@inbook{21230, abstract = {Asteroseismology is the study of the interior physics and structure of stars using their pulsations. It is applicable to stars across the Hertzsprung–Russell (HR) diagram and a powerful technique not only to measure masses, radii, and ages but also directly constrain interior rotation, chemical mixing, and magnetism. This is because a star's self-excited pulsation modes are sensitive to its structure. Asteroseismology generally requires long-duration and high-precision time-series data. The method of forward asteroseismic modeling, which is the statistical comparison of observed pulsation mode frequencies to theoretically predicted pulsation frequencies calculated from a grid of models, provides precise constraints for calibrating various transport phenomena. In this introduction to asteroseismology, we provide an overview of its principles, and the typical data sets and methodologies used to constrain stellar interiors. Finally, we present key highlights of asteroseismic results from across the HR diagram, and conclude with ongoing challenges and future prospects for this ever-expanding field within stellar astrophysics.}, author = {Bowman, Dominic M. and Bugnet, Lisa Annabelle}, booktitle = {Encyclopedia of Astrophysics}, editor = {Mandel, Ilya}, isbn = {9780443214400}, pages = {133--153}, publisher = {Elsevier}, title = {{Asteroseismology}}, doi = {10.1016/b978-0-443-21439-4.00036-5}, volume = {2}, year = {2026}, } @article{21658, abstract = {Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential rotation between the core and the envelope of evolved solar-like stars. Quadrupolar (ℓ = 2) mixed modes also contain information regarding internal dynamics but are very rarely characterised due to their low amplitude and the challenging identification of adjacent or overlapping rotationally split multiplets affected by near-degeneracy effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed modes while explicitly accounting for near-degeneracy effects that distort their rotational multiplets. We have derived a new asymptotic formulation of near-degenerate mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction between modes of adjacent radial orders. This formalism, expressed directly in the mixed-mode basis, provides analytical expressions for the near-degeneracy effects. We implemented the formalism within a global Bayesian mode-fitting framework for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were able to asymptotically model the asymmetric rotational splitting present in various radial orders of ℓ = 2 modes observed in young red giant stars without the need for any numerical stellar modelling. We applied our formalism to the Kepler target KIC 7341231, and it yielded core and envelope rotation rates consistent with previous numerical modelling while providing improved constraints from the global and model-independent approach. We also characterised the new target, KIC 8179973, measuring its rotation rate and mixed-mode parameters for the first time. As our framework relies on a direct global fit, it allows for much better precision on the asteroseismic parameters and rotation rate estimates than standard methods, yielding better constraints for rotation inversions. We have placed the first observational constraints on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes.}, author = {Liagre, Bastien Raymond Bernard and Desai, Aayush A and Einramhof, Lukas and Bugnet, Lisa Annabelle}, issn = {1432-0746}, journal = {Astronomy and Astrophysics}, publisher = {EDP Sciences}, title = {{Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting}}, doi = {10.1051/0004-6361/202558023}, volume = {707}, year = {2026}, } @article{21659, abstract = {The recent detection of solar equatorial Rossby waves has renewed interest in the study of gravito-inertial waves propagating in the convective envelope of solar-type stars. In particular, the ability of these envelope gravito-inertial modes to couple with those trapped in the radiative interior could open up new opportunities for probing the deep-layer dynamics of solar-type stars. The possibility for such a coupling to occur is particularly favoured among pre-main-sequence (PMS) solar-type stars. Indeed, due to the contraction of the protostellar object, they are able to reach high rotation frequencies before nuclear reactions are ignited and magnetic braking becomes the driving mechanism for their rotational evolution. In this work, we studied the coupling between the envelope inertial waves and the radiative interior g modes in PMS stars, focussing on the case of prograde dipolar modes. We considered the cases of 0.5 M⊙ and 1 M⊙ PMS models, each with three different scenarios of rotational evolution. We show that for stars that have formed with a sufficient amount of angular momentum, this coupling can occur in frequency ranges that are accessible to space-borne photometry, creating inertial dips in the period spacing pattern. Using an asymptotic analysis, we characterised the shape of these inertial dips to show that they depend on rotation and on the stiffness of the convective-radiative interface.}, author = {Breton, S. N. and Pezzotti, C. and Mathis, S. and Bugnet, Lisa Annabelle and Di Mauro, M. P. and Joergensen, J. and Zwintz, K. and Lanza, A. F.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {Wiley}, title = {{Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars}}, doi = {10.1051/0004-6361/202659309}, volume = {707}, year = {2026}, } @article{21760, abstract = {3I/ATLAS is the third interstellar object discovered to date, following 1I/‘Oumuamua and 2I/Borisov. Its unusually high excess velocity and active cometary nature make it a key probe of the Galactic population of icy planetesimals. Understanding its origin requires its past trajectory through the Galaxy to be traced and the possible role of stellar encounters to be assessed, both as a potential origin and a perturber to its orbit. We integrated the orbit of 3I/ATLAS backward in time for 10 Myr, together with a sample of Gaia DR3 stars with high-quality astrometry and radial velocities, to identify close passages within 2 pc. We identify 93 nominal encounters, 62 of which are significant at the 2σ level. However, none of these encounters produced any meaningful perturbation. The strongest perturber Gaia DR3 6863591389529611264 at 0.30 pc and with a relative velocity of 35 km s−1, imparted only a velocity change of ∣Δv∣ ≃ 5 × 10−4 km s−1 to the orbit of 3I/ATLAS. Our results indicate that no stellar flybys within the past 10 Myr and 500 pc contained in Gaia DR3 can account for the present trajectory of 3I/ATLAS or be associated with its origin. We further show that 3I/ATLAS is kinematically consistent with a thin-disk population, despite its large peculiar velocity.}, author = {Pérez-Couto, X. and Torres Rodriguez, Santiago and Villaver, E. and Mustill, A. J. and Manteiga, M.}, issn = {1538-4357}, journal = {The Astrophysical Journal}, number = {2}, publisher = {IOP Publishing}, title = {{3I/ATLAS: In search of the witnesses to its voyage}}, doi = {10.3847/1538-4357/ae56ff}, volume = {1001}, year = {2026}, } @article{20350, abstract = {Context. Rotation plays an important role in stellar evolution. However, the mechanisms behind the transport of angular momentum in stars at various stages of their evolution are not well understood. To improve our understanding of these processes, it is necessary to measure and validate the internal rotation profiles of stars across different stages of evolution and mass regimes. Aims. Our aim is to constrain the internal rotation profile of the 12-M⊙ β Cep pulsator HD 192575 from the observed pulsational multiplets and the asymmetries of their component frequencies. Methods. We updated the forward asteroseismic modelling of HD 192575 based on new TESS observations. We inverted the rotation profile from the symmetric part of the splittings and computed the multiplet asymmetries due to the Coriolis force and stellar deformation, which we treated perturbatively. We compared the computed asymmetries with the observed asymmetries. Results. Our new forward asteroseismic modelling is in agreement with previous results but with increased uncertainties, partially due to increased frequency precision, which required us to relax certain constraints. Ambiguity in the mode identification is the main source of the uncertainty, which also affects the inferred rotation profiles. Almost all acceptable rotation profiles occur in the regime below 0.4 d−1 and favour weak radial differential rotation, with a ratio of core to envelope rotation of less than 2. We find that the quality of the match between the observed and theoretically predicted mode asymmetries is strongly dependent on the mode identification and the internal structure of the star. Conclusions. Our results offer the first detailed rotation inversion for a β Cep pulsator. They show that the rotation profile and the mode asymmetries provide a valuable tool for further constraining the evolutionary properties of HD 192575, and in particular the details of angular momentum transport in massive stars.}, author = {Vanlaer, V. and Bowman, D. M. and Burssens, S. and Das, Srijan B and Bugnet, Lisa Annabelle and Mathis, S. and Aerts, C.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries}}, doi = {10.1051/0004-6361/202452885}, volume = {701}, year = {2025}, } @article{20454, abstract = {Context. γ Dor stars are ideal targets for studies of the innermost dynamical properties of stars, due to their rich asteroseismic spectrum of gravity modes. Integrating internal magnetism to the picture appears as the next milestone of detailed asteroseismic studies, for its prime importance on stellar evolution. The inertial dip in prograde dipole modes period-spacing pattern of γ Dors stands out as a unique window on the convective core structure and dynamics. Recent studies have highlighted the dependence of the dip structure on core density stratification, the contrast of the near-core Brunt-Väisälä frequency and rotation rate, as well as the core-to-near-core differential rotation. In addition, the effect of envelope magnetism has been derived on low-frequency magneto-gravito-inertial waves. Aims. We revisited the inertial dip formation including core and envelope magnetism, and explored the probing power of this feature on dynamo-generated core fields. Methods. We considered as a first step a toroidal magnetic field with a bi-layer (core and envelope) Alfvén frequency. This configuration allowed us to revisit the coupling problem using our knowledge on both core magneto-inertial modes and envelope magneto-gravito-inertial modes. Using this configuration, we were able to stay in an analytical framework to exhibit the magnetic effects on the inertial dip shape and location. This configuration allowed a laboratory to be set up that moves us towards the comprehension of magnetic effects on the dip structure. Results. We show a shift of the inertial dip towards lower spin parameter values and a thinner dip with increasing core magnetic field’s strength, quite similar to the signature of differential rotation. The magnetic effects become sizeable when the ratio of the magnetic to the Coriolis effects is high enough. We explored the potential degeneracy of the magnetic effects with differential rotation. We studied the detectability of core magnetism, considering both observational constraints on the periods of the modes and potential gravito-inertial mode suppression.}, author = {Barrault, Lucas and Bugnet, Lisa Annabelle and Mathis, S. and Mombarg, J. S.G.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{Exploring the probing power of γ Dor's inertial dip for core magnetism: The case of a toroidal field}}, doi = {10.1051/0004-6361/202555213}, volume = {701}, year = {2025}, } @article{18984, abstract = {Although planets have been found orbiting binary systems, whether they can survive binary interactions is debated. While the tightest-orbit binaries should host the most dynamically stable and long-lived circumbinary planetary systems, they are also the systems that are expected to experience mass transfer, common envelope evolution, or stellar mergers. In this study, we explore the effect of stable non-conservative mass transfer on the dynamical evolution of circumbinary planets. We present a new script that seamlessly integrates binary evolution data from the 1D binary stellar evolution code MESA into the N-body simulation code REBOUND. This integration framework enables a comprehensive examination of the dynamical evolution of circumbinary planets orbiting mass-transferring binaries, while simultaneously accounting for the detailed stellar structure evolution. In addition, we introduce a recalibration method to mitigate numerical errors from updates of binary properties during the system's dynamical evolution. We construct a reference binary model in which a 2.21M⊙ star loses its hydrogen-rich envelope through non-conservative mass transfer to the 1.76M⊙ companion star, creating a 0.38M⊙ subdwarf. We find the tightest stable orbital separation for circumbinary planets to be ≃2.5 times the binary separation after mass transfer. Accounting for tides by using the interior stellar structure, we find that tidal effects become apparent after the rapid mass transfer phase and start to fade away during the latter stage of the slow mass transfer phase. Our research provides a new framework for exploring circumbinary planet dynamics in interacting binary systems.}, author = {Xing, Zepei and Torres Rodriguez, Santiago and Götberg, Ylva Louise Linsdotter and Trani, Alessandro A. and Korol, Valeriya and Cuadra, Jorge}, issn = {1365-2966}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {1}, pages = {285--292}, publisher = {Oxford University Press}, title = {{Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries}}, doi = {10.1093/mnras/stae2820}, volume = {537}, year = {2025}, } @article{19283, abstract = {Context. The presence of dips in the gravity mode period spacing versus period diagram of γ Doradus stars is now well established thanks to recent asteroseismic studies. Such Lorentzian-shaped inertial dips arise from the interaction of gravito-inertial modes in the radiative envelope of intermediate-mass main sequence stars with pure inertial modes in their convective core, and allow us to study stellar internal properties. This window onto stellar internal dynamics is extremely valuable in the context of the understanding of angular-momentum transport inside stars, as it allows us to probe rotation in their core. Aims. We investigate the signature and the detectability of a differential rotation between the convective core and the near-core region inside γ Doradus stars from the properties of inertial dips. Methods. We studied the coupling between gravito-inertial modes in the radiative zone and pure inertial modes in the convective core in the sub-inertial regime, allowing for a two-zone differential rotation from the two sides of the core-to-envelope boundary. We solved the coupling equation numerically and matched the result to an analytical derivation of the Lorentzian dip properties. We then used typical values of measured near-core rotation and buoyancy travel time to infer ranges of parameters for which differential core to near-core rotation would be detectable in current Kepler data. Results. We show that increasing the convective core rotation with respect to the near-core rotation leads to a shift of the period of the observed dip to lower periods. In addition, the dip gets deeper and thinner as the convective core rotation increases. We demonstrate that such a signature is detectable in Kepler data, given appropriate dip-parameter ranges and near-core structural properties. Conclusions. Studying the dip properties in asteroseismic data thus allows us to access core to near-core radial differential rotation and to better understand the transport of angular momentum at convective–radiative interfaces in intermediate-mass main sequence stars.}, author = {Barrault, Lucas and Mathis, S. and Bugnet, Lisa Annabelle}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{Constraining differential rotation in γ Doradus stars from the properties of inertial dips}}, doi = {10.1051/0004-6361/202451541}, volume = {694}, year = {2025}, } @article{19405, abstract = {In the third APOKASC catalog, we present data for the complete sample of 15,808 evolved stars with APOGEE spectroscopic parameters and Kepler asteroseismology. We used 10 independent asteroseismic analysis techniques and anchor our system on fundamental radii derived from Gaia L and spectroscopic Teff. We provide evolutionary state, asteroseismic surface gravity, mass, radius, age, and the data used to derive them for 12,418 stars. This includes 10,036 exceptionally precise measurements, with median fractional uncertainties in vmax, Δν, mass, radius, and age of 0.6%, 0.6%, 3.8%, 1.8%, and 11.1%, respectively. We provide more limited data for 1624 additional stars that either have lower-quality data or are outside of our primary calibration domain. Using lower red giant branch (RGB) stars, we find a median age for the chemical thick disk of 9.14 ± 0.05(ran) ± 0.9(sys) Gyr with an age dispersion of 1.1 Gyr, consistent with our error model. We calibrate our red clump (RC) mass loss to derive an age consistent with the lower RGB and provide asymptotic GB and RGB ages for luminous stars. We also find a sharp upper-age boundary in the chemical thin disk. We find that scaling relations are precise and accurate on the lower RGB and RC, but they become more model dependent for more luminous giants and break down at the tip of the RGB. We recommend the use of multiple methods, calibration to a fundamental scale, and the use of stellar models to interpret frequency spacings.}, author = {Pinsonneault, Marc H. and Zinn, Joel C. and Tayar, Jamie and Serenelli, Aldo and García, Rafael A. and Mathur, Savita and Vrard, Mathieu and Elsworth, Yvonne P. and Mosser, Benoit and Stello, Dennis and Bell, Keaton J. and Bugnet, Lisa Annabelle and Corsaro, Enrico and Gaulme, Patrick and Hekker, Saskia and Hon, Marc and Huber, Daniel and Kallinger, Thomas and Cao, Kaili and Johnson, Jennifer A. and Liagre, Bastien and Patton, Rachel A. and Santos, Ângela R.G. and Basu, Sarbani and Beck, Paul G. and Beers, Timothy C. and Chaplin, William J. and Cunha, Katia and Frinchaboy, Peter M. and Girardi, Léo and Godoy-Rivera, Diego and Holtzman, Jon A. and Jönsson, Henrik and Mészáros, Szabolcs and Reyes, Claudia and Rix, Hans Walter and Shetrone, Matthew and Smith, Verne V. and Spoo, Taylor and Stassun, Keivan G. and Wang, Ji}, issn = {0067-0049}, journal = {Astrophysical Journal, Supplement Series}, number = {2}, publisher = {IOP Publishing}, title = {{APOKASC-3: The third joint spectroscopic and asteroseismic catalog for evolved stars in the Kepler fields}}, doi = {10.3847/1538-4365/ad9fef}, volume = {276}, year = {2025}, } @article{20930, abstract = {Context. Beta Pictoris is an A-type star that hosts a complex planetary system with two massive gas giants and a prominent debris disc. Variable absorption lines in its stellar spectrum have been interpreted as signatures of exocomets – comet-like bodies transiting the star. Stellar flybys can gravitationally perturb objects in the outer comet reservoir, altering their orbits and potentially injecting them into the inner system, thereby triggering exocomet showers. Aims. We assessed the contribution of stellar flybys to the observed exocomet activity by reconstructing the stellar encounter history of β Pictoris in the past and future. Methods. We used Gaia DR3 data, supplemented with radial velocities from complementary spectroscopic surveys, to compile a catalogue of stars currently within 80 pc of β Pictoris. Their orbits were integrated backwards and forwards in time in an axisymmetric Galactic potential (via the GALA package) to identify encounters within 2 pc of the system. Results. We identified 99 416 stars currently within 80 pc of β Pictoris with resolved kinematics. Among these, 49 stars (including the eight components of five binaries) encounter β Pictoris within 2 pc between –1.5 Myr and +2 Myr. For four of the binaries, the centre-of-mass trajectories also pass within 2 pc. We estimated the sample to be more than 60% complete within 0.5 Myr of today. Conclusions. Despite β Pictoris being the eponym of its famous moving group, none of the identified encounters involved its moving group members; all are unrelated field stars. We found no encounter capable of shaping the observed disc structures, although stellar flybys may contribute to the long-term evolution of an Oort Cloud-like structure. Our catalogue constitutes the most complete reconstruction of the β Pictoris encounter history to date and provides a robust foundation for future dynamical simulations.}, author = {Gragera-Más, J. L. and Torres Rodriguez, Santiago and Mustill, A. J. and Villaver, E.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{A kinematic history of stellar encounters with Beta Pictoris}}, doi = {10.1051/0004-6361/202555940}, volume = {704}, year = {2025}, } @article{20931, abstract = {Context. Asymmetries in the observed rotational splittings of a multiplet contain information about the star’s rotation profile and internal magnetic field. Moreover, the frequency regularities of multiplets can be used for mode identification. However, to exploit this information, highly accurate theoretical predictions are needed. Aims. We aim to quantify the difference in the predicted mode asymmetries between a 1D perturbative method and a 2D method that includes a 2D stellar structure model, which takes rotation into account. We then place these differences between 1D and 2D methods in the context of asteroseismic measurements of internal magnetic fields. We only focus on the asymmetries and not on possible additional frequency peaks that can arise when the magnetic and rotation axis are misaligned. Methods. We coupled the 1D pulsation codes GYRE and StORM to the 2D stellar structure code ESTER and compared the oscillation predictions with the results from the 2D TOP pulsation code. We focused on zero-age main-sequence models representative of rotating β Cephei pulsators spinning at up to 20 per cent of the critical Keplerian rotation rate. Specifically, we investigated low-radial-order gravity and pressure modes. Results. We find a generally good agreement between the oscillation frequencies resulting from the 1D and 2D pulsation codes. We report differences in predicted mode multiplet asymmetries of mostly below 0.06 d−1. Since the magnetic asymmetries are small compared to the differences in the rotational asymmetries resulting from the 1D and 2D predictions, accurate measurements of the magnetic field are in most cases challenging. Conclusions. Differences in the predicted mode asymmetries of a rotating star between 1D perturbative methods and 2D non-perturbative methods can greatly hinder accurate measurements of internal magnetic fields in main-sequence pulsators with low-order modes. Nevertheless, reasonably accurate measurements could be possible with npg ≥ 2 modes if the internal rotation is roughly below 10 per cent of the Keplerian critical rotation frequency for (aligned) magnetic fields of the order of a few hundred kilogauss. While the differences between the 1D and 2D frequency predictions are mostly too large for internal magnetic field detections, the rotational asymmetries predicted by StORM are in general accurate enough for asteroseismic modelling of the stellar rotation in main-sequence stars with identified low-order modes.}, author = {Mombarg, J. S.G. and Vanlaer, V. and Das, Srijan B and Rieutord, M. and Aerts, C. and Bugnet, Lisa Annabelle and Mathis, S. and Reese, D. R. and Ballot, J.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields}}, doi = {10.1051/0004-6361/202557247}, volume = {704}, year = {2025}, } @misc{20936, abstract = {Supplementary material for Mombarg et al. (2025, A&A). Title: "Is a 1D perturbative method sufficient for asteroseismic modelling of ~Cephei pulsators? Implications for measurements of rotation and internal magnetic fields" Content: - 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. - 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) - 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 = {Mombarg, Joey and Vanlaer, Vincent and Das, Srijan B and Rieutord, Michel and Aerts, Conny and Bugnet, Lisa Annabelle and Mathis, Stephane and Reese, Daniel and Ballot, Jerome}, publisher = {Zenodo}, title = {{Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?}}, doi = {10.5281/ZENODO.17580178}, year = {2025}, } @article{21252, abstract = {Context. Recent observational results from asteroseismic studies show that an important fraction of solar-like stars do not present detectable stochastically excited acoustic oscillations. This non-detectability seems to correlate with a high rotation rate in the convective envelope and a high surface magnetic activity. At the same time, the properties of stellar convection are affected by rotation and magnetism. Aims. We investigate the role of rotation in the excitation of acoustic modes in the convective envelope of solar-like stars, to evaluate its impact on the energy injected in the oscillations. Methods. We derived theoretical prescriptions for the excitation of acoustic waves in the convective envelope of rotating solar-like stars. We adopted the rotating mixing-length Theory to model the influence of rotation on convection. We used the MESA stellar evolution code and the GYRE stellar oscillation code to estimate the power injected in the oscillations from our theoretical prescriptions. Results. We demonstrate that the power injected in the acoustic modes is insensitive to rotation if a Gaussian time-correlation function is assumed, while it can decrease by up to 60% for a Lorentzian time-correlation function, for a 20 Ω⊙ rotation rate. We show that the modification of the excitation rate by rotation depends not only on the rotation rate but also on the radial and angular orders of the considered oscillation mode. This result can allow for better constraints on the properties of stellar convection by studying observationally acoustic mode excitation. Conclusions. These results demonstrate how important it is to take into account the modification of stellar convection by rotation when evaluating the amplitude of the stellar oscillations it stochastically excites. They open the path for understanding the large variety of observed acoustic-mode amplitudes at the surface of solar-like stars as a function of surface rotation rates.}, author = {Bessila, L. and Deckx van Ruys, A. and Buriasco, V. and Mathis, S. and Bugnet, Lisa Annabelle and García, R. A. and Mathur, S.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators}}, doi = {10.1051/0004-6361/202452093}, volume = {700}, year = {2025}, } @article{19637, abstract = {PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2R Earth) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.}, author = {Rauer, Heike and Aerts, Conny and Cabrera, Juan and Deleuil, Magali and Erikson, Anders and Gizon, Laurent and Goupil, Mariejo and Heras, Ana and Walloschek, Thomas and Lorenzo-Alvarez, Jose and Marliani, Filippo and Martin-Garcia, César and Mas-Hesse, J. Miguel and O’Rourke, Laurence and Osborn, Hugh and Pagano, Isabella and Piotto, Giampaolo and Pollacco, Don and Ragazzoni, Roberto and Ramsay, Gavin and Udry, Stéphane and Appourchaux, Thierry and Benz, Willy and Brandeker, Alexis and Güdel, Manuel and Janot-Pacheco, Eduardo and Kabath, Petr and Kjeldsen, Hans and Min, Michiel and Santos, Nuno and Smith, Alan and Suarez, Juan Carlos and Werner, Stephanie C. and Aboudan, Alessio and Abreu, Manuel and Acuña, Lorena and Adams, Moritz and Adibekyan, Vardan and Affer, Laura and Agneray, François and Agnor, Craig and Aguirre Børsen-Koch, Victor and Ahmed, Saad and Aigrain, Suzanne and Al-Bahlawan, Ashraf and Alcacera Gil, Ma De Los Angeles and Alei, Eleonora and Alencar, Silvia and Alexander, Richard and Alfonso-Garzón, Julia and Alibert, Yann and Allende Prieto, Carlos and Almeida, Leonardo and Alonso Sobrino, Roi and Altavilla, Giuseppe and Althaus, Christian and Alvarez Trujillo, Luis Alonso and Amarsi, Anish and Ammler-Von Eiff, Matthias and Amôres, Eduardo and Andrade, Laerte and Antoniadis-Karnavas, Alexandros and António, Carlos and Aparicio Del Moral, Beatriz and Appolloni, Matteo and Arena, Claudio and Armstrong, David and Aroca Aliaga, Jose and Asplund, Martin and Audenaert, Jeroen and Auricchio, Natalia and Avelino, Pedro and Baeke, Ann and Baillié, Kevin and Balado, Ana and Ballber Balagueró, Pau and Balestra, Andrea and Ball, Warrick and Ballans, Herve and Ballot, Jerome and Barban, Caroline and Barbary, Gaële and Barbieri, Mauro and Barceló Forteza, Sebastià and Barker, Adrian and Barklem, Paul and Barnes, Sydney and Barrado Navascues, David and Barragan, Oscar and Baruteau, Clément and Basu, Sarbani and Baudin, Frederic and Baumeister, Philipp and Bayliss, Daniel and Bazot, Michael and Beck, Paul G. and Belkacem, Kevin and Bellinger, Earl and Benatti, Serena and Benomar, Othman and Bérard, Diane and Bergemann, Maria and Bergomi, Maria and Bernardo, Pierre and Biazzo, Katia and Bignamini, Andrea and Bigot, Lionel and Billot, Nicolas and Binet, Martin and Biondi, David and Biondi, Federico and Birch, Aaron C. and Bitsch, Bertram and Bluhm Ceballos, Paz Victoria and Bódi, Attila and Bognár, Zsófia and Boisse, Isabelle and Bolmont, Emeline and Bonanno, Alfio and Bonavita, Mariangela and Bonfanti, Andrea and Bonfils, Xavier and Bonito, Rosaria and Bonomo, Aldo Stefano and Börner, Anko and Boro Saikia, Sudeshna and Borreguero Martín, Elisa and Borsa, Francesco and Borsato, Luca and Bossini, Diego and Bouchy, Francois and Boué, Gwenaël and Boufleur, Rodrigo and Boumier, Patrick and Bourrier, Vincent and Bowman, Dominic M. and Bozzo, Enrico and Bradley, Louisa and Bray, John and Bressan, Alessandro and Breton, Sylvain and Brienza, Daniele and Brito, Ana and Brogi, Matteo and Brown, Beverly and Brown, David J.A. and Brun, Allan Sacha and Bruno, Giovanni and Bruns, Michael and Buchhave, Lars A. and Bugnet, Lisa Annabelle and Buldgen, Gaël and Burgess, Patrick and Busatta, Andrea and Busso, Giorgia and Buzasi, Derek and Caballero, José A. and Cabral, Alexandre and Cabrero Gomez, Juan Francisco and Calderone, Flavia and Cameron, Robert and Cameron, Andrew and Campante, Tiago and Campos Gestal, Néstor and Canto Martins, Bruno Leonardo and Cara, Christophe and Carone, Ludmila and Carrasco, Josep Manel and Casagrande, Luca and Casewell, Sarah L. and Cassisi, Santi and Castellani, Marco and Castro, Matthieu and Catala, Claude and Catalán Fernández, Irene and Catelan, Márcio and Cegla, Heather and Cerruti, Chiara and Cessa, Virginie and Chadid, Merieme and Chaplin, William and Charpinet, Stephane and Chiappini, Cristina and Chiarucci, Simone and Chiavassa, Andrea and Chinellato, Simonetta and Chirulli, Giovanni and Christensen-Dalsgaard, Jørgen and Church, Ross and Claret, Antonio and Clarke, Cathie and Claudi, Riccardo and Clermont, Lionel and Coelho, Hugo and Coelho, Joao and Cogato, Fabrizio and Colomé, Josep and Condamin, Mathieu and Conde García, Fernando and Conseil, Simon and Corbard, Thierry and Correia, Alexandre C.M. and Corsaro, Enrico and Cosentino, Rosario and Costes, Jean and Cottinelli, Andrea and Covone, Giovanni and Creevey, Orlagh L. and Crida, Aurelien and Csizmadia, Szilard and Cunha, Margarida and Curry, Patrick and Da Costa, Jefferson and Da Silva, Francys and Dalal, Shweta and Damasso, Mario and Damiani, Cilia and Damiani, Francesco and Das Chagas, Maria Liduina and Davies, Melvyn and Davies, Guy and Davies, Ben and Davison, Gary and De Almeida, Leandro and De Angeli, Francesca and De Barros, Susana Cristina Cabral and De Castroleão, Izan and De Freitas, Daniel Brito and De Freitas, Marcia Cristina and De Martino, Domitilla and De Medeiros, José Renan and De Paula, Luiz Alberto and De Pedraza Gómez, Álvaro and De Plaa, Jelle and De Ridder, Joris and Deal, Morgan and Decin, Leen and Deeg, Hans and Degl’Innocenti, Scilla and Deheuvels, Sebastien and Del Burgo, Carlos and Del Sordo, Fabio and Delgado-Mena, Elisa and Demangeon, Olivier and Denk, Tilmann and Derekas, Aliz and Desert, Jean Michel and Desidera, Silvano and Dexet, Marc and Di Criscienzo, Marcella and Di Giorgio, Anna Maria and Di Mauro, Maria Pia and Diaz Rial, Federico Jose and Díaz-García, José Javier and Dima, Marco and Dinuzzi, Giacomo and Dionatos, Odysseas and Distefano, Elisa and Do Nascimento, Jose Dias and Domingo, Albert and D’Orazi, Valentina and Dorn, Caroline and Doyle, Lauren and Duarte, Elena and Ducellier, Florent and Dumaye, Luc and Dumusque, Xavier and Dupret, Marc Antoine and Eggenberger, Patrick and Ehrenreich, David and Eigmüller, Philipp and Eising, Johannes and Emilio, Marcelo and Eriksson, Kjell and Ermocida, Marco and Escate Giribaldi, Riano Isidoro and Eschen, Yoshi and Espinosa Yáñez, Lucía and Estrela, Inês and Evans, Dafydd Wyn and Fabbian, Damian and Fabrizio, Michele and Faria, João Pedro and Farina, Maria and Farinato, Jacopo and Feliz, Dax and Feltzing, Sofia and Fenouillet, Thomas and Fernández, Miguel and Ferrari, Lorenza and Ferraz-Mello, Sylvio and Fialho, Fabio and Fienga, Agnes and Figueira, Pedro and Fiori, Laura and Flaccomio, Ettore and Focardi, Mauro and Foley, Steve and Fontignie, Jean and Ford, Dominic and Fornazier, Karin and Forveille, Thierry and Fossati, Luca and Franca, Rodrigo De Marca and Franco Da Silva, Lucas and Frasca, Antonio and Fridlund, Malcolm and Furlan, Marco and Gabler, Sarah Maria and Gaido, Marco and Gallagher, Andrew and Gallego Sempere, Paloma I. and Galli, Emanuele and García, Rafael A. and García Hernández, Antonio and Garcia Munoz, Antonio and García-Vázquez, Hugo and Garrido Haba, Rafael and Gaulme, Patrick and Gauthier, Nicolas and Gehan, Charlotte and Gent, Matthew and Georgieva, Iskra and Ghigo, Mauro and Giana, Edoardo and Gill, Samuel and Girardi, Leo and Giuliatti Winter, Silvia and Giusi, Giovanni and Gomes Da Silva, João and Gómez Zazo, Luis Jorge and Gomez-Lopez, Juan Manuel and González Hernández, Jonay Isai and Gonzalez Murillo, Kevin and Gonzalo Melchor, Alejandro and Gorius, Nicolas and Gouel, Pierre Vincent and Goulty, Duncan and Granata, Valentina and Grenfell, John Lee and Grießbach, Denis and Grolleau, Emmanuel and Grouffal, Salomé and Grziwa, Sascha and Guarcello, Mario Giuseppe and Gueguen, Loïc and Guenther, Eike Wolf and Guilhem, Terrasa and Guillerot, Lucas and Guillot, Tristan and Guiot, Pierre and Guterman, Pascal and Gutiérrez, Antonio and Gutiérrez-Canales, Fernando and Hagelberg, Janis and Haldemann, Jonas and Hall, Cassandra and Handberg, Rasmus and Harrison, Ian and Harrison, Diana L. and Hasiba, Johann and Haswell, Carole A. and Hatalova, Petra and Hatzes, Artie and Haywood, Raphaelle and Hébrard, Guillaume and Heckes, Frank and Heiter, Ulrike and Hekker, Saskia and Heller, René and Helling, Christiane and Helminiak, Krzysztof and Hemsley, Simon and Heng, Kevin and Herbst, Konstantin and Hermans, Aline and Hermes, J. J. and Hidalgo Torres, Nadia and Hinkel, Natalie and Hobbs, David and Hodgkin, Simon and Hofmann, Karl and Hojjatpanah, Saeed and Houdek, Günter and Huber, Daniel and Huesler, Joseph and Hui-Bon-Hoa, Alain and Huygen, Rik and Huynh, Duc Dat and Iro, Nicolas and Irwin, Jonathan and Irwin, Mike and Izidoro, André and Jacquinod, Sophie and Jannsen, Nicholas Emborg and Janson, Markus and Jeszenszky, Harald and Jiang, Chen and Jimenez Mancebo, Antonio José and Jofre, Paula and Johansen, Anders and Johnston, Cole and Jones, Geraint and Kallinger, Thomas and Kálmán, Szilárd and Kanitz, Thomas and Karjalainen, Marie and Karjalainen, Raine and Karoff, Christoffer and Kawaler, Steven and Kawata, Daisuke and Keereman, Arnoud and Keiderling, David and Kennedy, Tom and Kenworthy, Matthew and Kerschbaum, Franz and Kidger, Mark and Kiefer, Flavien and Kintziger, Christian and Kislyakova, Kristina and Kiss, László and Klagyivik, Peter and Klahr, Hubert and Klevas, Jonas and Kochukhov, Oleg and Köhler, Ulrich and Kolb, Ulrich and Koncz, Alexander and Korth, Judith and Kostogryz, Nadiia and Kovács, Gábor and Kovács, József and Kozhura, Oleg and Krivova, Natalie and Kuĉinskas, Arūnas and Kuhlemann, Ilyas and Kupka, Friedrich and Laauwen, Wouter and Labiano, Alvaro and Lagarde, Nadege and Laget, Philippe and Laky, Gunter and Lam, Kristine Wai Fun and Lambrechts, Michiel and Lammer, Helmut and Lanza, Antonino Francesco and Lanzafame, Alessandro and Lares Martiz, Mariel and Laskar, Jacques and Latter, Henrik and Lavanant, Tony and Lawrenson, Alastair and Lazzoni, Cecilia and Lebre, Agnes and Lebreton, Yveline and Lecavelier Des Etangs, Alain and Lee, Katherine and Leinhardt, Zoe and Leleu, Adrien and Lendl, Monika and Leto, Giuseppe and Levillain, Yves and Libert, Anne Sophie and Lichtenberg, Tim and Ligi, Roxanne and Lignieres, Francois and Lillo-Box, Jorge and Linsky, Jeffrey and Liu, John Scige and Loidolt, Dominik and Longval, Yuying and Lopes, Ilídio and Lorenzani, Andrea and Ludwig, Hans Guenter and Lund, Mikkel and Lundkvist, Mia Sloth and Luri, Xavier and Maceroni, Carla and Madden, Sean and Madhusudhan, Nikku and Maggio, Antonio and Magliano, Christian and Magrin, Demetrio and Mahy, Laurent and Maibaum, Olaf and Malac-Allain, Lee Roy and Malapert, Jean Christophe and Malavolta, Luca and Maldonado, Jesus and Mamonova, Elena and Manchon, Louis and Manjón, Andres and Mann, Andrew and Mantovan, Giacomo and Marafatto, Luca and Marconi, Marcella and Mardling, Rosemary and Marigo, Paola and Marinoni, Silvia and Marques, Rico and Marques, Joao Pedro and Marrese, Paola Maria and Marshall, Douglas and Martínez Perales, Silvia and Mary, David and Marzari, Francesco and Masana, Eduard and Mascher, Andrina and Mathis, Stéphane and Mathur, Savita and Martín Vodopivec, Iris and Mattiuci Figueiredo, Ana Carolina and Maxted, Pierre F.L. and Mazeh, Tsevi and Mazevet, Stephane and Mazzei, Francesco and Mccormac, James and Mcmillan, Paul and Menou, Lucas and Merle, Thibault and Meru, Farzana and Mesa, Dino and Messina, Sergio and Mészáros, Szabolcs and Meunier, Nadége and Meunier, Jean Charles and Micela, Giuseppina and Michaelis, Harald and Michel, Eric and Michielsen, Mathias and Michtchenko, Tatiana and Miglio, Andrea and Miguel, Yamila and Milligan, David and Mirouh, Giovanni and Mitchell, Morgan and Moedas, Nuno and Molendini, Francesca and Molnár, László and Mombarg, Joey and Montalban, Josefina and Montalto, Marco and Monteiro, Mário J.P.F.G. and Montoro Sánchez, Francisco and Morales, Juan Carlos and Morales-Calderon, Maria and Morbidelli, Alessandro and Mordasini, Christoph and Moreau, Chrystel and Morel, Thierry and Morello, Giuseppe and Morin, Julien and Mortier, Annelies and Mosser, Benoît and Mourard, Denis and Mousis, Olivier and Moutou, Claire and Mowlavi, Nami and Moya, Andrés and Muehlmann, Prisca and Muirhead, Philip and Munari, Matteo and Musella, Ilaria and Mustill, Alexander James and Nardetto, Nicolas and Nardiello, Domenico and Narita, Norio and Nascimbeni, Valerio and Nash, Anna and Neiner, Coralie and Nelson, Richard P. and Nettelmann, Nadine and Nicolini, Gianalfredo and Nielsen, Martin and Niemi, Sami Matias and Noack, Lena and Noels-Grotsch, Arlette and Noll, Anthony and Norazman, Azib and Norton, Andrew J. and Nsamba, Benard and Ofir, Aviv and Ogilvie, Gordon and Olander, Terese and Olivetto, Christian and Olofsson, Göran and Ong, Joel and Ortolani, Sergio and Oshagh, Mahmoudreza and Ottacher, Harald and Ottensamer, Roland and Ouazzani, Rhita Maria and Paardekooper, Sijme Jan and Pace, Emanuele and Pajas, Miriam and Palacios, Ana and Palandri, Gaelle and Palle, Enric and Paproth, Carsten and Parro, Vanderlei and Parviainen, Hannu and Pascual Granado, Javier and Passegger, Vera Maria and Pastor-Morales, Carmen and Pätzold, Martin and Pedersen, May Gade and Pena Hidalgo, David and Pepe, Francesco and Pereira, Filipe and Persson, Carina M. and Pertenais, Martin and Peter, Gisbert and Petit, Antoine C. and Petit, Pascal and Pezzuto, Stefania and Pichierri, Gabriele and Pietrinferni, Adriano and Pinheiro, Fernando and Pinsonneault, Marc and Plachy, Emese and Plasson, Philippe and Plez, Bertrand and Poppenhaeger, Katja and Poretti, Ennio and Portaluri, Elisa and Portell, Jordi and Porto De Mello, Gustavo Frederico and Poyatos, Julien and Pozuelos, Francisco J. and Prada Moroni, Pier Giorgio and Pricopi, Dumitru and Prisinzano, Loredana and Quade, Matthias and Quirrenbach, Andreas and Rabanal Reina, Julio Arturo and Rabello Soares, Maria Cristina and Raimondo, Gabriella and Rainer, Monica and Ramón Rodón, Jose and Ramón-Ballesta, Alejandro and Ramos Zapata, Gonzalo and Rätz, Stefanie and Rauterberg, Christoph and Redman, Bob and Redmer, Ronald and Reese, Daniel and Regibo, Sara and Reiners, Ansgar and Reinhold, Timo and Renie, Christian and Ribas, Ignasi and Ribeiro, Sergio and Ricciardi, Thiago Pereira and Rice, Ken and Richard, Olivier and Riello, Marco and Rieutord, Michel and Ripepi, Vincenzo and Rixon, Guy and Rockstein, Steve and Rodón Ortiz, José Ramón and Rodrigo Rodríguez, María Teresa and Rodríguez Amor, Alberto and Rodríguez Díaz, Luisa Fernanda and Rodriguez Garcia, Juan Pablo and Rodriguez-Gomez, Julio and Roehlly, Yannick and Roig, Fernando and Rojas-Ayala, Bárbara and Rolf, Tobias and Rørsted, Jakob Lysgaard and Rosado, Hugo and Rosotti, Giovanni and Roth, Olivier and Roth, Markus and Rousseau, Alex and Roxburgh, Ian and Roy, Fabrice and Royer, Pierre and Ruane, Kirk and Rufini Mastropasqua, Sergio and Ruiz De Galarreta, Claudia and Russi, Andrea and Saar, Steven and Saillenfest, Melaine and Salaris, Maurizio and Salmon, Sebastien and Saltas, Ippocratis and Samadi, Réza and Samadi, Aunia and Samra, Dominic and Sanches Da Silva, Tiago and Sánchez Carrasco, Miguel Andrés and Santerne, Alexandre and Santiago Pé, Amaia and Santoli, Francesco and Santos, Ängela R.G. and Sanz Mesa, Rosario and Sarro, Luis Manuel and Scandariato, Gaetano and Schäfer, Martin and Schlafly, Edward and Schmider, François Xavier and Schneider, Jean and Schou, Jesper and Schunker, Hannah and Schwarzkopf, Gabriel Jörg and Serenelli, Aldo and Seynaeve, Dries and Shan, Yutong and Shapiro, Alexander and Shipman, Russel and Sicilia, Daniela and Sierra Sanmartin, Maria Angeles and Sigot, Axelle and Silliman, Kyle and Silvotti, Roberto and Simon, Attila E. and Simoyama Napoli, Ricardo and Skarka, Marek and Smalley, Barry and Smiljanic, Rodolfo and Smit, Samuel and Smith, Alexis and Smith, Leigh and Snellen, Ignas and Sódor, Ádám and Sohl, Frank and Solanki, Sami K. and Sortino, Francesca and Sousa, Sérgio and Southworth, John and Souto, Diogo and Sozzetti, Alessandro and Stamatellos, Dimitris and Stassun, Keivan and Steller, Manfred and Stello, Dennis and Stelzer, Beate and Stiebeler, Ulrike and Stokholm, Amalie and Storelvmo, Trude and Strassmeier, Klaus and Strøm, Paul Anthony and Strugarek, Antoine and Sulis, Sophia and Švanda, Michal and Szabados, László and Szabó, Róbert and Szabó, Gyula M. and Szuszkiewicz, Ewa and Talens, Geert Jan and Teti, Daniele and Theisen, Tom and Thévenin, Frédéric and Thoul, Anne and Tiphene, Didier and Titz-Weider, Ruth and Tkachenko, Andrew and Tomecki, Daniel and Tonfat, Jorge and Tosi, Nicola and Trampedach, Regner and Traven, Gregor and Triaud, Amaury and Trønnes, Reidar and Tsantaki, Maria and Tschentscher, Matthias and Turin, Arnaud and Tvaruzka, Adam and Ulmer, Bernd and Ulmer-Moll, Solène and Ulusoy, Ceren and Umbriaco, Gabriele and Valencia, Diana and Valentini, Marica and Valio, Adriana and Valverde Guijarro, Ángel Luis and Van Eylen, Vincent and Van Grootel, Valerie and Van Kempen, Tim A. and Van Reeth, Timothy and Van Zelst, Iris and Vandenbussche, Bart and Vasiliou, Konstantinos and Vasilyev, Valeriy and Vaz De Mascarenhas, David and Vazan, Allona and Vela Nunez, Marina and Velloso, Eduardo Nunes and Ventura, Rita and Ventura, Paolo and Venturini, Julia and Vera Trallero, Isabel and Veras, Dimitri and Verdugo, Eva and Verma, Kuldeep and Vibert, Didier and Vicanek Martinez, Tobias and Vida, Krisztián and Vigan, Arthur and Villacorta, Antonio and Villaver, Eva and Villaverde Aparicio, Marcos and Viotto, Valentina and Vorobyov, Eduard and Vorontsov, Sergey and Wagner, Frank W. and Walton, Nicholas and Walton, Dave and Wang, Haiyang and Waters, Rens and Watson, Christopher and Wedemeyer, Sven and Weeks, Angharad and Weingrill, Jörg and Weiss, Annita and Wendler, Belinda and West, Richard and Westerdorff, Karsten and Westphal, Pierre Amaury and Wheatley, Peter and White, Tim and Whittaker, Amadou and Wickhusen, Kai and Wilson, Thomas and Windsor, James and Winter, Othon and Winther, Mark Lykke and Winton, Alistair and Witteck, Ulrike and Witzke, Veronika and Woitke, Peter and Wolter, David and Wuchterl, Günther and Wyatt, Mark and Yang, Dan and Yu, Jie and Zanmar Sanchez, Ricardo and Zapatero Osorio, María Rosa and Zechmeister, Mathias and Zhou, Yixiao and Ziemke, Claas and Zwintz, Konstanze and Böhm, Torsten and Dansac, Léo Michel}, issn = {1572-9508}, journal = {Experimental Astronomy}, number = {3}, publisher = {Springer Nature}, title = {{The PLATO mission}}, doi = {10.1007/s10686-025-09985-9}, volume = {59}, year = {2025}, } @unpublished{21309, abstract = {The polarization of light is a critically under-utilized, rich source of information in astronomy. For stars in particular, surface magnetism polarization that can be detected and measured with spectro-polarimetry. Many questions about these surface fields remain unanswered due to a lack of dedicated instruments capable of probing weak and strong surface magnetic fields for the entire mass range of stars, from M-dwarfs (and even substellar objects) to massive O-type stars at different evolutionary stages and metallicities. These questions range from the origin of these fields to their true incidence rate throughout the stellar population and the dependence on metallicity. Magnetic fields, although currently often excluded from stellar evolution models, play an important role in stellar evolution. Connecting the surface fields to internal fields through asteroseismology will instigate a new era of understanding stellar evolution and the transport of angular momentum and chemical elements throughout stellar interiors, also impacting our understanding of star-planet interactions and stellar remnants. Polarimetry is also an under-utilized tool to observationally constrain the mode identification of nonradial oscillations, which lies at the basis of accurate asteroseismic parameter estimation at percentage-level for stellar radii, masses, ages, internal rotation, and magnetic field strengths. Combining strong constraints on mode identification and surface magnetic properties through the acquisition of time-resolved, high-resolution and high-signal-to-noise (S/N) spectro-polarimetry and spectroscopy promises to bring leaps forward in our understanding of stellar structure, particularly when combined with long-term space photometric data from past, current, and future missions.}, author = {Vandersnickt, J. and Armenta, R. Ochoa and Vanlaer, V. and A. David-Uraz, A. David-Uraz and Aerts, C. and Das, S. B. and Bouret, J. -C. and Bowman, D. M. and Bugnet, Lisa Annabelle and Khalack, V. and J. Labadie-Bartz, J. Labadie-Bartz and Mathis, S. and Nazé, Y. and Neiner, C. and Petit, P. and Petit, V. and K. Thomson-Paressant, K. Thomson-Paressant and Doorsselaere, T. Van and Vanrespaille, M.}, booktitle = {arXiv}, title = {{Expanding stellar horizons with polarized light}}, doi = {10.48550/arXiv.2512.15170}, year = {2025}, } @phdthesis{19853, abstract = {The internal dynamical properties of red giant stars have been explored extensively in recent years as a result of the increase in high precision data availability from the space missions Kepler and TESS (Transiting Exoplanet Survey Satellite), and in this exploration, it has been discovered that some of these stars are not behaving as expected. Red giants are stars that have evolved off of the main sequence after having completed fusing hydrogen into helium in their core. Observational data shows that the cores are rotating significantly slower than models can recreate consistently across evolutionary stages. This discrepancy has prompted investigation into the efficiency of angular momentum transport mechanisms and mixing processes including meridional circulation, shear instability, internal gravity waves, Tayler-Spruit dynamo, fossil magnetic fields etc., to explain this behavior. Analyzing seismic oscillations in stars, via asteroseismology, is a powerful tool as it is the only way in which the deep stellar interior can be probed and subsequently characterized; this is possible as global oscillations modulating the stellar surface are effected by internal processes. For red giants, p-modes (pressure modes; resonating through the entire star) and g-modes (gravity-modes; resonating in the radiative interior) couple to create mixed modes. These mixed modes give access to the otherwise hidden stellar interior as g-modes couple to p-modes, delivering information from the interior to the surface. Internal magnetic signatures have been observationally confirmed in red giant stars via asteroseismology and characterized in two ways. One being that dipole mixed modes with ℓ = 1 will display a global asymmetric frequency shift of its azimuthal components; where the m = 0 and m = ±1 components of the ℓ = 1 dipole mode will be shifted by two different power laws, respectively. And the other being a reduced visibility of dipole mixed mode amplitudes in the power spectra, where stars presenting with this feature are denoted as suppressed. Several studies of the suppressed dipole mixed mode amplitudes have been carried out, but thus far, no dedicated studies of the asymmetric frequency shifts of suppressed red giants have been conducted; one reason being that the asymmetric frequency shifts cannot be characterized when the dipole mixed mode amplitudes are severely reduced in many of the suppressed stars. Sincefullysuppressedstarsdonothavedetectablemixed-modestoevaluate, partiallysuppressed stars, that is, red giant stars presenting with suppressed dipole mixed modes in select parts of their power spectra rather than across the entire spectra, will be the subject of this study as the respective mode amplitudes are still visible at high frequencies. As such, this study will search for asymmetric frequency shifts on the dipole mixed modes of partially suppressed red giant stars; the aim here is to investigate if both mode suppression and magnetic shifting of dipole mixed modes occur simultaneously. Thisstudywillbeconductedbycreatingapipelinetoestimatepriorsofasteroseismicparameters, use the priors to model the power spectra with the stellar modeling code sloscillations_ISTA, and perform a Bayesian fit of the parameters with the simulated data on the star KIC 6975038, a target with partially suppressed dipolar mode amplitudes identified in the literature, to fit its magnetic parameters. I present a novel method to model the stellar power spectra of partially suppressed red giants by application of a sigmoid profile to the ℓ= 1 dipolar mode component of the spectra. With the results of this study I aim at constraining the cause of this partial dipole mode amplitude suppression, allowing for more detailed studies regarding their astrophysical nature. Furthermore, the long term hope for the method used in this study will be to expand the sample of partially suppressed red giants and fit their asteroseismic parameters accordingly.}, author = {Smith, Kanah}, issn = {2791-4585}, keywords = {asteroseismology, stellar physics, red giant, magnetism, suppressed}, pages = {38}, publisher = {Institute of Science and Technology Austria}, title = {{Exploring internal magnetism in partially suppressed red giant stars}}, doi = {10.15479/AT-ISTA-19853}, year = {2025}, } @article{18172, abstract = {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.}, author = {Hatt, Emily J. and Ong, J. M.Joel and Nielsen, Martin B. and Chaplin, William J. and Davies, Guy R. and Deheuvels, Sébastien and Ballot, Jérôme and Li, Gang and Bugnet, Lisa Annabelle}, issn = {1365-2966}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {2}, pages = {1060--1076}, publisher = {Oxford University Press}, title = {{Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants}}, doi = {10.1093/mnras/stae2053}, volume = {534}, year = {2024}, } @article{18306, abstract = {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 = {Oza, Apurva V. and Seidel, Julia V. and Hoeijmakers, H. Jens and Unni, Athira and Kesseli, Aurora Y. and Schmidt, Carl A. and Sivarani, Thirupathi and Bello-Arufe, Aaron and Gebek, Andrea and Meyer Zu Westram, Moritz and Sousa, Sérgio G. and Lopes, Rosaly M.C. and Hu, Renyu and De Kleer, Katherine and Fisher, Chloe and Charnoz, Sébastien and Baker, Ashley D. and Halverson, Samuel P. and Schneider, Nick M. and Psaridi, Angelica and Wyttenbach, Aurélien and Torres Rodriguez, Santiago and Bhatnagar, Ishita and Johnson, Robert E.}, issn = {2041-8213}, journal = {Astrophysical Journal Letters}, number = {2}, publisher = {IOP Publishing}, title = {{Redshifted sodium transient near exoplanet transit}}, doi = {10.3847/2041-8213/ad6b29}, volume = {973}, year = {2024}, } @article{18528, abstract = {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.}, author = {Das, Srijan B and Einramhof, Lukas and Bugnet, Lisa Annabelle}, issn = {1432-0746}, journal = {Astronomy and Astrophysics}, publisher = {EDP Sciences}, title = {{Unveiling complex magnetic field configurations in red giant stars}}, doi = {10.1051/0004-6361/202450918}, volume = {690}, year = {2024}, } @article{18904, abstract = {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.}, author = {Breton, S. N. and Lanza, A. F. and Messina, S. and Pagano, I. and Bugnet, Lisa Annabelle and Corsaro, E. and García, R. A. and Mathur, S. and Santos, A. R. G. and Aigrain, S. and Amard, L. and Brun, A. S. and Degott, L. and Noraz, Q. and Palakkatharappil, D. B. and Panetier, E. and Strugarek, A. and Belkacem, K. and Goupil, M.-J and Ouazzani, R. M. and Philidet, J. and Renié, C. and Roth, O.}, issn = {1432-0746}, journal = {Astronomy and Astrophysics}, publisher = {EDP Sciences}, title = {{Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves}}, doi = {10.1051/0004-6361/202449893}, volume = {689}, year = {2024}, }