[{"date_updated":"2026-07-22T06:20:53Z","citation":{"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>.","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>","short":"J. Mombarg, V. Vanlaer, S.B. Das, M. Rieutord, C. Aerts, L.A. Bugnet, S. Mathis, D. Reese, J. Ballot, (2025).","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>","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>.","ieee":"J. Mombarg <i>et al.</i>, “Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?” Zenodo, 2025."},"main_file_link":[{"url":"https://doi.org/10.5281/zenodo.17580178","open_access":"1"}],"date_created":"2026-01-05T08:39:33Z","department":[{"_id":"LiBu"}],"date_published":"2025-11-11T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_place":"repository","title":"Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?","month":"11","publisher":"Zenodo","related_material":{"record":[{"id":"20931","relation":"used_in_publication","status":"public"}]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"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)"}],"author":[{"last_name":"Mombarg","full_name":"Mombarg, Joey","first_name":"Joey"},{"full_name":"Vanlaer, Vincent","first_name":"Vincent","last_name":"Vanlaer"},{"last_name":"Das","full_name":"Das, Srijan B","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","first_name":"Srijan B","orcid":"0000-0003-0896-7972"},{"last_name":"Rieutord","full_name":"Rieutord, Michel","first_name":"Michel"},{"last_name":"Aerts","full_name":"Aerts, Conny","first_name":"Conny"},{"last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"},{"last_name":"Mathis","first_name":"Stephane","full_name":"Mathis, Stephane"},{"last_name":"Reese","full_name":"Reese, Daniel","first_name":"Daniel"},{"first_name":"Jerome","full_name":"Ballot, Jerome","last_name":"Ballot"}],"type":"research_data_reference","oa":1,"article_processing_charge":"No","OA_type":"gold","status":"public","ddc":["520"],"doi":"10.5281/ZENODO.17580178","fulldoi":"https://doi.org/10.5281/ZENODO.17580178","oa_version":"Published Version","year":"2025","_id":"20936","day":"11"},{"researchdata_availability":"yes","publication":"Astrophysical Journal","volume":970,"year":"2024","intvolume":"       970","status":"public","ddc":["520"],"quality_controlled":"1","scopus_import":"1","DOAJ_listed":"1","abstract":[{"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.","lang":"eng"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"author":[{"first_name":"Shatanik","full_name":"Bhattacharya, Shatanik","last_name":"Bhattacharya"},{"full_name":"Das, Srijan B","orcid":"0000-0003-0896-7972","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","first_name":"Srijan B","last_name":"Das"},{"last_name":"Bugnet","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"Panda, Subrata","first_name":"Subrata","last_name":"Panda"},{"last_name":"Hanasoge","full_name":"Hanasoge, Shravan M.","first_name":"Shravan M."}],"oa":1,"file_date_updated":"2024-07-29T11:02:48Z","publisher":"IOP Publishing","supplementarymaterial":"yes","month":"07","date_published":"2024-07-15T00:00:00Z","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.","date_created":"2024-07-28T22:01:09Z","ec_funded":1,"department":[{"_id":"LiBu"}],"date_updated":"2026-10-16T08:51:03Z","das_tickbox":"0","file":[{"relation":"main_file","content_type":"application/pdf","file_size":3912290,"file_id":"17340","creator":"dernst","access_level":"open_access","date_updated":"2024-07-29T11:02:48Z","checksum":"acb42a87deecbc9228fbbe6a48a37ec6","date_created":"2024-07-29T11:02:48Z","success":1,"file_name":"2024_AstrophysicalJourn_Bhattacharya.pdf"}],"doi":"10.3847/1538-4357/ad4708","language":[{"iso":"eng"}],"fulldoi":"https://doi.org/10.3847/1538-4357/ad4708","oa_version":"Published Version","_id":"17326","day":"15","article_processing_charge":"Yes","project":[{"call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413"}],"has_accepted_license":"1","type":"journal_article","issue":"1","arxiv":1,"isi":1,"article_type":"original","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publication_status":"published","external_id":{"arxiv":["2404.17167"],"isi":["001270972500001"]},"title":"Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_number":"42","citation":{"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.","short":"S. Bhattacharya, S.B. Das, L.A. Bugnet, S. Panda, S.M. Hanasoge, Astrophysical Journal 970 (2024).","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>","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.","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>"}},{"doi":"10.1093/mnras/stae2053","fulldoi":"https://doi.org/10.1093/mnras/stae2053","oa_version":"Published Version","language":[{"iso":"eng"}],"day":"01","_id":"18172","article_processing_charge":"Yes","has_accepted_license":"1","type":"journal_article","issue":"2","arxiv":1,"isi":1,"page":"1060-1076","article_type":"original","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","external_id":{"isi":["001320536900011"],"arxiv":["2409.01157"]},"title":"Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","citation":{"ama":"Hatt EJ, Ong JMJ, Nielsen MB, et al. Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;534(2):1060-1076. doi:<a href=\"https://doi.org/10.1093/mnras/stae2053\">10.1093/mnras/stae2053</a>","short":"E.J. Hatt, J.M.J. Ong, M.B. Nielsen, W.J. Chaplin, G.R. Davies, S. Deheuvels, J. Ballot, G. Li, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 534 (2024) 1060–1076.","ieee":"E. J. Hatt <i>et al.</i>, “Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 2. Oxford University Press, pp. 1060–1076, 2024.","mla":"Hatt, Emily J., et al. “Asteroseismic Signatures of Core Magnetism and Rotation in Hundreds of Low-Luminosity Red Giants.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 2, Oxford University Press, 2024, pp. 1060–76, doi:<a href=\"https://doi.org/10.1093/mnras/stae2053\">10.1093/mnras/stae2053</a>.","apa":"Hatt, E. J., Ong, J. M. J., Nielsen, M. B., Chaplin, W. J., Davies, G. R., Deheuvels, S., … Bugnet, L. A. (2024). Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2053\">https://doi.org/10.1093/mnras/stae2053</a>","chicago":"Hatt, Emily J., J. M.Joel Ong, Martin B. Nielsen, William J. Chaplin, Guy R. Davies, Sébastien Deheuvels, Jérôme Ballot, Gang Li, and Lisa Annabelle Bugnet. “Asteroseismic Signatures of Core Magnetism and Rotation in Hundreds of Low-Luminosity Red Giants.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae2053\">https://doi.org/10.1093/mnras/stae2053</a>.","ista":"Hatt EJ, Ong JMJ, Nielsen MB, Chaplin WJ, Davies GR, Deheuvels S, Ballot J, Li G, Bugnet LA. 2024. Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. Monthly Notices of the Royal Astronomical Society. 534(2), 1060–1076."},"researchdata_availability":"yes","publication":"Monthly Notices of the Royal Astronomical Society","year":"2024","volume":534,"intvolume":"       534","OA_type":"gold","quality_controlled":"1","ddc":["520"],"status":"public","PlanS_conform":"1","scopus_import":"1","DOAJ_listed":"1","abstract":[{"text":"Red Giant stars host solar-like oscillations which have mixed character, being sensitive to conditions both in the outer convection zone and deep within the interior. The properties of these modes are sensitive to both core rotation and magnetic fields. While asteroseismic studies of the former have been done on a large scale, studies of the latter are currently limited to tens of stars. We aim to produce the first large catalogue of both magnetic and rotational perturbations. We jointly constrain these parameters by devising an automated method for fitting the power spectra directly. We successfully apply the method to 302 low-luminosity red giants. We find a clear bimodality in core rotation rate. The primary peak is at δνrot = 0.32 μHz, and the secondary at δνrot = 0.47 μHz. Combining our results with literature values, we find that the percentage of stars rotating much more rapidly than the population average increases with evolutionary state. We measure magnetic splittings of 2σ significance in 23 stars. While the most extreme magnetic splitting values appear in stars with masses > 1.1M⊙, implying they formerly hosted a convective core, a small but statistically significant magnetic splitting is measured at lower masses. Asymmetry between the frequencies of a rotationally split multiplet has previously been used to diagnose the presence of a magnetic perturbation. We find that of the stars with a significant detection of magnetic perturbation, 43\\% do not show strong asymmetry. We find no strong evidence of correlation between the rotation and magnetic parameters.","lang":"eng"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"author":[{"last_name":"Hatt","first_name":"Emily J.","full_name":"Hatt, Emily J."},{"last_name":"Ong","first_name":"J. M.Joel","full_name":"Ong, J. M.Joel"},{"full_name":"Nielsen, Martin B.","first_name":"Martin B.","last_name":"Nielsen"},{"last_name":"Chaplin","full_name":"Chaplin, William J.","first_name":"William J."},{"last_name":"Davies","first_name":"Guy R.","full_name":"Davies, Guy R."},{"last_name":"Deheuvels","first_name":"Sébastien","full_name":"Deheuvels, Sébastien"},{"last_name":"Ballot","full_name":"Ballot, Jérôme","first_name":"Jérôme"},{"last_name":"Li","first_name":"Gang","full_name":"Li, Gang"},{"first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"}],"file_date_updated":"2024-10-07T09:14:03Z","oa":1,"publisher":"Oxford University Press","supplementarymaterial":"yes","OA_place":"publisher","month":"10","date_published":"2024-10-01T00:00:00Z","dataavailabilitystatement":"Table 1 is available at the CDS. Light curves used in this work are available at Mikulski Archive for Space Telescopes at the Space Telescope Science Institute (MAST)1. Other intermediate data products will be made available upon reasonable request.","date_created":"2024-10-06T22:01:11Z","acknowledgement":"EJH, WJC, and GRD acknowledge the support of Science and Technology Facilities Council. MBN acknowledges support from the UK Space Agency. JMJO acknowledges support from NASA through the NASA Hubble Fellowship grant HST-HF2-51517.001, awarded by STScI (Space Telescope Science Institute), which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The authors acknowledge use of the Blue-BEAR HPC service at the University of Birmingham. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission was provided by the NASA Science Mission Directorate. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/web/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC was provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (CartographY GA. 804752). SD and JB acknowledge support from the Centre National d’Etudes Spatiales (CNES).","department":[{"_id":"LiBu"}],"date_updated":"2026-10-16T08:52:08Z","das_tickbox":"1","file":[{"relation":"main_file","content_type":"application/pdf","file_id":"18182","file_size":2813008,"creator":"dernst","date_updated":"2024-10-07T09:14:03Z","access_level":"open_access","success":1,"date_created":"2024-10-07T09:14:03Z","file_name":"2024_MonthlyNRoyalAstronSoc_Hatt.pdf","checksum":"b79f3c6a5991516abbcc8d34fa4bfb5f"}]},{"publisher":"EDP Sciences","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"abstract":[{"text":"The Planetary Transits and Oscillations of stars mission (PLATO) will allow us to measure surface rotation and monitor photometric activity of tens of thousands of main sequence solar-type and subgiant stars. This paper is the first of a series dedicated to the preparation of the analysis of stellar surface rotation and photospheric activity with the near-future PLATO data. We describe in this work the strategy that will be implemented in the PLATO pipeline to measure stellar surface rotation, photometric activity, and long-term modulations. The algorithms are applied on both noise-free and noisy simulations of solar-type stars, which include activity cycles, latitudinal differential rotation, and spot evolution. PLATO simulated systematics are included in the noisy light curves. We show that surface rotation periods can be recovered with confidence for most of the stars with only six months of observations and that the recovery rate of the analysis significantly improves as additional observations are collected. This means that the first PLATO data release will already provide a substantial set of measurements for this quantity, with a significant refinement on their quality as the instrument obtains longer light curves. Measuring the Schwabe-like magnetic activity cycle during the mission will require that the same field be observed over a significant timescale (more than four years). Nevertheless, PLATO will provide a vast and robust sample of solar-type stars with constraints on the activity-cycle length. Such a sample is lacking from previous missions dedicated to space photometry.","lang":"eng"}],"author":[{"full_name":"Breton, S. N.","first_name":"S. N.","last_name":"Breton"},{"first_name":"A. F.","full_name":"Lanza, A. F.","last_name":"Lanza"},{"full_name":"Messina, S.","first_name":"S.","last_name":"Messina"},{"last_name":"Pagano","first_name":"I.","full_name":"Pagano, I."},{"orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"},{"first_name":"E.","full_name":"Corsaro, E.","last_name":"Corsaro"},{"full_name":"García, R. A.","first_name":"R. A.","last_name":"García"},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"last_name":"Santos","first_name":"A. R. G.","full_name":"Santos, A. R. G."},{"first_name":"S.","full_name":"Aigrain, S.","last_name":"Aigrain"},{"last_name":"Amard","full_name":"Amard, L.","first_name":"L."},{"last_name":"Brun","full_name":"Brun, A. S.","first_name":"A. S."},{"first_name":"L.","full_name":"Degott, L.","last_name":"Degott"},{"first_name":"Q.","full_name":"Noraz, Q.","last_name":"Noraz"},{"full_name":"Palakkatharappil, D. B.","first_name":"D. B.","last_name":"Palakkatharappil"},{"full_name":"Panetier, E.","first_name":"E.","last_name":"Panetier"},{"last_name":"Strugarek","full_name":"Strugarek, A.","first_name":"A."},{"last_name":"Belkacem","first_name":"K.","full_name":"Belkacem, K."},{"last_name":"Goupil","full_name":"Goupil, M.-J","first_name":"M.-J"},{"last_name":"Ouazzani","full_name":"Ouazzani, R. M.","first_name":"R. M."},{"first_name":"J.","full_name":"Philidet, J.","last_name":"Philidet"},{"full_name":"Renié, C.","first_name":"C.","last_name":"Renié"},{"last_name":"Roth","first_name":"O.","full_name":"Roth, O."}],"oa":1,"file_date_updated":"2025-01-27T13:18:41Z","intvolume":"       689","quality_controlled":"1","ddc":["520"],"OA_type":"hybrid","status":"public","scopus_import":"1","researchdata_availability":"yes","publication":"Astronomy & Astrophysics","year":"2024","volume":689,"date_updated":"2026-10-16T08:55:46Z","das_tickbox":"0","file":[{"success":1,"date_created":"2025-01-27T13:18:41Z","file_name":"2024_AstronomyAstrophysics_Breton.pdf","checksum":"5c871ba7370a507ed6ea9fb2304d8263","creator":"dernst","date_updated":"2025-01-27T13:18:41Z","access_level":"open_access","file_id":"18905","file_size":6212007,"content_type":"application/pdf","relation":"main_file"}],"date_created":"2025-01-27T13:12:44Z","acknowledgement":"This work presents results from the European Space Agency (ESA) space mission PLATO. The PLATO payload, the PLATO Ground Segment and PLATO data processing are joint developments of ESA and the PLATO Mission Consortium (PMC). Funding for the PMC is provided at national levels, in particular by countries participating in the PLATO Multilateral Agreement (Austria, Belgium, Czech Republic, Denmark, France, Germany, Italy, Netherlands, Portugal, Spain, Sweden, Switzerland, Norway, and United Kingdom) and institutions from Brazil. Members of the PLATO Consortium can be found at https://platomission.com. The ESA PLATO mission website is https://www.cosmos.esa.int/plato. The authors thank the teams working for PLATO for all their work. They acknowledge the critical reading and the constructive comments from the anonymous referee that significantly allowed improving the original version of this paper. They finally thank R. Samadi for helpful advice and suggestions concerning the PSLS abilities. S.N.B, A.F.L, S.Me, I.P and E.C acknowledge support from PLATO ASI-INAF agreement no. 2022-28-HH.0 “PLATO Fase D”. S.N.B, L.A, A.S.B, Q.N, and A.S acknowledge financial support by ERC Whole Sun Synergy grant #810218. S.N.B, R.A.G, L.A, A.S.B, Q.N., D.B.P, E.P, and A.S acknowledge the support from PLATO CNES grant. R.A.G, D.B.P, and E.P acknowledge the support from SoHO/GOLF CNES grant. A.S.B, Q.N, and A.S acknowledge the support from INSU/PNST grant and Solar Orbiter CNES grant. A.S acknowledges funding from from the European Union’s Horizon-2020 research and innovation program (grant agreement no. 776403 ExoplANETS-A) and the Programme National de Planétologie (PNP). A.R.G.S acknowledges the support from the FCT through national funds and FEDER through COMPETE2020 (UIDB/04434/2020, UIDP/04434/2020, 2022.03993.PTDC) and the support from the FCT through the work contract No. 2020.02480.CEECIND/CP1631/CT0001. S.Ma acknowledges support from the Spanish Ministry of Science and Innovation (MICINN) with the Ramón y Cajal fellowship no. RYC-2015-17697 and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). S.Ma acknowledges support from the Spanish Ministry of Science and Innovation (MICINN) with the grant no. PID2019-107187GB-I00. M.J.G., K.B., R.M.O, J.P, O.R., C.R. acknowledge support from CNES. The computations were performed with the IRFU/CEA Saclay server facilities, funded by ERC Synergy grant WholeSun No.810218, the P2IO Labex emergence project FlarePredict, and CNES PLATO funds. Software:star-privateer (this work), pyspot (Aigrain et al. 2015), PSLS (Samadi et al. 2019), numpy (Harris et al. 2020), matplotlib (Hunter 2007), scipy (Virtanen et al. 2020), astropy (Astropy Collaboration 2022), pandas (Wes McKinney 2010; The pandas development team 2020), scikit-learn (Pedregosa et al. 2011).","department":[{"_id":"LiBu"}],"date_published":"2024-09-01T00:00:00Z","OA_place":"publisher","supplementarymaterial":"yes","month":"09","arxiv":1,"isi":1,"article_type":"original","has_accepted_license":"1","type":"journal_article","article_processing_charge":"No","doi":"10.1051/0004-6361/202449893","fulldoi":"https://doi.org/10.1051/0004-6361/202449893","language":[{"iso":"eng"}],"oa_version":"Published Version","_id":"18904","day":"01","citation":{"apa":"Breton, S. N., Lanza, A. F., Messina, S., Pagano, I., Bugnet, L. A., Corsaro, E., … Roth, O. (2024). Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202449893\">https://doi.org/10.1051/0004-6361/202449893</a>","ama":"Breton SN, Lanza AF, Messina S, et al. Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves. <i>Astronomy &#38; Astrophysics</i>. 2024;689. doi:<a href=\"https://doi.org/10.1051/0004-6361/202449893\">10.1051/0004-6361/202449893</a>","short":"S.N. Breton, A.F. Lanza, S. Messina, I. Pagano, L.A. Bugnet, E. Corsaro, R.A. García, S. Mathur, A.R.G. Santos, S. Aigrain, L. Amard, A.S. Brun, L. Degott, Q. Noraz, D.B. Palakkatharappil, E. Panetier, A. Strugarek, K. Belkacem, M.-J. Goupil, R.M. Ouazzani, J. Philidet, C. Renié, O. Roth, Astronomy &#38; Astrophysics 689 (2024).","ieee":"S. N. Breton <i>et al.</i>, “Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves,” <i>Astronomy &#38; Astrophysics</i>, vol. 689. EDP Sciences, 2024.","mla":"Breton, S. N., et al. “Measuring Stellar Surface Rotation and Activity with the PLATO Mission. I. Strategy and Application to Simulated Light Curves.” <i>Astronomy &#38; Astrophysics</i>, vol. 689, A229, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202449893\">10.1051/0004-6361/202449893</a>.","chicago":"Breton, S. N., A. F. Lanza, S. Messina, I. Pagano, Lisa Annabelle Bugnet, E. Corsaro, R. A. García, et al. “Measuring Stellar Surface Rotation and Activity with the PLATO Mission. I. Strategy and Application to Simulated Light Curves.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202449893\">https://doi.org/10.1051/0004-6361/202449893</a>.","ista":"Breton SN, Lanza AF, Messina S, Pagano I, Bugnet LA, Corsaro E, García RA, Mathur S, Santos ARG, Aigrain S, Amard L, Brun AS, Degott L, Noraz Q, Palakkatharappil DB, Panetier E, Strugarek A, Belkacem K, Goupil M-J, Ouazzani RM, Philidet J, Renié C, Roth O. 2024. Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves. Astronomy &#38; Astrophysics. 689, A229."},"article_number":"A229","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_status":"published","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"external_id":{"arxiv":["2407.03709"],"isi":["001366206400007"]},"title":"Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves"},{"date_updated":"2026-10-16T08:52:49Z","das_tickbox":"1","file":[{"creator":"dernst","date_updated":"2024-10-21T11:05:11Z","access_level":"open_access","success":1,"file_name":"2024_AstrophysicalJourn_Oza.pdf","date_created":"2024-10-21T11:05:11Z","checksum":"23eea2a6a0519694a84998957ad7b7fb","content_type":"application/pdf","relation":"main_file","file_id":"18456","file_size":1249747}],"date_created":"2024-10-13T22:01:49Z","acknowledgement":"The research described in this Letter was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics Space Administration, © 2024. California Institute of Technology. Government sponsorship acknowledged. A.V.O. and J.V.S. thank M. Lendl for constraints and discussions on the mass of WASP-49 A b. S.G.S acknowledges the support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC).","department":[{"_id":"LiBu"}],"date_published":"2024-10-01T00:00:00Z","dataavailabilitystatement":"ESO data is available publicly on ESO’s science archive facility at archive.eso.org/eso/eso_archive_main.html.","OA_place":"publisher","supplementarymaterial":"no","month":"10","publisher":"IOP Publishing","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"abstract":[{"lang":"eng","text":"Neutral sodium (Na i) is an alkali metal with a favorable absorption cross section such that tenuous gases are easily illuminated at select transiting exoplanet systems. We examine both the time-averaged and time-series alkali spectral flux individually, over 4 nights at a hot Saturn system on a ∼2.8 day orbit about a Sun-like star WASP-49 A. Very Large Telescope/ESPRESSO observations are analyzed, providing new constraints. We recover the previously confirmed residual sodium flux uniquely when averaged, whereas night-to-night Na i varies by more than an order of magnitude. On HARPS/3.6 m Epoch II, we report a Doppler redshift at vΓ,NaD = + 9.7 ± 1.6 km s−1 with respect to the planet's rest frame. Upon examining the lightcurves, we confirm night-to-night variability, on the order of ∼1%–4% in NaD, rarely coinciding with exoplanet transit, not readily explained by stellar activity, starspots, tellurics, or the interstellar medium. Coincident with the ∼+10 km s−1 Doppler redshift, we detect a transient sodium absorption event dFNaD/F⋆ = 3.6% ± 1% at a relative difference of ΔFNaD(t) ∼ 4.4% ± 1%, lasting ΔtNaD ≳ 40 minutes. Since exoplanetary alkali signatures are blueshifted due to the natural vector of radiation pressure, estimated here at roughly ∼−5.7 km s−1, the radial velocity is rather at +15.4 km s−1, far larger than any known exoplanet system. Given that the redshift magnitude vΓ is in between the Roche limit and dynamically stable satellite orbits, the transient sodium may be a putative indication of a natural satellite orbiting WASP-49 A b."}],"author":[{"full_name":"Oza, Apurva V.","first_name":"Apurva V.","last_name":"Oza"},{"last_name":"Seidel","full_name":"Seidel, Julia V.","first_name":"Julia V."},{"first_name":"H. Jens","full_name":"Hoeijmakers, H. Jens","last_name":"Hoeijmakers"},{"full_name":"Unni, Athira","first_name":"Athira","last_name":"Unni"},{"first_name":"Aurora Y.","full_name":"Kesseli, Aurora Y.","last_name":"Kesseli"},{"last_name":"Schmidt","full_name":"Schmidt, Carl A.","first_name":"Carl A."},{"first_name":"Thirupathi","full_name":"Sivarani, Thirupathi","last_name":"Sivarani"},{"full_name":"Bello-Arufe, Aaron","first_name":"Aaron","last_name":"Bello-Arufe"},{"last_name":"Gebek","full_name":"Gebek, Andrea","first_name":"Andrea"},{"last_name":"Meyer Zu Westram","first_name":"Moritz","full_name":"Meyer Zu Westram, Moritz"},{"full_name":"Sousa, Sérgio G.","first_name":"Sérgio G.","last_name":"Sousa"},{"last_name":"Lopes","first_name":"Rosaly M.C.","full_name":"Lopes, Rosaly M.C."},{"first_name":"Renyu","full_name":"Hu, Renyu","last_name":"Hu"},{"last_name":"De Kleer","full_name":"De Kleer, Katherine","first_name":"Katherine"},{"first_name":"Chloe","full_name":"Fisher, Chloe","last_name":"Fisher"},{"first_name":"Sébastien","full_name":"Charnoz, Sébastien","last_name":"Charnoz"},{"full_name":"Baker, Ashley D.","first_name":"Ashley D.","last_name":"Baker"},{"full_name":"Halverson, Samuel P.","first_name":"Samuel P.","last_name":"Halverson"},{"first_name":"Nick M.","full_name":"Schneider, Nick M.","last_name":"Schneider"},{"first_name":"Angelica","full_name":"Psaridi, Angelica","last_name":"Psaridi"},{"full_name":"Wyttenbach, Aurélien","first_name":"Aurélien","last_name":"Wyttenbach"},{"last_name":"Torres Rodriguez","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2","first_name":"Santiago","orcid":"0000-0002-3150-8988","full_name":"Torres Rodriguez, Santiago"},{"full_name":"Bhatnagar, Ishita","first_name":"Ishita","last_name":"Bhatnagar"},{"last_name":"Johnson","first_name":"Robert E.","full_name":"Johnson, Robert E."}],"file_date_updated":"2024-10-21T11:05:11Z","oa":1,"intvolume":"       973","quality_controlled":"1","ddc":["520"],"status":"public","OA_type":"gold","scopus_import":"1","DOAJ_listed":"1","researchdata_availability":"yes","publication":"Astrophysical Journal Letters","volume":973,"year":"2024","citation":{"apa":"Oza, A. V., Seidel, J. V., Hoeijmakers, H. J., Unni, A., Kesseli, A. Y., Schmidt, C. A., … Johnson, R. E. (2024). Redshifted sodium transient near exoplanet transit. <i>Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad6b29\">https://doi.org/10.3847/2041-8213/ad6b29</a>","ama":"Oza AV, Seidel JV, Hoeijmakers HJ, et al. Redshifted sodium transient near exoplanet transit. <i>Astrophysical Journal Letters</i>. 2024;973(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad6b29\">10.3847/2041-8213/ad6b29</a>","short":"A.V. Oza, J.V. Seidel, H.J. Hoeijmakers, A. Unni, A.Y. Kesseli, C.A. Schmidt, T. Sivarani, A. Bello-Arufe, A. Gebek, M. Meyer Zu Westram, S.G. Sousa, R.M.C. Lopes, R. Hu, K. De Kleer, C. Fisher, S. Charnoz, A.D. Baker, S.P. Halverson, N.M. Schneider, A. Psaridi, A. Wyttenbach, S. Torres Rodriguez, I. Bhatnagar, R.E. Johnson, Astrophysical Journal Letters 973 (2024).","mla":"Oza, Apurva V., et al. “Redshifted Sodium Transient near Exoplanet Transit.” <i>Astrophysical Journal Letters</i>, vol. 973, no. 2, L53, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad6b29\">10.3847/2041-8213/ad6b29</a>.","ieee":"A. V. Oza <i>et al.</i>, “Redshifted sodium transient near exoplanet transit,” <i>Astrophysical Journal Letters</i>, vol. 973, no. 2. IOP Publishing, 2024.","chicago":"Oza, Apurva V., Julia V. Seidel, H. Jens Hoeijmakers, Athira Unni, Aurora Y. Kesseli, Carl A. Schmidt, Thirupathi Sivarani, et al. “Redshifted Sodium Transient near Exoplanet Transit.” <i>Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad6b29\">https://doi.org/10.3847/2041-8213/ad6b29</a>.","ista":"Oza AV, Seidel JV, Hoeijmakers HJ, Unni A, Kesseli AY, Schmidt CA, Sivarani T, Bello-Arufe A, Gebek A, Meyer Zu Westram M, Sousa SG, Lopes RMC, Hu R, De Kleer K, Fisher C, Charnoz S, Baker AD, Halverson SP, Schneider NM, Psaridi A, Wyttenbach A, Torres Rodriguez S, Bhatnagar I, Johnson RE. 2024. Redshifted sodium transient near exoplanet transit. Astrophysical Journal Letters. 973(2), L53."},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_number":"L53","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"publication_status":"published","external_id":{"isi":["001322169500001"],"arxiv":["2409.19844"]},"title":"Redshifted sodium transient near exoplanet transit","issue":"2","arxiv":1,"isi":1,"article_type":"original","has_accepted_license":"1","type":"journal_article","article_processing_charge":"Yes","doi":"10.3847/2041-8213/ad6b29","fulldoi":"https://doi.org/10.3847/2041-8213/ad6b29","oa_version":"Published Version","language":[{"iso":"eng"}],"_id":"18306","day":"01"},{"citation":{"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>.","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.","short":"S.B. Das, L. Einramhof, L.A. Bugnet, Astronomy &#38; Astrophysics 690 (2024).","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>","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>","ista":"Das SB, Einramhof L, Bugnet LA. 2024. Unveiling complex magnetic field configurations in red giant stars. Astronomy &#38; Astrophysics. 690, A217.","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>."},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_number":"A217","title":"Unveiling complex magnetic field configurations in red giant stars","external_id":{"isi":["001336485200015"],"arxiv":["2405.20133"]},"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"publication_status":"published","article_type":"original","isi":1,"arxiv":1,"related_material":{"record":[{"id":"22802","status":"public","relation":"research_data"}]},"type":"journal_article","has_accepted_license":"1","project":[{"grant_number":"101034413","name":"IST-BRIDGE: International postdoctoral program","call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"}],"article_processing_charge":"No","_id":"18528","day":"01","fulldoi":"https://doi.org/10.1051/0004-6361/202450918","language":[{"iso":"eng"}],"oa_version":"Published Version","doi":"10.1051/0004-6361/202450918","file":[{"file_size":5306256,"file_id":"18534","relation":"main_file","content_type":"application/pdf","checksum":"d43bbe6ed8ce4512e65e2d0d87070cf6","date_created":"2024-11-11T09:01:11Z","success":1,"file_name":"2024_AstronomyAstrophysics_Das.pdf","creator":"dernst","access_level":"open_access","date_updated":"2024-11-11T09:01:11Z"}],"das_tickbox":"1","date_updated":"2026-10-16T08:53:44Z","department":[{"_id":"LiBu"}],"ec_funded":1,"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.","date_created":"2024-11-10T23:02:00Z","dataavailabilitystatement":"The MESA inlist file is available at https://doi.org/10.5281/zenodo.12804810","date_published":"2024-10-01T00:00:00Z","month":"10","OA_place":"publisher","supplementarymaterial":"yes","publisher":"EDP Sciences","oa":1,"file_date_updated":"2024-11-11T09:01:11Z","author":[{"full_name":"Das, Srijan B","orcid":"0000-0003-0896-7972","first_name":"Srijan B","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","last_name":"Das"},{"full_name":"Einramhof, Lukas","first_name":"Lukas","id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c","last_name":"Einramhof"},{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet"}],"corr_author":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"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"}],"scopus_import":"1","status":"public","OA_type":"hybrid","quality_controlled":"1","ddc":["520"],"intvolume":"       690","year":"2024","volume":690,"publication":"Astronomy & Astrophysics","researchdata_availability":"yes"},{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Supergranular-scale solar convection not explained by mixing-length theory","external_id":{"isi":["001254181700001"]},"publication_identifier":{"eissn":["2397-3366"]},"publication_status":"published","citation":{"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>","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>","short":"C.S. Hanson, S.B. Das, P. Mani, S. Hanasoge, K.R. Sreenivasan, Nature Astronomy 8 (2024) 1088–1101.","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>.","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.","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>.","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."},"article_processing_charge":"No","_id":"17189","day":"01","language":[{"iso":"eng"}],"fulldoi":"https://doi.org/10.1038/s41550-024-02304-w","oa_version":"None","doi":"10.1038/s41550-024-02304-w","article_type":"original","page":"1088-1101","isi":1,"type":"journal_article","project":[{"name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","call_identifier":"H2020"}],"dataavailabilitystatement":"The HMI data are courtesy of NASA/SDO and the HMI Science Team. The HMI data are available from the Joint Science Operations Center export site http://jsoc.stanford.edu/. Due to the large volume of data, the mode-coupling products and kernels are available from the authors upon request. The numerical simulations are available upon request from M. Rempel.","date_published":"2024-09-01T00:00:00Z","month":"09","supplementarymaterial":"yes","das_tickbox":"1","date_updated":"2026-10-16T08:55:21Z","department":[{"_id":"LiBu"}],"ec_funded":1,"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).","date_created":"2024-06-30T22:01:05Z","scopus_import":"1","OA_type":"closed access","status":"public","quality_controlled":"1","intvolume":"         8","year":"2024","volume":8,"publication":"Nature Astronomy","researchdata_availability":"yes","publisher":"Springer Nature","author":[{"last_name":"Hanson","full_name":"Hanson, Chris S.","first_name":"Chris S."},{"orcid":"0000-0003-0896-7972","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","first_name":"Srijan B","full_name":"Das, Srijan B","last_name":"Das"},{"first_name":"Prasad","full_name":"Mani, Prasad","last_name":"Mani"},{"last_name":"Hanasoge","full_name":"Hanasoge, Shravan","first_name":"Shravan"},{"last_name":"Sreenivasan","first_name":"Katepalli R.","full_name":"Sreenivasan, Katepalli R."}],"abstract":[{"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.","lang":"eng"}]},{"related_material":{"record":[{"relation":"used_in_publication","status":"public","id":"18528"}]},"publisher":"Institute of Science and Technology Austria","author":[{"last_name":"Das","full_name":"Das, Srijan B","first_name":"Srijan B"},{"full_name":"Einramhof, Lukas","first_name":"Lukas","last_name":"Einramhof"},{"last_name":"Bugnet","full_name":"Bugnet, Lisa","first_name":"Lisa"}],"type":"research_data_reference","oa":1,"abstract":[{"text":"MESA inlist file for the paper \"Unveiling complex magnetic field configurations in red giant stars\" (10.1051/0004-6361/202450918)","lang":"eng"}],"ddc":["520"],"status":"public","OA_type":"green","article_processing_charge":"No","fulldoi":"https://doi.org/10.5281/zenodo.12804810","oa_version":"None","_id":"22802","day":"24","year":"2024","doi":"10.5281/zenodo.12804810","main_file_link":[{"open_access":"1","url":"https://doi.org/10.5281/zenodo.12804810"}],"date_updated":"2026-10-16T08:53:43Z","citation":{"chicago":"Das, Srijan B, Lukas Einramhof, and Lisa Bugnet. “MESA Inlist File.” Institute of Science and Technology Austria, 2024. <a href=\"https://doi.org/10.5281/zenodo.12804810\">https://doi.org/10.5281/zenodo.12804810</a>.","ista":"Das SB, Einramhof L, Bugnet L. 2024. MESA inlist file, Institute of Science and Technology Austria, <a href=\"https://doi.org/10.5281/zenodo.12804810\">10.5281/zenodo.12804810</a>.","ama":"Das SB, Einramhof L, Bugnet L. MESA inlist file. 2024. doi:<a href=\"https://doi.org/10.5281/zenodo.12804810\">10.5281/zenodo.12804810</a>","short":"S.B. Das, L. Einramhof, L. Bugnet, (2024).","mla":"Das, Srijan B., et al. <i>MESA Inlist File</i>. Institute of Science and Technology Austria, 2024, doi:<a href=\"https://doi.org/10.5281/zenodo.12804810\">10.5281/zenodo.12804810</a>.","ieee":"S. B. Das, L. Einramhof, and L. Bugnet, “MESA inlist file.” Institute of Science and Technology Austria, 2024.","apa":"Das, S. B., Einramhof, L., &#38; Bugnet, L. (2024). MESA inlist file. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.5281/zenodo.12804810\">https://doi.org/10.5281/zenodo.12804810</a>"},"department":[{"_id":"LiBu"}],"date_created":"2026-09-04T09:42:23Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_published":"2024-07-24T00:00:00Z","month":"07","title":"MESA inlist file","OA_place":"repository"},{"department":[{"_id":"LiBu"}],"date_created":"2023-08-02T07:30:43Z","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2307.03237","open_access":"1"}],"citation":{"ista":"Huber D, Pinsonneault M, Beck P, Bedding TR, Joss Bland-Hawthorn JB-H, Breton SN, Bugnet LA, Chaplin WJ, Garcia RA, Grunblatt SK, Guzik JA, Hekker S, Kawaler SD, Mathis S, Mathur S, Metcalfe T, Mosser B, Ness MK, Piro AL, Serenelli A, Sharma S, Soderblom DR, Stassun KG, Stello D, Tayar J, Belle GT van, Zinn JC. Asteroseismology with the Roman galactic bulge time-domain survey. arXiv, 2307.03237.","chicago":"Huber, Daniel, Marc Pinsonneault, Paul Beck, Timothy R. Bedding, Joss Bland-Hawthorn Joss Bland-Hawthorn, Sylvain N. Breton, Lisa Annabelle Bugnet, et al. “Asteroseismology with the Roman Galactic Bulge Time-Domain Survey.” <i>ArXiv</i>, n.d. <a href=\"https://doi.org/10.48550/arXiv.2307.03237\">https://doi.org/10.48550/arXiv.2307.03237</a>.","ieee":"D. Huber <i>et al.</i>, “Asteroseismology with the Roman galactic bulge time-domain survey,” <i>arXiv</i>. .","mla":"Huber, Daniel, et al. “Asteroseismology with the Roman Galactic Bulge Time-Domain Survey.” <i>ArXiv</i>, 2307.03237, doi:<a href=\"https://doi.org/10.48550/arXiv.2307.03237\">10.48550/arXiv.2307.03237</a>.","ama":"Huber D, Pinsonneault M, Beck P, et al. Asteroseismology with the Roman galactic bulge time-domain survey. <i>arXiv</i>. doi:<a href=\"https://doi.org/10.48550/arXiv.2307.03237\">10.48550/arXiv.2307.03237</a>","short":"D. Huber, M. Pinsonneault, P. Beck, T.R. Bedding, J.B.-H. Joss Bland-Hawthorn, S.N. Breton, L.A. Bugnet, W.J. Chaplin, R.A. Garcia, S.K. Grunblatt, J.A. Guzik, S. Hekker, S.D. Kawaler, S. Mathis, S. Mathur, T. Metcalfe, B. Mosser, M.K. Ness, A.L. Piro, A. Serenelli, S. Sharma, D.R. Soderblom, K.G. Stassun, D. Stello, J. Tayar, G.T. van Belle, J.C. Zinn, ArXiv (n.d.).","apa":"Huber, D., Pinsonneault, M., Beck, P., Bedding, T. R., Joss Bland-Hawthorn, J. B.-H., Breton, S. N., … Zinn, J. C. (n.d.). Asteroseismology with the Roman galactic bulge time-domain survey. <i>arXiv</i>. <a href=\"https://doi.org/10.48550/arXiv.2307.03237\">https://doi.org/10.48550/arXiv.2307.03237</a>"},"date_updated":"2023-08-02T07:36:00Z","month":"07","title":"Asteroseismology with the Roman galactic bulge time-domain survey","external_id":{"arxiv":["2307.03237"]},"publication_status":"submitted","article_number":"2307.03237","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_published":"2023-07-06T00:00:00Z","oa":1,"type":"preprint","author":[{"last_name":"Huber","full_name":"Huber, Daniel","first_name":"Daniel"},{"first_name":"Marc","full_name":"Pinsonneault, Marc","last_name":"Pinsonneault"},{"last_name":"Beck","full_name":"Beck, Paul","first_name":"Paul"},{"last_name":"Bedding","first_name":"Timothy R.","full_name":"Bedding, Timothy R."},{"first_name":"Joss Bland-Hawthorn","full_name":"Joss Bland-Hawthorn, Joss Bland-Hawthorn","last_name":"Joss Bland-Hawthorn"},{"last_name":"Breton","first_name":"Sylvain N.","full_name":"Breton, Sylvain N."},{"last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"Chaplin, William J.","first_name":"William J.","last_name":"Chaplin"},{"full_name":"Garcia, Rafael A.","first_name":"Rafael A.","last_name":"Garcia"},{"last_name":"Grunblatt","first_name":"Samuel K.","full_name":"Grunblatt, Samuel K."},{"last_name":"Guzik","full_name":"Guzik, Joyce A.","first_name":"Joyce A."},{"full_name":"Hekker, Saskia","first_name":"Saskia","last_name":"Hekker"},{"first_name":"Steven D.","full_name":"Kawaler, Steven D.","last_name":"Kawaler"},{"first_name":"Stephane","full_name":"Mathis, Stephane","last_name":"Mathis"},{"last_name":"Mathur","full_name":"Mathur, Savita","first_name":"Savita"},{"last_name":"Metcalfe","first_name":"Travis","full_name":"Metcalfe, Travis"},{"full_name":"Mosser, Benoit","first_name":"Benoit","last_name":"Mosser"},{"last_name":"Ness","first_name":"Melissa K.","full_name":"Ness, Melissa K."},{"full_name":"Piro, Anthony L.","first_name":"Anthony L.","last_name":"Piro"},{"first_name":"Aldo","full_name":"Serenelli, Aldo","last_name":"Serenelli"},{"last_name":"Sharma","first_name":"Sanjib","full_name":"Sharma, Sanjib"},{"last_name":"Soderblom","full_name":"Soderblom, David R.","first_name":"David R."},{"full_name":"Stassun, Keivan G.","first_name":"Keivan G.","last_name":"Stassun"},{"full_name":"Stello, Dennis","first_name":"Dennis","last_name":"Stello"},{"first_name":"Jamie","full_name":"Tayar, Jamie","last_name":"Tayar"},{"last_name":"Belle","full_name":"Belle, Gerard T. van","first_name":"Gerard T. van"},{"last_name":"Zinn","first_name":"Joel C.","full_name":"Zinn, Joel C."}],"abstract":[{"text":"Asteroseismology has transformed stellar astrophysics. Red giant asteroseismology is a prime example, with oscillation periods and amplitudes that are readily detectable with time-domain space-based telescopes. These oscillations can be used to infer masses, ages and radii for large numbers of stars, providing unique constraints on stellar populations in our galaxy. The cadence, duration, and spatial resolution of the Roman galactic bulge time-domain survey (GBTDS) are well-suited for asteroseismology and will probe an important population not studied by prior missions. We identify photometric precision as a key requirement for realizing the potential of asteroseismology with Roman. A precision of 1 mmag per 15-min cadence or better for saturated stars will enable detections of the populous red clump star population in the Galactic bulge. If the survey efficiency is better than expected, we argue for repeat observations of the same fields to improve photometric precision, or covering additional fields to expand the stellar population reach if the photometric precision for saturated stars is better than 1 mmag. Asteroseismology is relatively insensitive to the timing of the observations during the mission, and the prime red clump targets can be observed in a single 70 day campaign in any given field. Complementary stellar characterization, particularly astrometry tied to the Gaia system, will also dramatically expand the diagnostic power of asteroseismology. We also highlight synergies to Roman GBTDS exoplanet science using transits and microlensing.","lang":"eng"}],"arxiv":1,"_id":"13447","day":"06","year":"2023","oa_version":"Preprint","fulldoi":"https://doi.org/10.48550/arXiv.2307.03237","language":[{"iso":"eng"}],"publication":"arXiv","doi":"10.48550/arXiv.2307.03237","status":"public","article_processing_charge":"No"},{"citation":{"ieee":"S. Mathur <i>et al.</i>, “Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations,” <i>The Astrophysical Journal</i>, vol. 952, no. 2. IOP Publishing, 2023.","mla":"Mathur, Savita, et al. “Magnetic Activity Evolution of Solar-like Stars. I. Sph–Age Relation Derived from Kepler Observations.” <i>The Astrophysical Journal</i>, vol. 952, no. 2, 131, IOP Publishing, 2023, doi:<a href=\"https://doi.org/10.3847/1538-4357/acd118\">10.3847/1538-4357/acd118</a>.","short":"S. Mathur, Z.R. Claytor, Â.R.G. Santos, R.A. García, L. Amard, L.A. Bugnet, E. Corsaro, A. Bonanno, S.N. Breton, D. Godoy-Rivera, M.H. Pinsonneault, J. van Saders, The Astrophysical Journal 952 (2023).","ama":"Mathur S, Claytor ZR, Santos ÂRG, et al. Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations. <i>The Astrophysical Journal</i>. 2023;952(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/acd118\">10.3847/1538-4357/acd118</a>","apa":"Mathur, S., Claytor, Z. R., Santos, Â. R. G., García, R. A., Amard, L., Bugnet, L. A., … van Saders, J. (2023). Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/acd118\">https://doi.org/10.3847/1538-4357/acd118</a>","ista":"Mathur S, Claytor ZR, Santos ÂRG, García RA, Amard L, Bugnet LA, Corsaro E, Bonanno A, Breton SN, Godoy-Rivera D, Pinsonneault MH, van Saders J. 2023. Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations. The Astrophysical Journal. 952(2), 131.","chicago":"Mathur, Savita, Zachary R. Claytor, Ângela R. G. Santos, Rafael A. García, Louis Amard, Lisa Annabelle Bugnet, Enrico Corsaro, et al. “Magnetic Activity Evolution of Solar-like Stars. I. Sph–Age Relation Derived from Kepler Observations.” <i>The Astrophysical Journal</i>. IOP Publishing, 2023. <a href=\"https://doi.org/10.3847/1538-4357/acd118\">https://doi.org/10.3847/1538-4357/acd118</a>."},"publication_status":"published","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"external_id":{"isi":["001034185700001"]},"title":"Magnetic activity evolution of solar-like stars. I. Sph–age relation derived from Kepler observations","article_number":"131","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","type":"journal_article","issue":"2","isi":1,"article_type":"original","doi":"10.3847/1538-4357/acd118","fulldoi":"https://doi.org/10.3847/1538-4357/acd118","oa_version":"Published Version","language":[{"iso":"eng"}],"day":"01","_id":"13443","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_processing_charge":"Yes","date_created":"2023-08-01T14:19:16Z","acknowledgement":"This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the NASA Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. We acknowledge that this research was supported in part by the National Science Foundation under grant No. NSF PHY-1748958. S.M. acknowledges support from the Spanish Ministry of Science and Innovation (MICINN) with the Ramón y Cajal fellowship No. RYC-2015-17697, the grant No. PID2019-107061GB-C66, and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). S.M. and D.G.R. acknowledge support from the Spanish Ministry of Science and Innovation (MICINN) with the grant No. PID2019-107187GB-I00. Z.R.C. acknowledges support from National Aeronautics and Space Administration via the TESS Guest Investigator Program (grant No. 80NSSC18K18584). The work presented here was partially supported by the NASA grant NNX17AF27G. A.R.G.S. acknowledges the support by FCT through national funds and by FEDER through COMPETE2020 by the following grants: UIDB/04434/2020 and UIDP/04434/2020. A.R.G.S. is supported by FCT through the work contract No. 2020.02480.CEECIND/CP1631/CT0001. R.A.G., L.A., and S.N.B. acknowledge the support from PLATO and GOLF CNES grants. S.N.B. acknowledges support from PLATO ASI-INAF agreement No. 2015-019-R.1-2018.","department":[{"_id":"LiBu"}],"date_updated":"2026-07-06T12:20:17Z","das_tickbox":"1","file":[{"date_created":"2023-08-02T07:42:26Z","file_name":"2023_AstrophysicalJour_Mathur.pdf","success":1,"checksum":"f12452834d7ed6748dbf5ace18af4723","date_updated":"2023-08-02T07:42:26Z","access_level":"open_access","creator":"dernst","file_id":"13448","file_size":4192386,"relation":"main_file","content_type":"application/pdf"}],"month":"08","date_published":"2023-08-01T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"abstract":[{"lang":"eng","text":"The ages of solar-like stars have been at the center of many studies such as exoplanet characterization or Galactic-archeology. While ages are usually computed from stellar evolution models, relations linking ages to other stellar properties, such as rotation and magnetic activity, have been investigated. With the large catalog of 55,232 rotation periods, Prot, and photometric magnetic activity index, Sph from Kepler data, we have the opportunity to look for such magneto-gyro-chronology relations. Stellar ages are obtained with two stellar evolution codes that include treatment of angular momentum evolution, hence using Prot as input in addition to classical atmospheric parameters. We explore two different ways of predicting stellar ages on three subsamples with spectroscopic observations: solar analogs, late-F and G dwarfs, and K dwarfs. We first perform a Bayesian analysis to derive relations between Sph and ages between 1 and 5 Gyr, and other stellar properties. For late-F and G dwarfs, and K dwarfs, the multivariate regression favors the model with Prot and Sph with median differences of 0.1% and 0.2%, respectively. We also apply Machine Learning techniques with a Random Forest algorithm to predict ages up to 14 Gyr with the same set of input parameters. For late-F, G and K dwarfs together, predicted ages are on average within 5.3% of the model ages and improve to 3.1% when including Prot. These are very promising results for a quick age estimation for solar-like stars with photometric observations, especially with current and future space missions."}],"author":[{"first_name":"Savita","full_name":"Mathur, Savita","last_name":"Mathur"},{"last_name":"Claytor","full_name":"Claytor, Zachary R.","first_name":"Zachary R."},{"last_name":"Santos","first_name":"Ângela R. G.","full_name":"Santos, Ângela R. G."},{"last_name":"García","full_name":"García, Rafael A.","first_name":"Rafael A."},{"first_name":"Louis","full_name":"Amard, Louis","last_name":"Amard"},{"last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle"},{"last_name":"Corsaro","full_name":"Corsaro, Enrico","first_name":"Enrico"},{"first_name":"Alfio","full_name":"Bonanno, Alfio","last_name":"Bonanno"},{"last_name":"Breton","first_name":"Sylvain N.","full_name":"Breton, Sylvain N."},{"first_name":"Diego","full_name":"Godoy-Rivera, Diego","last_name":"Godoy-Rivera"},{"full_name":"Pinsonneault, Marc H.","first_name":"Marc H.","last_name":"Pinsonneault"},{"last_name":"van Saders","first_name":"Jennifer","full_name":"van Saders, Jennifer"}],"file_date_updated":"2023-08-02T07:42:26Z","oa":1,"publisher":"IOP Publishing","publication":"The Astrophysical Journal","year":"2023","volume":952,"intvolume":"       952","quality_controlled":"1","status":"public","ddc":["520"],"scopus_import":"1"},{"arxiv":1,"isi":1,"article_type":"letter_note","has_accepted_license":"1","type":"journal_article","article_processing_charge":"Yes (in subscription journal)","doi":"10.1051/0004-6361/202346832","oa_version":"Published Version","fulldoi":"https://doi.org/10.1051/0004-6361/202346832","language":[{"iso":"eng"}],"_id":"14256","day":"01","citation":{"apa":"Mathis, S., &#38; Bugnet, L. A. (2023). Asymmetries of frequency splittings of dipolar mixed modes: A window on the topology of deep magnetic fields. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202346832\">https://doi.org/10.1051/0004-6361/202346832</a>","mla":"Mathis, S., and Lisa Annabelle Bugnet. “Asymmetries of Frequency Splittings of Dipolar Mixed Modes: A Window on the Topology of Deep Magnetic Fields.” <i>Astronomy &#38; Astrophysics</i>, vol. 676, L9, EDP Sciences, 2023, doi:<a href=\"https://doi.org/10.1051/0004-6361/202346832\">10.1051/0004-6361/202346832</a>.","ieee":"S. Mathis and L. A. Bugnet, “Asymmetries of frequency splittings of dipolar mixed modes: A window on the topology of deep magnetic fields,” <i>Astronomy &#38; Astrophysics</i>, vol. 676. EDP Sciences, 2023.","ama":"Mathis S, Bugnet LA. Asymmetries of frequency splittings of dipolar mixed modes: A window on the topology of deep magnetic fields. <i>Astronomy &#38; Astrophysics</i>. 2023;676. doi:<a href=\"https://doi.org/10.1051/0004-6361/202346832\">10.1051/0004-6361/202346832</a>","short":"S. Mathis, L.A. Bugnet, Astronomy &#38; Astrophysics 676 (2023).","ista":"Mathis S, Bugnet LA. 2023. Asymmetries of frequency splittings of dipolar mixed modes: A window on the topology of deep magnetic fields. Astronomy &#38; Astrophysics. 676, L9.","chicago":"Mathis, S., and Lisa Annabelle Bugnet. “Asymmetries of Frequency Splittings of Dipolar Mixed Modes: A Window on the Topology of Deep Magnetic Fields.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2023. <a href=\"https://doi.org/10.1051/0004-6361/202346832\">https://doi.org/10.1051/0004-6361/202346832</a>."},"article_number":"L9","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"external_id":{"isi":["001046037700007"],"arxiv":["2306.11587"]},"title":"Asymmetries of frequency splittings of dipolar mixed modes: A window on the topology of deep magnetic fields","publisher":"EDP Sciences","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"abstract":[{"lang":"eng","text":"Context. Space asteroseismology is revolutionizing our knowledge of the internal structure and dynamics of stars. A breakthrough is ongoing with the recent discoveries of signatures of strong magnetic fields in the core of red giant stars. The key signature for such a detection is the asymmetry these fields induce in the frequency splittings of observed dipolar mixed gravito-acoustic modes.\r\nAims. We investigate the ability of the observed asymmetries of the frequency splittings of dipolar mixed modes to constrain the geometrical properties of deep magnetic fields.\r\nMethods. We used the powerful analytical Racah-Wigner algebra used in quantum mechanics to characterize the geometrical couplings of dipolar mixed oscillation modes with various realistically plausible topologies of fossil magnetic fields. We also computed the induced perturbation of their frequencies.\r\nResults. First, in the case of an oblique magnetic dipole, we provide the exact analytical expression of the asymmetry as a function of the angle between the rotation and magnetic axes. Its value provides a direct measure of this angle. Second, considering a combination of axisymmetric dipolar and quadrupolar fields, we show how the asymmetry is blind to the unraveling of the relative strength and sign of each component. Finally, in the case of a given multipole, we show that a negative asymmetry is a signature of non-axisymmetric topologies.\r\nConclusions. Asymmetries of dipolar mixed modes provide a key bit of information on the geometrical topology of deep fossil magnetic fields, but this is insufficient on its own. Asteroseismic constraints should therefore be combined with spectropolarimetric observations and numerical simulations, which aim to predict the more probable stable large-scale geometries."}],"author":[{"last_name":"Mathis","full_name":"Mathis, S.","first_name":"S."},{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet"}],"oa":1,"file_date_updated":"2023-09-06T07:13:19Z","intvolume":"       676","status":"public","ddc":["520"],"quality_controlled":"1","scopus_import":"1","publication":"Astronomy & Astrophysics","volume":676,"year":"2023","date_updated":"2026-07-08T06:45:55Z","das_tickbox":"1","file":[{"date_updated":"2023-09-06T07:13:19Z","access_level":"open_access","creator":"dernst","success":1,"date_created":"2023-09-06T07:13:19Z","file_name":"2023_AstronomyAstrophysics_Mathis.pdf","checksum":"7b30d26fb2b7bcb5b5be1414950615f9","content_type":"application/pdf","relation":"main_file","file_id":"14271","file_size":458120}],"date_created":"2023-09-03T22:01:15Z","acknowledgement":"The authors are grateful to the referee for her/his detailed and constructive report, which has allowed us to improve our article. S. M. acknowledges support from the CNES GOLF-SOHO and PLATO grants at CEA/DAp and PNPS (CNRS/INSU). We thank R. A. Garcia for fruitful discussions and suggestions.","department":[{"_id":"LiBu"}],"date_published":"2023-08-01T00:00:00Z","month":"08"}]