reapxdev/zenodo-scraper huggingface dataset:
The potential of SPATO: Survey of PLATO A-Type stars Oscillation frequencies
Authors: Camino Mesa, Carlos Casimiro, García Hernández, Antonio, Suárez, Juan Carlos, Mirouh, Giovanni, Florido Tomé, Alejandro José, Godoy-Rivera, Diego
Type: Presentation
Published: 2026-07-13

<p>Pulsating A-F type stars on the main sequence occupy the region where the classical instability strip intersects the main sequence, a regime in which different excitation mechanisms coexist and overlap in the HR diagram. This degeneracy hinders a clear observational classification and calls for large, homogeneous statistical studies.</p>
<p>To address this, we present SPATO, a new catalogue of oscillation frequencies for A-F type stars in the PLATO LOPS2 field, combining TESS light curves with Gaia DR3 and TIC stellar parameters. SPATO provides a unique dataset in which both stellar parameters and frequency content are consistently derived, including all significant pulsation frequencies down to a well-defined noise level.</p>
<p>Using this catalogue, we find a pulsator fraction of about 60% for $\delta$ Scuti stars, and revisit the classification of $\delta$ Scuti and $\gamma$ Dor variables. The classical 5 c/d boundary does not translate into a clear separation in the HR diagram. Instead, the period-luminosity diagram reveals two dominant populations, with $\delta$ Scuti stars forming a well-defined sequence along the period-luminosity relation and $\gamma$ Dor stars located below it. We propose the low-density region between them as a new purely observational discriminator.</p>
<p>Combining Gaia-based pulsation constants with TESS frequencies, we identify radial modes and show that the fundamental and first overtone define tight, nearly parallel relations. These correlate strongly with stellar radius and surface gravity, enabling $\nu_A$ to act as a proxy for $R$ and $\log g$ with high precision. Higher overtones show larger dispersion, consistent with theoretical expectations and possible misidentification with non-radial modes.</p>
<p>SPATO demonstrates the power of frequency-based catalogues for population studies and provides a reference dataset to identify targets for detailed follow-up and to prepare future analyses with PLATO.</p>
Facing the Phase of asymptotic g-mode frequencies on the red-giant branch
Authors: van Lier, Tobias, Müller, Jonas, Hekker, Saskia
Type: Presentation
Published: 2026-07-13

<p>The pattern of mode frequencies observed in red-giant stars can be well approximated by asymptotic theory. In this limit, the oscillations are characterized by a handful of parameters, which can be obtained from observed oscillation spectra via frequency fitting. In order to interpret the observed parameters in terms of physics, it is essential to understand their sensitivity to the stellar structure.</p>
<p>We study one asymptotic parameter, the g--mode frequency phase, which probes the buoyancy cavity in the stellar core. In the literature, two contributions to this phase are discussed individually: non-asymptotic behavior at the outer cavity boundary, and buoyancy glitches. Using stellar models, we show that it is necessary to account for both these phase terms simultaneously. We further identify glitches in the evanescent region at larger radii as an additional contribution. We demonstrate how correctly interpreted ensemble observations of the g--mode frequency phase on the red-giant branch provide a test for convective-boundary treatment in stellar modeling.</p>
Disentangling the role of nonlinear terms in δ Scuti oscillations
Authors: Rodríguez Sánchez, Miriam, Lares-Martiz, Mariel, Moya Bedón, Andrés, Pascual-Granado, Javier
Type: Presentation
Published: 2026-07-13

<p> Scuti stars exhibit rich, complex power spectra in which numerous radial and nonradial modes are excited.<br>Nonlinear contributions to the oscillations have generally not been taken into account, and most studies<br>have remained within the linear regime due to the complexity involved.<br>However, some approximations to nonlinear codes have been developed, mainly focused on RR Lyrae<br>stars and Cepheids. Complete nonlinear codes have been developed for white dwarfs (Brickhill 1991; Wu<br>2001), but their physics cannot be directly applied to these stars.<br>In this work, we investigate the role of nonlinear contributions by analysing the nonlinear oscillation<br>equations derived from the fundamental hydrodynamic equations expanded to second order in perturbations<br>in terms of the displacement vector. This approach follows the framework presented in Unno et al. (1989)<br>and Aerts et al. (2010), considering no rotation, no magnetic fields, no viscosity, adiabaticity, and no<br>turbulent convection.<br>The expansion introduces numerous cross terms that prevent us from getting a direct numerical solution.<br>To address this problem, we quantify the relative importance of the nonlinear terms. This is done considering<br>the simplest case of radial modes and a snapshot in time at which nonlinear terms have their maximum<br>contribution. We compute the nonlinear terms using a grid of stellar models spanning the δ Scuti instability<br>strip (1.5–2.5M⊙) and the eigenfunctions from the linear adiabatic oscillation equations for radial modes.<br>The results show that nonlinear contributions are more significant in the continuity and energy equations.<br>In the outer convective regions, a point-by-point dominance analysis shows that nonlinear terms can become<br>the largest contribution over a large fraction of the radial grid, reaching maximum dominance fractions<br>between 63% and 83% across the models and modes considered. The first overtone systematically shows<br>larger nonlinear contributions than the fundamental mode. These results suggest that second-order terms<br>may play a role in the external pulsation dynamics of δ Scuti stars and may need to be considered in future<br>nonlinear pulsation codes</p>
A forward-looking perspective on
mission synergies in asteroseismology
Authors: Campante, Tiago L.
Type: Presentation
Published: 2026-07-13

<p class="moz-quote-pre">Over the past 25 years, the number of stars observed with precise space-based time-domain photometry has increased by roughly four orders of magnitude, driven largely by CoRoT, Kepler, and TESS. Remarkably, we are now on the verge of yet another order-of-magnitude leap, with missions such as Roman, PLATO, and Earth 2.0 coming into operation within the next couple of years. In this talk, I will offer a forward-looking perspective on mission synergies in asteroseismology. Rather than attempting a comprehensive review, I will highlight a few examples of overarching opportunities that I find particularly promising, with an emphasis on upcoming missions.</p>
Toward asteroseismic magnetometry for the full diversity of magnetic structures
Authors: Rui, Nicholas, Ong, Joel, Leclerc, Armand, Lecoanet, Daniel, Bugnet, Lisa, Dewberry, Janosz, Liagre, Bastien, Mathis, Stéphane
Type: Presentation
Published: 2026-07-14

<p>Talk given in the "Red giant interiors" splinter session on Thursday, 9 July 2026 at the TASC10/KASC17 Workshop in Aarhus, Denmark. Slides 6, 7, and 11 were presented as animations corresponding to <code>animFig1.mp4</code>, <code>animFig2.mp4</code>, and <code>animFig4.mp4</code> in the Zenodo repository corresponding to the manuscript attached to this work <a href="https://zenodo.org/records/20561425">here</a>.</p>
Asteroseismology in the Rubin/LSST Era
Authors: Das, Susmita
Type: Presentation
Published: 2026-07-14

<p class="p1">The Vera C. Rubin Observatory, named after astronomer Vera Rubin, promises to revolutionize our view</p>
<p class="p1">of the dynamic night sky. Rubin’s 10-year survey, the Legacy Survey of Space and Time (LSST), will</p>
<p class="p1">provide a unique optical time-domain view of the southern sky through repeated multi-band observations</p>
<p class="p1">using the largest digital camera ever built. Although Rubin is not a dedicated asteroseismology mission,</p>
<p class="p1">its combination of depth, sky coverage and long temporal baseline will enable large-scale studies of</p>
<p class="p1">stellar variability across diverse Galactic environments, opening a new era of variability studies across the</p>
<p class="p1">Hertzsprung-Russell diagram.</p>
<p class="p1">In this talk, I will briefly introduce Rubin-LSST and discuss its relevance for the asteroseismology</p>
<p class="p1">community. Rubin’s strengths in probing faint and distant stellar populations will be highlighted, including</p>
<p class="p1">applications to Galactic archaeology, stellar evolution, cluster studies and variability in the Magellanic</p>
<p class="p1">Clouds and nearby dwarf galaxies. I will also discuss the challenges and opportunities of variability</p>
<p class="p1">analyses using Rubin’s sparse and irregular cadence data.</p>
<p class="p1">A major focus will be the complementarity between Rubin and current and future space missions.</p>
<p class="p1">Synergies with TESS and PLATO will help extend variability studies to much larger stellar populations,</p>
<p class="p1">while the Nancy Grace Roman Space Telescope will provide important complementary capabilities in</p>
<p class="p1">crowded and dust-obscured regions. I will briefly discuss Rubin’s role within the broader landscape of</p>
<p class="p1">upcoming stellar astrophysics missions and surveys.</p>
The SYMPHONY of pulsations and binarity in massive star populations
Authors: Thomson-Paressant, Keegan, Bowman, Dominic
Type: Presentation
Published: 2026-07-17

<p>Massive stars play a central role in the cosmic ecosystem through their intense radiation, powerful winds, and dramatic endpoints as supernovae or gamma-ray bursts, all of which strongly influence their surroundings. By producing heavy elements and enriching the interstellar medium, and as progenitors of black holes and neutron stars whose mergers generate gravitational waves, they provide key insight on the Universe and offer unique tests of fundamental physics. However, our ability to predict the outcomes of massive star evolution are currently limited by large uncertainties in stellar evolution models; for example, rotation and mixing, and how these are impacted by binarity and magnetic fields. Fortunately, thanks to modern space telescopes and advanced ground-based observatories, high-precision data sets are now available to constrain these different aspects of physics. Variability in massive stars arises from a combination of physical processes, including binarity, rotational modulation, pulsation, mass loss, and magnetic activity. Asteroseismology of pulsations has significantly advanced our understanding of stellar interiors for massive stars, as they exhibit pressure and gravity modes that constrain different internal layers. Here we present the analysis of a large and homogeneous sample of 873 O- and B-type stars using high-resolution HERMES spectroscopy and 2-minute cadence photometry from TESS, which provide complementary constraints on spectroscopic and photometric variability. Through this joint analysis, we disentangle the contributions of binarity, pulsation, rotation and magnetism. We find that vast majority of the sample exhibit pulsations, and we compare empirical and theoretical instability strips in the Hertzsprung–Russell diagram. We also discover many new eclipsing binaries, which are important laboratories for measuring model-independent masses and radii, and we identify 223 candidate-magnetic stars based on rotational modulation and their 5200-Angstrom flux depression. Our study represents one of the most extensive homogeneous surveys of variability among massive stars in the Northern hemisphere to date. This work establishes a statistical foundation for future asteroseismic modelling efforts and offers new insight into the physical processes governing stellar structure and evolution, particularly from the perspective of improving rotation, magnetism and binarity using pulsations.</p>
Red-Giant Seismology of Population III Stars
Authors: Ferreira dos Santos, Thiago, Bellinger, Earl, Farag, Ebraheem, Lindsay, Christopher
Type: Presentation
Published: 2026-07-20
Keywords: Population III Stars, Asteroseismology, Stellar Pulsations, Stellar Oscillations, Red Giant Stars, Stellar Interiors, Stellar Evolutionary Models

<p><br>Low-mass Population III (Pop III) stars remain undetected despite being potential survivors of the first star-formation epoch, largely because they are difficult to distinguish from later stellar generations. Chemical tagging alone is often ineffective, as internal mixing and external pollution can obscure primordial signatures, thereby motivating diagnostics that probe stellar interiors. Asteroseismology offers then a powerful, yet largely unexplored, avenue to identify primordial stars through the structural imprint of metal-free evolution. Using evolutionary models below 1 MSun, we quantify how convection and associated mixing processes shape internal structure and evolutionary pathways, including self-enrichment episodes. Building on these models, we compute the first non-radial adiabatic pulsation analysis of low-mass Pop III stars. Focusing on a 0.85 MSun red giant as a case study, we show that metal-free models occupy a distinct and observationally separable asteroseismic regime: at similar evolutionary stages, they exhibit systematically altered seismic signatures driven by lower opacities, higher internal sound speeds, steeper core-envelope stratification, and delayed mean-molecular-weight gradient development. We introduce a diagnostic based on the coupling between acoustic and buoyancy cavities and demonstrate that it robustly discriminates Pop III stars from metal-enriched counterparts, even in the presence of surface pollution. These results establish asteroseismology as a viable pathway for identifying surviving Pop III stars in the Milky Way, particularly in the era of large-scale photometric and spectroscopic surveys.</p>
Decoding Massive Stars With MAGIC
Authors: Buzasi, Derek
Type: Presentation
Published: 2026-07-20

<p>Stars constitute the primary building blocks for astronomical systems ranging in scale from exoplanets to galaxies. Massive stars in particular play pivotal roles in the universe, shaping its dynamic evolution and chemical composition as well as serving as progenitors for the compact object mergers which are a current focus for multimessenger astrophysics. Facilities such as Kepler and TESS have revolutionized modern stellar astrophysics by enabling asteroseismology for thousands of stars across the HR diagram, while upcoming missions like Plato promise to extend the asteroseismic golden age into the future. However, the study of oscillations in upper main sequence stars poses some unique problems which current platforms -- all of which are single-color -- are poorly suited to address. Identifying the geometry of individual oscillation modes (mode identification) is the key to successfully interpreting the oscillation frequencies, but the different excitation mechanisms for oscillations in these stars compared to solar-like oscillators means that new tools for mode identification are required. In this talk, I will present a proposed NASA Pioneer-class mission, the Massive Star AsteroseismoloGy Instrument Cubesat (MAGIC), which has the potential to unlock the asteroseismology toolkit for these important astrophysical objects</p>
High Precision Galactic  Chemo-Chronology  from Asteroseismology and Spectroscopy with TESS, K2, and HARPS
Authors: Reyes, Claudia
Type: Presentation
Published: 2026-07-21

<div>We present a high precision chemo-chronological study of Galactic stellar populations using asteroseismology as the primary chronometer. Combining HARPS spectroscopy with TESS asteroseismic constraints, we derive precise stellar ages for a sample of red giant branch stars, with tightly constrained stellar modelling yielding internally consistent age estimates.</div>
<div>We link these ages to homogeneous chemical abundances of Ti, Y, Nd, and Eu, spanning the iron-peak, first s-process peak, mixed s/r, and pure r-process regimes, to establish well-defined age abundance relations across distinct nucleosynthetic channels. This elemental set probes the differing enrichment timescales of core-collapse supernovae, AGB stars, and r-process sites such as neutron star mergers, with Nd providing a diagnostic of the interplay between s- and r-process contributions.</div>
The magnetic field inside the intermediate-mass main-sequence star KIC 9244992 and its relation to the red-giant case
Authors: Takata, Masao, Murphy, Simon, Kurtz, Donald, Saio, Hideyuki, Shibahashi, Hiromoto
Type: Presentation
Published: 2026-07-28

<p>Detection and measurement of stellar internal magnetic fields using asteroseismology has only recently been achieved in red giants. Since then, the study of internal magnetic fields has become one of the hottest research topics in asteroseismology. In this presentation, we firstly report results from the main-sequence star KIC9244992, the first clear example of this type of star. Both p and g modes were detected in this star, and a series of triplets in the rotation-induced frequency splitting of the g modes were particularly clearly observed. All of the triplets originate from dipole modes with different azimuthal orders, but detailed analysis revealed that their frequency distribution slightly deviates from equidistant spacing. This cannot be explained by rotation alone. We therefore constructed a model that takes into account magnetic fields and aspherical buoyancy glitches in addition to rotation, and found that it can successfully explain the observed asymmetry. It is noteworthy that the magnetic field effect must be considered not only in its radial component but also in its azimuthal component. This model imposes the following constraints on the magnetic field strength: The root-mean-square lower bound for the steep chemical gradient layer just outside the convective core is $3.5 \pm 0.1$\,kG in the radial component and $92 \pm 7$\,kG in the azimuthal component. This implies that the azimuthal component is much stronger than the radial component. Furthermore, this presentation will discuss how these magnetic field structures develop as the star evolves into a red giant, and in particular whether they can be detected from the observed oscillation frequencies of red giants.</p>
A Whole New Lab:  Exploring ELNs and Digital Transformation
Authors: Pearman-Kanza, Samantha
Type: Presentation
Published: 2026-07-30
Keywords: elns, FAIR, digital lab, lab of the future

<p>Presentation by Dr Samantha Pearman-Kanza on "A Whole New Lab:  Exploring ELNs and Digital Transformation" for the PSDI & Royce Materials Data Summit 2026. </p>
<p>Abstract: Electronic Lab Notebooks (ELNs) are becoming an increasingly important part of the digital research landscape. They have evolved from basic digital versions of paper notebooks to fully fledged systems that (if implemented properly) can help researchers improve collaboration, reproducibility, and FAIR (Findable, Accessible, Interoperable, and Reusable) data practices. Yet the introduction of any new technology doesn’t guarantee a magical transformation. Successfully introducing ELNs requires more than technology alone; it involves embedding good data practices, supporting cultural change, and carefully integrating tools into everyday research workflows. Drawing on experiences from the University of Southampton on our ELN deployments, FAIR data initiatives, and our wider work on digital laboratories, this talk will explore both the challenges and opportunities of creating more connected research environments. From implementing ELNs in academic settings and supporting FAIR data capture, to emerging developments in smart laboratories, connected systems, automation, and voice-enabled technologies. Join me on a magic carpet ride to explore the potential of the modern digital laboratory</p>
Isochrone-cloud fitting and asteroseismology of the Kepler open cluster NGC 6866
Authors: Wang, Haotian, Aerts, Conny, Fritzewski, Dario, Li, Gang, Van Reeth, Timothy
Type: Presentation
Published: 2026-07-09

<p class="p1">We aim to investigate how isochrones based on different input physics and computed for a variety of initial conditions affect age dating of the open cluster NGC 6866. By using the 4-year-long light curves of its members assembled by the <em>Kepler</em> mission, we further compare these results with asteroseismically derived ages.</p>
<p class="p1">We developed an "isochrone-cloud” fitting method that simultaneously accounts for the range of free parameters occurring in the input physics. Synthetic colour–magnitude diagrams (CMDs) with various initial rotation rates were generated and compared with the observations to determine the <span class="s1">best-fitting rotation distribution. Variable stars were then identified among the cluster members. For the </span>19 gravity-mode (g-mode) pulsators, we performed modelling using a dedicated grid of rotating stellar <span class="s2">models. This modelling was constrained by stellar surface parameters, the measured asymptotic gravity-</span>mode (g-mode) period spacing \Pi_0, and the near-core rotation rate. Two approaches were considered: <span class="s1">modelling the pulsators individually and under the assumption that they share a common age. We found </span>discrepant age estimates from PARSEC and MIST isochrones, which yielded $690^{<span class="s3">+140}_{</span>−30}$ <span class="s1">Myr </span><span class="s4">and $467^{</span>+70}_{−50}$ <span class="s1">Myr</span><span class="s4">,</span>respectively. The isochrone-cloud fitting indicates that NGC 6866 has an initial rotation distribution peaking at <span class="s1">v</span>/<span class="s1">v</span><span class="s3">crit </span>= 0<span class="s5">.</span>6, which is a discrepancy with a factor of about two compared to the asteroseismic values.</p>
<p class="p1">The asteroseismic modelling of the g-mode pulsators revealed agreement between seismic and isochronal masses, whereas the derived ages differ substantially due to the difference in internal mixing. When the g-mode pulsators were modelled under the assumption of one shared cluster age, we obtained a value of $759^{<span class="s3">+54}_{</span>−82}$ <span class="s1">Myr</span><span class="s4">, </span><span class="s1">in agreement with the PARSEC-based isochronal age. We also observe an increased scatter in the rotation </span>and internal mixing parameters under the shared age assumption, which is a possible representation of <span class="s1">the nature of member stars. We conclude that using different input physics and various initial conditions  </span><span class="s4">impacts the age-dating results of open clusters. Our findings point to the need for more carefully calibrated </span><span class="s1">evolutionary models. We also report the existance of a pulsating blue stragger star, which will be valuable </span><span class="s1">for future direct merger seismology analysis.</span></p>
Galactic Archaeology: From cartography to reconstructing the Milky Way's assembly history in detail
Authors: Stokholm, Amalie
Type: Presentation
Published: 2026-07-08

<p>Galactic Archaeology seeks to reconstruct the formation and evolutionary history of the Milky Way by decoding the fossil record preserved in stars. Over the past decade, the field has been transformed by an explosion of data from large-scale spectroscopic, astrometric, photometric, and asteroseismic surveys combined with rapid advances in computational power and numerical simulations. Together, these developments have enabled detailed insight into the assembly history and dynamical evolution of our Galaxy.</p>
<p>In this talk, I will summarise recent advances in mapping the structure and evolution of different parts of our Galaxy, highlighting discoveries that are reshaping our picture of Galactic evolution. I will also discuss the exciting opportunities emerging from upcoming missions and next-generation surveys, and explore how new data and analysis techniques are set to drive the next era of discovery</p>