[{"publication_status":"published","type":"journal_article","publisher":"IOP Publishing","doi":"10.3847/1538-4357/ae7a3c","oa":1,"quality_controlled":"1","date_published":"2026-07-10T00:00:00Z","article_processing_charge":"Yes","citation":{"mla":"De Vries, Nils B., et al. “Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars.” <i>The Astrophysical Journal</i>, vol. 1005, no. 2, 154, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">10.3847/1538-4357/ae7a3c</a>.","ama":"De Vries NB, Le Saux A, Baraffe I, et al. Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. <i>The Astrophysical Journal</i>. 2026;1005(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">10.3847/1538-4357/ae7a3c</a>","ieee":"N. B. De Vries <i>et al.</i>, “Revealing mixed modes in compressible hydrodynamical simulations of red giant stars,” <i>The Astrophysical Journal</i>, vol. 1005, no. 2. IOP Publishing, 2026.","apa":"De Vries, N. B., Le Saux, A., Baraffe, I., Guillet, T., Townsend, R. H. D., Leclerc, A., &#38; Morison, A. (2026). Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">https://doi.org/10.3847/1538-4357/ae7a3c</a>","chicago":"De Vries, Nils B., Arthur Le Saux, Isabelle Baraffe, Thomas Guillet, Richard H.D. Townsend, Armand Leclerc, and Adrien Morison. “Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">https://doi.org/10.3847/1538-4357/ae7a3c</a>.","ista":"De Vries NB, Le Saux A, Baraffe I, Guillet T, Townsend RHD, Leclerc A, Morison A. 2026. Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. The Astrophysical Journal. 1005(2), 154.","short":"N.B. De Vries, A. Le Saux, I. Baraffe, T. Guillet, R.H.D. Townsend, A. Leclerc, A. Morison, The Astrophysical Journal 1005 (2026)."},"article_type":"original","keyword":["Stellar physics","Stellar interiors","Asteroseismology","Stellar oscillations","Hydrodynamical simulations"],"abstract":[{"text":"Mixed modes are observed in many low-mass evolved stars. They provide information about core rotation rates of these stars, which are lower than predicted by stellar evolution models. The mixed modes themselves have been invoked as an angular momentum (AM) transport mechanism, but estimating their transport efficiency requires knowledge of their amplitudes. We constrain, for the first time, the mixed-mode amplitudes in 2D hydrodynamical simulations of a 1.3M⊙ red giant using the code MUSIC. We perform two simulations with outer radial truncations at fractional radii ro/r⋆ = 0.90 and 0.98. We compare the modes in the simulation with those found using both GYRE and a Dedalus eigenvalue solver. Excellent frequency agreement is found for all p-dominated modes, with minor discrepancies for g-dominated modes, especially in the frequency range [60, 240] μHz. We find excellent eigenfunction agreement for all modes except those in this frequency range. According to empirical predictions, the largest kinetic energies are located around Vmax= 312.μHz, but in both simulations, the modes with frequencies of ν < 50 μHz have the largest kinetic energies. In the simulation with r/r⋆ = 0.98, the simulated modes have extrapolated surface velocities comparable to the empirical predictions, with the highest surface velocities in a bell-shaped curve peaking around ν = 700 μHz. The extrapolated surface velocities of the low-frequency modes are small and thus hard to observe, but their large kinetic energies deeper in the interior could significantly impact AM transport, which has not yet been investigated.","lang":"eng"}],"file_date_updated":"2026-07-13T08:14:01Z","_id":"22262","project":[{"name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","grant_number":"101165631"}],"date_created":"2026-07-12T22:02:17Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","author":[{"last_name":"De Vries","first_name":"Nils B.","full_name":"De Vries, Nils B."},{"full_name":"Le Saux, Arthur","last_name":"Le Saux","first_name":"Arthur"},{"last_name":"Baraffe","first_name":"Isabelle","full_name":"Baraffe, Isabelle"},{"full_name":"Guillet, Thomas","first_name":"Thomas","last_name":"Guillet"},{"first_name":"Richard H.D.","last_name":"Townsend","full_name":"Townsend, Richard H.D."},{"id":"2a1fb1fc-f373-11ef-901a-87cee43a1217","full_name":"Leclerc, Armand","last_name":"Leclerc","first_name":"Armand"},{"full_name":"Morison, Adrien","last_name":"Morison","first_name":"Adrien"}],"OA_place":"publisher","OA_type":"gold","title":"Revealing mixed modes in compressible hydrodynamical simulations of red giant stars","file":[{"file_name":"2026_AstrophysicalJour_deVries.pdf","content_type":"application/pdf","creator":"dernst","file_size":14866194,"checksum":"d32061d2341bac3adeb404975c6bd59e","success":1,"date_created":"2026-07-13T08:14:01Z","file_id":"22275","relation":"main_file","date_updated":"2026-07-13T08:14:01Z","access_level":"open_access"}],"external_id":{"arxiv":["2606.07125"]},"intvolume":"      1005","ddc":["520"],"article_number":"154","has_accepted_license":"1","department":[{"_id":"LiBu"}],"scopus_import":"1","oa_version":"Published Version","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"DOAJ_listed":"1","day":"10","researchdata_availability":"yes","year":"2026","das_tickbox":"1","supplementarymaterial":"yes","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"date_updated":"2026-07-13T08:16:25Z","volume":1005,"dataavailabilitystatement":"The kinetic energies and surface velocities shown in Figure 4, as well as the underlying spectral data of this work, can be found in a Zenodo repository at doi:10.5281/zenodo.18661976.","arxiv":1,"month":"07","acknowledgement":"We would like to thank the referee for their careful reading of the manuscript and their constructive comments that helped improve the paper. N.B.V. would like to thank K. Belkacem and J. Philidet for helpful discussions. N.B.V. is supported by STFC grant ST/Y002164/1. A.L.S. acknowledges support from the European Research Council (ERC) under the Horizon Europe program (Synergy grant agreement 101071505: 4D-STAR) from the CNES SOHO-GOLF and PLATO grants at CEA-DAp, and from ATPS (CNRS/INSU). Part of this work was supported by the ERC grant No. 787361-COBOM. R.H.D.T. acknowledges support from NASA grants 80NSSC24K0895 and 80NSSC23K1517, and NSF grant 2407636. A.L. is supported by ERC Starting Grant 101165631 (“Calcifer”). The authors would like to acknowledge the use of the University of Exeter High-Performance Computing (HPC) facility, ISCA, in carrying out this work. This work used the DiRAC Memory Intensive service (Cosma8) at Durham University, managed by the Institute for Computational Cosmology, and the DiRAC Data Intensive service (DIaL3) at the University of Leicester, managed by the University of Leicester Research Computing Service. These facilities are managed on behalf of the STFC DiRAC HPC (www.dirac.ac.uk). The DiRAC services at Durham and Leicester were funded by BEIS, UKRI, and STFC capital funding, and STFC operations grants. The service at Durham received funding from Durham University. DiRAC is part of the UKRI Digital Research Infrastructure.","status":"public","PlanS_conform":"1"},{"has_accepted_license":"1","department":[{"_id":"GradSch"},{"_id":"LiBu"}],"ddc":["520"],"title":"Exploring internal magnetism in partially suppressed red giant stars","OA_place":"publisher","file":[{"access_level":"closed","date_updated":"2025-10-08T09:45:33Z","file_id":"20434","date_created":"2025-10-08T08:01:42Z","relation":"source_file","checksum":"80d241d11b69af771c1fab0998be4f19","content_type":"application/zip","file_size":8263624,"creator":"ksmith","file_name":"2025_Smith_Kanah_Thesis.zip"},{"content_type":"application/pdf","creator":"ksmith","file_size":9748339,"success":1,"checksum":"13cb48cc98e00fdfe32f3ff66f17aa26","file_name":"2025_Smith_Kanah_Thesis.pdf","date_updated":"2025-10-09T14:38:57Z","access_level":"open_access","date_created":"2025-10-09T14:38:57Z","relation":"main_file","file_id":"20439"}],"alternative_title":["ISTA Master's Thesis"],"date_created":"2025-06-20T13:27:08Z","user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","author":[{"id":"7703505d-3211-11ee-a6a9-a2ab9d936c15","full_name":"Smith, Kanah","last_name":"Smith","first_name":"Kanah"}],"keyword":["asteroseismology","stellar physics","red giant","magnetism","suppressed"],"file_date_updated":"2025-10-09T14:38:57Z","abstract":[{"lang":"eng","text":"The internal dynamical properties of red giant stars have been explored extensively in recent\r\nyears as a result of the increase in high precision data availability from the space missions\r\nKepler and TESS (Transiting Exoplanet Survey Satellite), and in this exploration, it has been\r\ndiscovered that some of these stars are not behaving as expected. Red giants are stars that have\r\nevolved off of the main sequence after having completed fusing hydrogen into helium in their\r\ncore. Observational data shows that the cores are rotating significantly slower than models can\r\nrecreate consistently across evolutionary stages. This discrepancy has prompted investigation\r\ninto the efficiency of angular momentum transport mechanisms and mixing processes including\r\nmeridional circulation, shear instability, internal gravity waves, Tayler-Spruit dynamo, fossil\r\nmagnetic fields etc., to explain this behavior.\r\nAnalyzing seismic oscillations in stars, via asteroseismology, is a powerful tool as it is the only\r\nway in which the deep stellar interior can be probed and subsequently characterized; this is\r\npossible as global oscillations modulating the stellar surface are effected by internal processes.\r\nFor red giants, p-modes (pressure modes; resonating through the entire star) and g-modes\r\n(gravity-modes; resonating in the radiative interior) couple to create mixed modes. These\r\nmixed modes give access to the otherwise hidden stellar interior as g-modes couple to p-modes,\r\ndelivering information from the interior to the surface.\r\nInternal magnetic signatures have been observationally confirmed in red giant stars via\r\nasteroseismology and characterized in two ways. One being that dipole mixed modes with\r\nℓ = 1 will display a global asymmetric frequency shift of its azimuthal components; where\r\nthe m = 0 and m = ±1 components of the ℓ = 1 dipole mode will be shifted by two\r\ndifferent power laws, respectively. And the other being a reduced visibility of dipole mixed\r\nmode amplitudes in the power spectra, where stars presenting with this feature are denoted as\r\nsuppressed.\r\nSeveral studies of the suppressed dipole mixed mode amplitudes have been carried out, but thus\r\nfar, no dedicated studies of the asymmetric frequency shifts of suppressed red giants have been\r\nconducted; one reason being that the asymmetric frequency shifts cannot be characterized\r\nwhen the dipole mixed mode amplitudes are severely reduced in many of the suppressed stars.\r\nSincefullysuppressedstarsdonothavedetectablemixed-modestoevaluate, partiallysuppressed\r\nstars, that is, red giant stars presenting with suppressed dipole mixed modes in select parts of\r\ntheir power spectra rather than across the entire spectra, will be the subject of this study as\r\nthe respective mode amplitudes are still visible at high frequencies.\r\nAs such, this study will search for asymmetric frequency shifts on the dipole mixed\r\nmodes of partially suppressed red giant stars; the aim here is to investigate if both\r\nmode suppression and magnetic shifting of dipole mixed modes occur simultaneously.\r\nThisstudywillbeconductedbycreatingapipelinetoestimatepriorsofasteroseismicparameters,\r\nuse the priors to model the power spectra with the stellar modeling code sloscillations_ISTA,\r\nand perform a Bayesian fit of the parameters with the simulated data on the star KIC 6975038,\r\na target with partially suppressed dipolar mode amplitudes identified in the literature, to fit its\r\nmagnetic parameters. I present a novel method to model the stellar power spectra of\r\npartially suppressed red giants by application of a sigmoid profile to the ℓ= 1 dipolar\r\nmode component of the spectra. With the results of this study I aim at constraining\r\nthe cause of this partial dipole mode amplitude suppression, allowing for more detailed\r\nstudies regarding their astrophysical nature. Furthermore, the long term hope for the method\r\nused in this study will be to expand the sample of partially suppressed red giants and fit their\r\nasteroseismic parameters accordingly."}],"_id":"19853","date_published":"2025-10-08T00:00:00Z","article_processing_charge":"No","citation":{"short":"K. Smith, Exploring Internal Magnetism in Partially Suppressed Red Giant Stars, Institute of Science and Technology Austria, 2025.","ista":"Smith K. 2025. Exploring internal magnetism in partially suppressed red giant stars. Institute of Science and Technology Austria.","chicago":"Smith, Kanah. “Exploring Internal Magnetism in Partially Suppressed Red Giant Stars.” Institute of Science and Technology Austria, 2025. <a href=\"https://doi.org/10.15479/AT-ISTA-19853\">https://doi.org/10.15479/AT-ISTA-19853</a>.","apa":"Smith, K. (2025). <i>Exploring internal magnetism in partially suppressed red giant stars</i>. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/AT-ISTA-19853\">https://doi.org/10.15479/AT-ISTA-19853</a>","ieee":"K. Smith, “Exploring internal magnetism in partially suppressed red giant stars,” Institute of Science and Technology Austria, 2025.","ama":"Smith K. Exploring internal magnetism in partially suppressed red giant stars. 2025. doi:<a href=\"https://doi.org/10.15479/AT-ISTA-19853\">10.15479/AT-ISTA-19853</a>","mla":"Smith, Kanah. <i>Exploring Internal Magnetism in Partially Suppressed Red Giant Stars</i>. Institute of Science and Technology Austria, 2025, doi:<a href=\"https://doi.org/10.15479/AT-ISTA-19853\">10.15479/AT-ISTA-19853</a>."},"publisher":"Institute of Science and Technology Austria","doi":"10.15479/AT-ISTA-19853","oa":1,"type":"dissertation","publication_status":"published","month":"10","acknowledgement":"I would like to give thanks to myself for my hard work on this document. This paper includes data collected by the Kepler mission and obtained from the MAST data\r\narchive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is\r\nprovided by the NASA Science Mission Directorate. STScI is operated by the Association of\r\nUniversities for Research in Astronomy, Inc., under NASA contract NAS 5–26555.\r\n","status":"public","page":"38","date_updated":"2026-04-07T12:01:37Z","supervisor":[{"orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"}],"year":"2025","publication_identifier":{"issn":["2791-4585"]},"day":"08","degree_awarded":"MS","corr_author":"1","language":[{"iso":"eng"}],"oa_version":"Published Version"},{"volume":647,"date_updated":"2024-10-14T11:39:21Z","arxiv":1,"month":"03","extern":"1","status":"public","acknowledgement":"The authors thank the referee and Pr. J. Christensen-Dalsgaard for their very constructive comments and remarks that allowed us to improve the article. St. M., L. B., V. P., and K. A. acknowledge support from the European Research Council through ERC grant SPIRE 647383. All the members from CEA acknowledge support from GOLF and PLATO CNES grants of the Astrophysics Division at CEA. S. Mathur acknowledges support by the Ramon y Cajal fellowship number RYC-2015-17697. We made great use of the megyr python package for interfacing MESA and GYRE codes.","scopus_import":"1","publication":"Astronomy & Astrophysics","oa_version":"Preprint","language":[{"iso":"eng"}],"day":"18","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"year":"2021","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2022-07-18T12:15:27Z","author":[{"last_name":"Mathis","first_name":"S.","full_name":"Mathis, S."},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet"},{"full_name":"Prat, V.","last_name":"Prat","first_name":"V."},{"last_name":"Augustson","first_name":"K.","full_name":"Augustson, K."},{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"full_name":"Garcia, R. A.","first_name":"R. A.","last_name":"Garcia"}],"title":"Probing the internal magnetism of stars using asymptotic magneto-asteroseismology","intvolume":"       647","external_id":{"arxiv":["2012.11050"]},"article_number":"A122","type":"journal_article","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2012.11050"}],"publisher":"EDP Sciences","oa":1,"doi":"10.1051/0004-6361/202039180","quality_controlled":"1","article_type":"original","citation":{"short":"S. Mathis, L.A. Bugnet, V. Prat, K. Augustson, S. Mathur, R.A. Garcia, Astronomy &#38; Astrophysics 647 (2021).","ista":"Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. 2021. Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. Astronomy &#38; Astrophysics. 647, A122.","chicago":"Mathis, S., Lisa Annabelle Bugnet, V. Prat, K. Augustson, S. Mathur, and R. A. Garcia. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039180\">https://doi.org/10.1051/0004-6361/202039180</a>.","apa":"Mathis, S., Bugnet, L. A., Prat, V., Augustson, K., Mathur, S., &#38; Garcia, R. A. (2021). Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039180\">https://doi.org/10.1051/0004-6361/202039180</a>","ieee":"S. Mathis, L. A. Bugnet, V. Prat, K. Augustson, S. Mathur, and R. A. Garcia, “Probing the internal magnetism of stars using asymptotic magneto-asteroseismology,” <i>Astronomy &#38; Astrophysics</i>, vol. 647. EDP Sciences, 2021.","ama":"Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. <i>Astronomy &#38; Astrophysics</i>. 2021;647. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039180\">10.1051/0004-6361/202039180</a>","mla":"Mathis, S., et al. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.” <i>Astronomy &#38; Astrophysics</i>, vol. 647, A122, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039180\">10.1051/0004-6361/202039180</a>."},"date_published":"2021-03-18T00:00:00Z","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / waves / stars","magnetic field / stars","oscillations / methods","analytical"],"_id":"11606","abstract":[{"text":"Context. Our knowledge of the dynamics of stars has undergone a revolution through the simultaneous large amount of high-quality photometric observations collected by space-based asteroseismology and ground-based high-precision spectropolarimetry. They allowed us to probe the internal rotation of stars and their surface magnetism in the whole Hertzsprung-Russell diagram. However, new methods should still be developed to probe the deep magnetic fields in these stars.\r\n\r\nAims. Our goal is to provide seismic diagnoses that allow us to probe the internal magnetism of stars.\r\n\r\nMethods. We focused on asymptotic low-frequency gravity modes and high-frequency acoustic modes. Using a first-order perturbative theory, we derived magnetic splittings of their frequencies as explicit functions of stellar parameters.\r\n\r\nResults. As in the case of rotation, we show that asymptotic gravity and acoustic modes can allow us to probe the different components of the magnetic field in the cavities in which they propagate. This again demonstrates the high potential of using mixed-modes when this is possible.","lang":"eng"}]},{"language":[{"iso":"eng"}],"oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","year":"2019","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"day":"01","date_updated":"2022-08-22T07:35:19Z","volume":485,"acknowledgement":"Funding for this Discovery mission is provided by NASA’s Science mission Directorate. We thank the entire Kepler team without whom this investigation would not be possible. DS is the recipient of an Australian Research Council Future Fellowship (project number FT1400147). RAG acknowledges the support from CNES. SM acknowledges support from NASA grant NNX15AF13G, NSF grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. ILC acknowledges scholarship support from the University of Sydney. We would like to thank Nicholas Barbara and Timothy Bedding for providing us with a list of variable stars that helped to validate a number of detections in this study. We also thank the group at the University of Sydney for fruitful discussions. Finally, we gratefully acknowledge the support of NVIDIA Corporation with the donation of the Titan Xp GPU used for this research.","status":"public","extern":"1","month":"06","arxiv":1,"page":"5616-5630","quality_controlled":"1","publisher":"Oxford University Press","doi":"10.1093/mnras/stz622","oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1903.00115"}],"publication_status":"published","type":"journal_article","abstract":[{"text":"The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000 targets observed during the mission. Despite this, no wide search for red giants showing solar-like oscillations have been made across all stars observed in Kepler’s long-cadence mode. In this work, we perform this task using custom apertures on the Kepler pixel files and detect oscillations in 21 914 stars, representing the largest sample of solar-like oscillating stars to date. We measure their frequency at maximum power, νmax, down to νmax≃4μHz and obtain log (g) estimates with a typical uncertainty below 0.05 dex, which is superior to typical measurements from spectroscopy. Additionally, the νmax distribution of our detections show good agreement with results from a simulated model of the Milky Way, with a ratio of observed to predicted stars of 0.992 for stars with 10<νmax<270μHz. Among our red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal is polluted by a neighbouring giant as a result of using larger photometric apertures than those used by the NASA Kepler science processing pipeline. We further find that only 293 of the polluting giants are known Kepler targets. The remainder comprises over 600 newly identified oscillating red giants, with many expected to belong to the Galactic halo, serendipitously falling within the Kepler pixel files of targeted stars.","lang":"eng"}],"_id":"11615","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","methods: data analysis","techniques: image processing","stars: oscillations","stars: statistics"],"date_published":"2019-06-01T00:00:00Z","article_processing_charge":"No","citation":{"ama":"Hon M, Stello D, García RA, et al. A search for red giant solar-like oscillations in all Kepler data. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;485(4):5616-5630. doi:<a href=\"https://doi.org/10.1093/mnras/stz622\">10.1093/mnras/stz622</a>","mla":"Hon, Marc, et al. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 485, no. 4, Oxford University Press, 2019, pp. 5616–30, doi:<a href=\"https://doi.org/10.1093/mnras/stz622\">10.1093/mnras/stz622</a>.","ieee":"M. Hon <i>et al.</i>, “A search for red giant solar-like oscillations in all Kepler data,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 485, no. 4. Oxford University Press, pp. 5616–5630, 2019.","apa":"Hon, M., Stello, D., García, R. A., Mathur, S., Sharma, S., Colman, I. L., &#38; Bugnet, L. A. (2019). A search for red giant solar-like oscillations in all Kepler data. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz622\">https://doi.org/10.1093/mnras/stz622</a>","chicago":"Hon, Marc, Dennis Stello, Rafael A García, Savita Mathur, Sanjib Sharma, Isabel L Colman, and Lisa Annabelle Bugnet. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz622\">https://doi.org/10.1093/mnras/stz622</a>.","short":"M. Hon, D. Stello, R.A. García, S. Mathur, S. Sharma, I.L. Colman, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 485 (2019) 5616–5630.","ista":"Hon M, Stello D, García RA, Mathur S, Sharma S, Colman IL, Bugnet LA. 2019. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 485(4), 5616–5630."},"article_type":"original","title":"A search for red giant solar-like oscillations in all Kepler data","issue":"4","author":[{"last_name":"Hon","first_name":"Marc","full_name":"Hon, Marc"},{"full_name":"Stello, Dennis","last_name":"Stello","first_name":"Dennis"},{"first_name":"Rafael A","last_name":"García","full_name":"García, Rafael A"},{"last_name":"Mathur","first_name":"Savita","full_name":"Mathur, Savita"},{"first_name":"Sanjib","last_name":"Sharma","full_name":"Sharma, Sanjib"},{"full_name":"Colman, Isabel L","last_name":"Colman","first_name":"Isabel L"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle"}],"date_created":"2022-07-18T14:26:03Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"arxiv":["1903.00115"]},"intvolume":"       485"},{"title":"Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques","date_updated":"2022-08-22T08:16:53Z","date_created":"2022-07-20T11:18:53Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"last_name":"Breton","first_name":"S. N.","full_name":"Breton, S. N."},{"first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"Santos, A. R. G.","last_name":"Santos","first_name":"A. R. G."},{"first_name":"A. Le","last_name":"Saux","full_name":"Saux, A. Le"},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"first_name":"P. L.","last_name":"Palle","full_name":"Palle, P. L."},{"last_name":"Garcia","first_name":"R. A.","full_name":"Garcia, R. A."}],"extern":"1","month":"06","status":"public","external_id":{"arxiv":["1906.09609"]},"arxiv":1,"article_number":"1906.09609","doi":"10.48550/arXiv.1906.09609","language":[{"iso":"eng"}],"oa":1,"publication_status":"submitted","type":"preprint","main_file_link":[{"url":"https://arxiv.org/abs/1906.09609","open_access":"1"}],"publication":"arXiv","oa_version":"Preprint","keyword":["asteroseismology","rotation","solar-like stars","kepler","machine learning","random forest"],"abstract":[{"lang":"eng","text":"For a solar-like star, the surface rotation evolves with time, allowing in principle to estimate the age of a star from its surface rotation period. Here we are interested in measuring surface rotation periods of solar-like stars observed by the NASA mission Kepler. Different methods have been developed to track rotation signals in Kepler photometric light curves: time-frequency analysis based on wavelet techniques, autocorrelation and composite spectrum. We use the learning abilities of random forest classifiers to take decisions during two crucial steps of the analysis. First, given some input parameters, we discriminate the considered Kepler targets between rotating MS stars, non-rotating MS stars, red giants, binaries and pulsators. We then use a second classifier only on the MS rotating targets to decide the best data analysis treatment."}],"_id":"11627","year":"2019","date_published":"2019-06-23T00:00:00Z","article_processing_charge":"No","day":"23","citation":{"ista":"Breton SN, Bugnet LA, Santos ARG, Saux AL, Mathur S, Palle PL, Garcia RA. Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. arXiv, 1906.09609.","short":"S.N. Breton, L.A. Bugnet, A.R.G. Santos, A.L. Saux, S. Mathur, P.L. Palle, R.A. Garcia, ArXiv (n.d.).","apa":"Breton, S. N., Bugnet, L. A., Santos, A. R. G., Saux, A. L., Mathur, S., Palle, P. L., &#38; Garcia, R. A. (n.d.). Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. <i>arXiv</i>. <a href=\"https://doi.org/10.48550/arXiv.1906.09609\">https://doi.org/10.48550/arXiv.1906.09609</a>","chicago":"Breton, S. N., Lisa Annabelle Bugnet, A. R. G. Santos, A. Le Saux, S. Mathur, P. L. Palle, and R. A. Garcia. “Determining Surface Rotation Periods of Solar-like Stars Observed by the Kepler Mission Using Machine Learning Techniques.” <i>ArXiv</i>, n.d. <a href=\"https://doi.org/10.48550/arXiv.1906.09609\">https://doi.org/10.48550/arXiv.1906.09609</a>.","ieee":"S. N. Breton <i>et al.</i>, “Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques,” <i>arXiv</i>. .","mla":"Breton, S. N., et al. “Determining Surface Rotation Periods of Solar-like Stars Observed by the Kepler Mission Using Machine Learning Techniques.” <i>ArXiv</i>, 1906.09609, doi:<a href=\"https://doi.org/10.48550/arXiv.1906.09609\">10.48550/arXiv.1906.09609</a>.","ama":"Breton SN, Bugnet LA, Santos ARG, et al. Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. <i>arXiv</i>. doi:<a href=\"https://doi.org/10.48550/arXiv.1906.09609\">10.48550/arXiv.1906.09609</a>"}},{"external_id":{"arxiv":["1906.09611"]},"article_number":"1906.09611","arxiv":1,"extern":"1","month":"06","status":"public","date_created":"2022-07-21T06:57:10Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"full_name":"Saux, A. Le","last_name":"Saux","first_name":"A. Le"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet"},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"first_name":"S. N.","last_name":"Breton","full_name":"Breton, S. N."},{"full_name":"Garcia, R. A.","first_name":"R. A.","last_name":"Garcia"}],"title":"Automatic classification of K2 pulsating stars using machine learning techniques","date_updated":"2022-08-22T08:20:29Z","date_published":"2019-06-23T00:00:00Z","article_processing_charge":"No","citation":{"ama":"Saux AL, Bugnet LA, Mathur S, Breton SN, Garcia RA. Automatic classification of K2 pulsating stars using machine learning techniques. <i>arXiv</i>. doi:<a href=\"https://doi.org/10.48550/arXiv.1906.09611\">10.48550/arXiv.1906.09611</a>","mla":"Saux, A. Le, et al. “Automatic Classification of K2 Pulsating Stars Using Machine Learning Techniques.” <i>ArXiv</i>, 1906.09611, doi:<a href=\"https://doi.org/10.48550/arXiv.1906.09611\">10.48550/arXiv.1906.09611</a>.","ieee":"A. L. Saux, L. A. Bugnet, S. Mathur, S. N. Breton, and R. A. Garcia, “Automatic classification of K2 pulsating stars using machine learning techniques,” <i>arXiv</i>. .","chicago":"Saux, A. Le, Lisa Annabelle Bugnet, S. Mathur, S. N. Breton, and R. A. Garcia. “Automatic Classification of K2 Pulsating Stars Using Machine Learning Techniques.” <i>ArXiv</i>, n.d. <a href=\"https://doi.org/10.48550/arXiv.1906.09611\">https://doi.org/10.48550/arXiv.1906.09611</a>.","apa":"Saux, A. L., Bugnet, L. A., Mathur, S., Breton, S. N., &#38; Garcia, R. A. (n.d.). Automatic classification of K2 pulsating stars using machine learning techniques. <i>arXiv</i>. <a href=\"https://doi.org/10.48550/arXiv.1906.09611\">https://doi.org/10.48550/arXiv.1906.09611</a>","short":"A.L. Saux, L.A. Bugnet, S. Mathur, S.N. Breton, R.A. Garcia, ArXiv (n.d.).","ista":"Saux AL, Bugnet LA, Mathur S, Breton SN, Garcia RA. Automatic classification of K2 pulsating stars using machine learning techniques. arXiv, 1906.09611."},"day":"23","keyword":["asteroseismology - methods","data analysis - thecniques","machine learning - stars","oscillations"],"abstract":[{"text":"The second mission of NASA’s Kepler satellite, K2, has collected hundreds of thousands of lightcurves for stars close to the ecliptic plane. This new sample could increase the number of known pulsating stars and then improve our understanding of those stars. For the moment only a few stars have been properly classified and published. In this work, we present a method to automaticly classify K2 pulsating stars using a Machine Learning technique called Random Forest. The objective is to sort out the stars in four classes: red giant (RG), main-sequence Solar-like stars (SL), classical pulsators (PULS) and Other. To do this we use the effective temperatures and the luminosities of the stars as well as the FliPer features, that measures the amount of power contained in the power spectral density. The classifier now retrieves the right classification for more than 80% of the stars.","lang":"eng"}],"year":"2019","_id":"11630","publication_status":"submitted","type":"preprint","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.1906.09611","open_access":"1"}],"oa_version":"Preprint","publication":"arXiv","language":[{"iso":"eng"}],"oa":1,"doi":"10.48550/arXiv.1906.09611"},{"arxiv":1,"acknowledgement":"We thank the anonymous referee for the very useful comments. We would also like to thank M. Benbakoura for his help in analyzing the light curves of several binary systems included in our set of stars. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support from the National Aeronautics and Space Administration under Grant NNX15AF13G, the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship no. RYC-2015-17697. E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement no. 664931. O.J.H and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106). This research has made use of NASA’s Astrophysics Data System. Data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.","status":"public","extern":"1","month":"12","date_updated":"2024-10-14T11:40:17Z","volume":620,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"day":"01","year":"2018","oa_version":"Preprint","publication":"Astronomy & Astrophysics","scopus_import":"1","language":[{"iso":"eng"}],"article_number":"A38","external_id":{"arxiv":["1809.05105"]},"intvolume":"       620","author":[{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000"},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"full_name":"Davies, G. R.","first_name":"G. R.","last_name":"Davies"},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"full_name":"Corsaro, E.","last_name":"Corsaro","first_name":"E."},{"full_name":"Hall, O. J.","first_name":"O. J.","last_name":"Hall"},{"first_name":"B. M.","last_name":"Rendle","full_name":"Rendle, B. M."}],"date_created":"2022-07-18T14:37:39Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants","date_published":"2018-12-01T00:00:00Z","article_processing_charge":"No","citation":{"chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, E. Corsaro, O. J. Hall, and B. M. Rendle. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201833106\">https://doi.org/10.1051/0004-6361/201833106</a>.","apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Corsaro, E., Hall, O. J., &#38; Rendle, B. M. (2018). FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833106\">https://doi.org/10.1051/0004-6361/201833106</a>","ista":"Bugnet LA, García RA, Davies GR, Mathur S, Corsaro E, Hall OJ, Rendle BM. 2018. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy &#38; Astrophysics. 620, A38.","short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, E. Corsaro, O.J. Hall, B.M. Rendle, Astronomy &#38; Astrophysics 620 (2018).","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” <i>Astronomy &#38; Astrophysics</i>, vol. 620, A38, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833106\">10.1051/0004-6361/201833106</a>.","ama":"Bugnet LA, García RA, Davies GR, et al. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. <i>Astronomy &#38; Astrophysics</i>. 2018;620. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833106\">10.1051/0004-6361/201833106</a>","ieee":"L. A. Bugnet <i>et al.</i>, “FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants,” <i>Astronomy &#38; Astrophysics</i>, vol. 620. EDP Sciences, 2018."},"article_type":"original","abstract":[{"text":"Asteroseismology provides global stellar parameters such as masses, radii, or surface gravities using mean global seismic parameters and effective temperature for thousands of low-mass stars (0.8 M⊙ < M < 3 M⊙). This methodology has been successfully applied to stars in which acoustic modes excited by turbulent convection are measured. Other methods such as the Flicker technique can also be used to determine stellar surface gravities, but only works for log g above 2.5 dex. In this work, we present a new metric called FliPer (Flicker in spectral power density, in opposition to the standard Flicker measurement which is computed in the time domain); it is able to extend the range for which reliable surface gravities can be obtained (0.1 < log g < 4.6 dex) without performing any seismic analysis for stars brighter than Kp < 14. FliPer takes into account the average variability of a star measured in the power density spectrum in a given range of frequencies. However, FliPer values calculated on several ranges of frequency are required to better characterize a star. Using a large set of asteroseismic targets it is possible to calibrate the behavior of surface gravity with FliPer through machine learning. This calibration made with a random forest regressor covers a wide range of surface gravities from main-sequence stars to subgiants and red giants, with very small uncertainties from 0.04 to 0.1 dex. FliPer values can be inserted in automatic global seismic pipelines to either give an estimation of the stellar surface gravity or to assess the quality of the seismic results by detecting any outliers in the obtained νmax values. FliPer also constrains the surface gravities of main-sequence dwarfs using only long-cadence data for which the Nyquist frequency is too low to measure the acoustic-mode properties.","lang":"eng"}],"_id":"11618","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / methods","data analysis / stars","oscillations"],"main_file_link":[{"url":"https://arxiv.org/abs/1809.05105","open_access":"1"}],"publication_status":"published","type":"journal_article","quality_controlled":"1","doi":"10.1051/0004-6361/201833106","oa":1,"publisher":"EDP Sciences"},{"date_updated":"2022-08-22T07:45:38Z","volume":478,"month":"08","extern":"1","status":"public","acknowledgement":"We gratefully acknowledge many helpful suggestions by the anonymous referee. Based on observations made with a) the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos; b) the ESO-3.6m telescope at La Silla Observatory under programme ID 0100.C-0808; c) the Italian Telescopio Nazionale Galileo operated on the island of La Palma by the Fundación Galileo Galilei of the Istituto Nazionale di Astrofisica. NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 730890. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. DG gratefully acknowledges the financial support of the Programma Giovani Ricercatori – Rita Levi Montalcini – Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR). SaM would like to acknowledge support from the Ramon y Cajal fellowship number RYC-2015-17697. AJ, MH, and SA acknowledge support by the Danish Council for Independent Research, through a DFF Sapere Aude Starting Grant nr. 4181-00487B. SzCs, APH, MP, and HR acknowledge the support of the DFG priority program SPP 1992Exploring the Diversity of Extrasolar Planets (grants HA 3279/12-1, PA 525/18-1, PA5 25/19-1 and PA525/20-1, RA 714/14-1) HD, CR, and FPH acknowledge the financial support from MINECO under grants ESP2015-65712-C5-4-R and AYA2016-76378-P. This paper has made use of the IAC Supercomputing facility HTCondor (http://research.cs.wisc.edu/htcondor/), partly financed by the Ministry of Economy and Competitiveness with FEDER funds, code IACA13-3E-2493. MF and CMP gratefully acknowledge the support of the Swedish National Space Board. RAG and StM thanks the support of the CNES PLATO grant. PGB is a postdoctoral fellow in the MINECO-programme ’Juan de la Cierva Incorporacion’ (IJCI-2015-26034). StM acknowledges support from ERC through SPIRE grant (647383) and from ISSI through the ENCELADE 2.0 team. VSA acknowledges support from VILLUM FONDEN (research grant 10118). MNL acknowledges support from the ESA-PRODEX programme. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106) This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research was made with the use of NASA’s Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.","page":"4866-4880","arxiv":1,"language":[{"iso":"eng"}],"scopus_import":"1","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","year":"2018","day":"01","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"title":"HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2022-07-18T14:43:17Z","author":[{"last_name":"Van Eylen","first_name":"V","full_name":"Van Eylen, V"},{"first_name":"F","last_name":"Dai","full_name":"Dai, F"},{"full_name":"Mathur, S","first_name":"S","last_name":"Mathur"},{"first_name":"D","last_name":"Gandolfi","full_name":"Gandolfi, D"},{"last_name":"Albrecht","first_name":"S","full_name":"Albrecht, S"},{"last_name":"Fridlund","first_name":"M","full_name":"Fridlund, M"},{"full_name":"García, R A","first_name":"R A","last_name":"García"},{"last_name":"Guenther","first_name":"E","full_name":"Guenther, E"},{"full_name":"Hjorth, M","last_name":"Hjorth","first_name":"M"},{"full_name":"Justesen, A B","first_name":"A B","last_name":"Justesen"},{"full_name":"Livingston, J","first_name":"J","last_name":"Livingston"},{"first_name":"M N","last_name":"Lund","full_name":"Lund, M N"},{"last_name":"Pérez Hernández","first_name":"F","full_name":"Pérez Hernández, F"},{"full_name":"Prieto-Arranz, J","first_name":"J","last_name":"Prieto-Arranz"},{"full_name":"Regulo, C","first_name":"C","last_name":"Regulo"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle"},{"last_name":"Everett","first_name":"M E","full_name":"Everett, M E"},{"first_name":"T","last_name":"Hirano","full_name":"Hirano, T"},{"last_name":"Nespral","first_name":"D","full_name":"Nespral, D"},{"last_name":"Nowak","first_name":"G","full_name":"Nowak, G"},{"full_name":"Palle, E","first_name":"E","last_name":"Palle"},{"full_name":"Silva Aguirre, V","first_name":"V","last_name":"Silva Aguirre"},{"full_name":"Trifonov, T","last_name":"Trifonov","first_name":"T"},{"full_name":"Winn, J N","last_name":"Winn","first_name":"J N"},{"last_name":"Barragán","first_name":"O","full_name":"Barragán, O"},{"last_name":"Beck","first_name":"P G","full_name":"Beck, P G"},{"full_name":"Chaplin, W J","last_name":"Chaplin","first_name":"W J"},{"first_name":"W D","last_name":"Cochran","full_name":"Cochran, W D"},{"full_name":"Csizmadia, S","last_name":"Csizmadia","first_name":"S"},{"first_name":"H","last_name":"Deeg","full_name":"Deeg, H"},{"full_name":"Endl, M","last_name":"Endl","first_name":"M"},{"first_name":"P","last_name":"Heeren","full_name":"Heeren, P"},{"last_name":"Grziwa","first_name":"S","full_name":"Grziwa, S"},{"full_name":"Hatzes, A P","last_name":"Hatzes","first_name":"A P"},{"last_name":"Hidalgo","first_name":"D","full_name":"Hidalgo, D"},{"full_name":"Korth, J","last_name":"Korth","first_name":"J"},{"last_name":"Mathis","first_name":"S","full_name":"Mathis, S"},{"full_name":"Montañes Rodriguez, P","first_name":"P","last_name":"Montañes Rodriguez"},{"full_name":"Narita, N","last_name":"Narita","first_name":"N"},{"full_name":"Patzold, M","last_name":"Patzold","first_name":"M"},{"first_name":"C M","last_name":"Persson","full_name":"Persson, C M"},{"last_name":"Rodler","first_name":"F","full_name":"Rodler, F"},{"full_name":"Smith, A M S","first_name":"A M S","last_name":"Smith"}],"issue":"4","external_id":{"arxiv":["1805.01860"]},"intvolume":"       478","oa":1,"publisher":"Oxford University Press","doi":"10.1093/mnras/sty1390","quality_controlled":"1","type":"journal_article","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.01860"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","planets and satellites: composition","planets and satellites: formation","planets and satellites: fundamental parameters"],"_id":"11620","abstract":[{"text":"We report the discovery and characterization of HD 89345b (K2-234b; EPIC 248777106b), a Saturn-sized planet orbiting a slightly evolved star. HD 89345 is a bright star (V = 9.3 mag) observed by the K2 mission with 1 min time sampling. It exhibits solar-like oscillations. We conducted asteroseismology to determine the parameters of the star, finding the mass and radius to be 1.12+0.04−0.01M⊙ and 1.657+0.020−0.004R⊙⁠, respectively. The star appears to have recently left the main sequence, based on the inferred age, 9.4+0.4−1.3Gyr⁠, and the non-detection of mixed modes. The star hosts a ‘warm Saturn’ (P = 11.8 d, Rp = 6.86 ± 0.14 R⊕). Radial-velocity follow-up observations performed with the FIbre-fed Echelle Spectrograph, HARPS, and HARPS-N spectrographs show that the planet has a mass of 35.7 ± 3.3 M⊕. The data also show that the planet’s orbit is eccentric (e ≈ 0.2). An investigation of the rotational splitting of the oscillation frequencies of the star yields no conclusive evidence on the stellar inclination angle. We further obtained Rossiter–McLaughlin observations, which result in a broad posterior of the stellar obliquity. The planet seems to confirm to the same patterns that have been observed for other sub-Saturns regarding planet mass and multiplicity, orbital eccentricity, and stellar metallicity.","lang":"eng"}],"article_type":"original","citation":{"ista":"Van Eylen V, Dai F, Mathur S, Gandolfi D, Albrecht S, Fridlund M, García RA, Guenther E, Hjorth M, Justesen AB, Livingston J, Lund MN, Pérez Hernández F, Prieto-Arranz J, Regulo C, Bugnet LA, Everett ME, Hirano T, Nespral D, Nowak G, Palle E, Silva Aguirre V, Trifonov T, Winn JN, Barragán O, Beck PG, Chaplin WJ, Cochran WD, Csizmadia S, Deeg H, Endl M, Heeren P, Grziwa S, Hatzes AP, Hidalgo D, Korth J, Mathis S, Montañes Rodriguez P, Narita N, Patzold M, Persson CM, Rodler F, Smith AMS. 2018. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. 478(4), 4866–4880.","short":"V. Van Eylen, F. Dai, S. Mathur, D. Gandolfi, S. Albrecht, M. Fridlund, R.A. García, E. Guenther, M. Hjorth, A.B. Justesen, J. Livingston, M.N. Lund, F. Pérez Hernández, J. Prieto-Arranz, C. Regulo, L.A. Bugnet, M.E. Everett, T. Hirano, D. Nespral, G. Nowak, E. Palle, V. Silva Aguirre, T. Trifonov, J.N. Winn, O. Barragán, P.G. Beck, W.J. Chaplin, W.D. Cochran, S. Csizmadia, H. Deeg, M. Endl, P. Heeren, S. Grziwa, A.P. Hatzes, D. Hidalgo, J. Korth, S. Mathis, P. Montañes Rodriguez, N. Narita, M. Patzold, C.M. Persson, F. Rodler, A.M.S. Smith, Monthly Notices of the Royal Astronomical Society 478 (2018) 4866–4880.","chicago":"Van Eylen, V, F Dai, S Mathur, D Gandolfi, S Albrecht, M Fridlund, R A García, et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty1390\">https://doi.org/10.1093/mnras/sty1390</a>.","apa":"Van Eylen, V., Dai, F., Mathur, S., Gandolfi, D., Albrecht, S., Fridlund, M., … Smith, A. M. S. (2018). HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty1390\">https://doi.org/10.1093/mnras/sty1390</a>","ieee":"V. Van Eylen <i>et al.</i>, “HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 4. Oxford University Press, pp. 4866–4880, 2018.","mla":"Van Eylen, V., et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 4, Oxford University Press, 2018, pp. 4866–80, doi:<a href=\"https://doi.org/10.1093/mnras/sty1390\">10.1093/mnras/sty1390</a>.","ama":"Van Eylen V, Dai F, Mathur S, et al. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(4):4866-4880. doi:<a href=\"https://doi.org/10.1093/mnras/sty1390\">10.1093/mnras/sty1390</a>"},"article_processing_charge":"No","date_published":"2018-08-01T00:00:00Z"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2022-07-21T07:05:23Z","author":[{"orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"last_name":"Davies","first_name":"G. R.","full_name":"Davies, G. R."},{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"full_name":"Hall, O. J.","last_name":"Hall","first_name":"O. J."},{"last_name":"Rendle","first_name":"B. M.","full_name":"Rendle, B. M."}],"title":"FliPer: Classifying TESS pulsating stars","date_updated":"2022-08-22T08:41:55Z","external_id":{"arxiv":["1811.12140"]},"arxiv":1,"article_number":"1811.12140","month":"11","extern":"1","status":"public","type":"preprint","publication_status":"submitted","oa_version":"Preprint","publication":"arXiv","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1811.12140"}],"oa":1,"doi":"10.48550/arXiv.1811.12140","language":[{"iso":"eng"}],"day":"29","citation":{"ista":"Bugnet LA, García RA, Davies GR, Mathur S, Hall OJ, Rendle BM. FliPer: Classifying TESS pulsating stars. arXiv, 1811.12140.","short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, O.J. Hall, B.M. Rendle, ArXiv (n.d.).","apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Hall, O. J., &#38; Rendle, B. M. (n.d.). FliPer: Classifying TESS pulsating stars. <i>arXiv</i>. <a href=\"https://doi.org/10.48550/arXiv.1811.12140\">https://doi.org/10.48550/arXiv.1811.12140</a>","chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, O. J. Hall, and B. M. Rendle. “FliPer: Classifying TESS Pulsating Stars.” <i>ArXiv</i>, n.d. <a href=\"https://doi.org/10.48550/arXiv.1811.12140\">https://doi.org/10.48550/arXiv.1811.12140</a>.","ieee":"L. A. Bugnet, R. A. García, G. R. Davies, S. Mathur, O. J. Hall, and B. M. Rendle, “FliPer: Classifying TESS pulsating stars,” <i>arXiv</i>. .","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: Classifying TESS Pulsating Stars.” <i>ArXiv</i>, 1811.12140, doi:<a href=\"https://doi.org/10.48550/arXiv.1811.12140\">10.48550/arXiv.1811.12140</a>.","ama":"Bugnet LA, García RA, Davies GR, Mathur S, Hall OJ, Rendle BM. FliPer: Classifying TESS pulsating stars. <i>arXiv</i>. doi:<a href=\"https://doi.org/10.48550/arXiv.1811.12140\">10.48550/arXiv.1811.12140</a>"},"date_published":"2018-11-29T00:00:00Z","article_processing_charge":"No","keyword":["asteroseismology - methods","data analysis - stars","oscillations"],"_id":"11631","year":"2018","abstract":[{"lang":"eng","text":"The recently launched NASA Transiting Exoplanet Survey Satellite (TESS) mission is going to collect lightcurves for a few hundred million of stars and we expect to increase the number of pulsating stars to analyze compared to the few thousand stars observed by the CoRoT, Kepler and K2 missions. However, most of the TESS targets have not yet been properly classified and characterized. In order to improve the analysis of the TESS data, it is crucial to determine the type of stellar pulsations in a timely manner. We propose an automatic method to classify stars attending to their pulsation properties, in particular, to identify solar-like pulsators among all TESS targets. It relies on the use of the global amount of power contained in the power spectrum (already known as the FliPer method) as a key parameter, along with\r\nthe effective temperature, to feed into a machine learning classifier. Our study, based on TESS simulated datasets, shows that we are able to classify pulsators with a 98% accuracy."}]},{"date_created":"2022-07-21T07:13:13Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"last_name":"Bugnet","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"R. A.","last_name":"Garcia","full_name":"Garcia, R. A."},{"first_name":"G. R.","last_name":"Davies","full_name":"Davies, G. R."},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"last_name":"Corsaro","first_name":"E.","full_name":"Corsaro, E."}],"title":"FliPer: Checking the reliability of global seismic parameters from automatic pipelines","date_updated":"2022-08-22T08:45:42Z","external_id":{"arxiv":["1711.02890"]},"arxiv":1,"article_number":"1711.02890","extern":"1","month":"11","status":"public","type":"preprint","publication_status":"submitted","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.1711.02890"}],"oa_version":"Preprint","publication":"arXiv","language":[{"iso":"eng"}],"oa":1,"doi":"10.48550/arXiv.1711.02890","date_published":"2017-11-08T00:00:00Z","article_processing_charge":"No","citation":{"ama":"Bugnet LA, Garcia RA, Davies GR, Mathur S, Corsaro E. FliPer: Checking the reliability of global seismic parameters from automatic pipelines. <i>arXiv</i>. doi:<a href=\"https://doi.org/10.48550/arXiv.1711.02890\">10.48550/arXiv.1711.02890</a>","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: Checking the Reliability of Global Seismic Parameters from Automatic Pipelines.” <i>ArXiv</i>, 1711.02890, doi:<a href=\"https://doi.org/10.48550/arXiv.1711.02890\">10.48550/arXiv.1711.02890</a>.","ieee":"L. A. Bugnet, R. A. Garcia, G. R. Davies, S. Mathur, and E. Corsaro, “FliPer: Checking the reliability of global seismic parameters from automatic pipelines,” <i>arXiv</i>. .","chicago":"Bugnet, Lisa Annabelle, R. A. Garcia, G. R. Davies, S. Mathur, and E. Corsaro. “FliPer: Checking the Reliability of Global Seismic Parameters from Automatic Pipelines.” <i>ArXiv</i>, n.d. <a href=\"https://doi.org/10.48550/arXiv.1711.02890\">https://doi.org/10.48550/arXiv.1711.02890</a>.","apa":"Bugnet, L. A., Garcia, R. A., Davies, G. R., Mathur, S., &#38; Corsaro, E. (n.d.). FliPer: Checking the reliability of global seismic parameters from automatic pipelines. <i>arXiv</i>. <a href=\"https://doi.org/10.48550/arXiv.1711.02890\">https://doi.org/10.48550/arXiv.1711.02890</a>","short":"L.A. Bugnet, R.A. Garcia, G.R. Davies, S. Mathur, E. Corsaro, ArXiv (n.d.).","ista":"Bugnet LA, Garcia RA, Davies GR, Mathur S, Corsaro E. FliPer: Checking the reliability of global seismic parameters from automatic pipelines. arXiv, 1711.02890."},"day":"08","keyword":["asteroseismology - methods","data analysis - stars","oscillations"],"abstract":[{"lang":"eng","text":"Our understanding of stars through asteroseismic data analysis is limited by our ability to take advantage of the huge amount of observed stars provided by space missions such as CoRoT, Kepler , K2, and soon TESS and PLATO. Global seismic pipelines provide global stellar parameters such as mass and radius using the mean seismic parameters, as well as the effective temperature. These pipelines are commonly used automatically on thousands of stars observed by K2 for 3 months (and soon TESS for at least ∼ 1 month). However, pipelines are not immune from misidentifying noise peaks and stellar oscillations. Therefore, new validation techniques are required to assess the quality of these results. We present a new metric called FliPer (Flicker in Power), which takes into account the average variability at all measured time scales. The proper calibration of FliPer enables us to obtain good estimations of global stellar parameters such as surface gravity that are robust against the influence of noise peaks and hence are an excellent way to find faults in asteroseismic pipelines."}],"_id":"11633","year":"2017"}]