magnetic field inversions using magnetic sensitivity kernels from standard perturbation analysis for forward modeling. Using this method, we explored the detectability of offset magnetic fields from ℓ = 1 and ℓ = 2 frequencies and demonstrate that offset fields may be mistaken for weak and centered magnetic fields, resulting in underestimating the magnetic field strength in stellar cores. We emphasize the need to characterize ℓ = 2 mixed-mode frequencies, (along with the currently characterized ℓ = 1 mixed modes), to unveil the higher-order components of the geometry of buried magnetic fields and to better constrain angular momentum transport inside stars.","lang":"eng"}],"file":[{"file_id":"18534","creator":"dernst","access_level":"open_access","file_name":"2024_AstronomyAstrophysics_Das.pdf","date_created":"2024-11-11T09:01:11Z","content_type":"application/pdf","success":1,"relation":"main_file","file_size":5306256,"date_updated":"2024-11-11T09:01:11Z","checksum":"d43bbe6ed8ce4512e65e2d0d87070cf6"}],"status":"public","isi":1,"article_processing_charge":"No","external_id":{"arxiv":["2405.20133"],"isi":["001336485200015"]},"ddc":["520"],"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"project":[{"grant_number":"101034413","call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","name":"IST-BRIDGE: International postdoctoral program"}],"month":"10","date_created":"2024-11-10T23:02:00Z","oa_version":"Published Version","publisher":"EDP Sciences","date_published":"2024-10-01T00:00:00Z","language":[{"iso":"eng"}],"type":"journal_article","file_date_updated":"2024-11-11T09:01:11Z","doi":"10.1051/0004-6361/202450918","date_updated":"2026-07-08T06:44:58Z","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png"},"article_type":"original","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","corr_author":"1","_id":"18528","OA_place":"publisher","author":[{"last_name":"Das","first_name":"Srijan B","full_name":"Das, Srijan B","orcid":"0000-0003-0896-7972","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149"},{"first_name":"Lukas","full_name":"Einramhof, Lukas","last_name":"Einramhof","id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000"}],"acknowledgement":"The authors thank S. Mathis, L. Barrault, S. Torres, A. Cristea, and K. M. Smith for very useful discussions. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curíe grant agreement No 101034413. The authors thank the anonymous referee for valuable comments and suggestions to improve the manuscript.","citation":{"ista":"Das SB, Einramhof L, Bugnet LA. 2024. Unveiling complex magnetic field configurations in red giant stars. Astronomy &#38; Astrophysics. 690, A217.","ama":"Das SB, Einramhof L, Bugnet LA. Unveiling complex magnetic field configurations in red giant stars. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450918\">10.1051/0004-6361/202450918</a>","chicago":"Das, Srijan B, Lukas Einramhof, and Lisa Annabelle Bugnet. “Unveiling Complex Magnetic Field Configurations in Red Giant Stars.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202450918\">https://doi.org/10.1051/0004-6361/202450918</a>.","apa":"Das, S. B., Einramhof, L., &#38; Bugnet, L. A. (2024). Unveiling complex magnetic field configurations in red giant stars. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450918\">https://doi.org/10.1051/0004-6361/202450918</a>","mla":"Das, Srijan B., et al. “Unveiling Complex Magnetic Field Configurations in Red Giant Stars.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A217, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450918\">10.1051/0004-6361/202450918</a>.","short":"S.B. Das, L. Einramhof, L.A. Bugnet, Astronomy &#38; Astrophysics 690 (2024).","ieee":"S. B. Das, L. Einramhof, and L. A. Bugnet, “Unveiling complex magnetic field configurations in red giant stars,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024."}}]