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<!DOCTYPE HTML>
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<h1><a href="index.html">May Gade Pedersen</a></h1>
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<h3>Internal mixing of rotating stars inferred from dipole gravity modes</h3>
<p><i>Pedersen et al. 2021, Nature Astronomy, Volume 5, p. 715-722</i></p>
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<p><!-- <i>Pedersen et al. 2021, Nature Astronomy, Volume 5, p. 715-722</i> -->
<div style="float:right;width:50%;margin-left:15px;margin-top:10px"><img src="images/Figure2.png" alt="" width="100%";/></div>
During most of their life, stars fuse hydrogen into helium in their cores.
The mixing of chemical elements in the radiative envelope of stars with a convective core is able to replenish the core with extra fuel.
If effective, such deep mixing allows stars to live longer and change their evolutionary path.
Yet localized observations to constrain internal mixing are absent so far.
Gravity modes probe the deep stellar interior near the convective core and allow us to calibrate internal mixing processes.
Here we provide core-to-surface mixing profiles inferred from observed dipole gravity modes in 26 rotating stars with masses between 3 and 10 solar masses.
We find a wide range of internal mixing levels across the sample.
Stellar models with stratified mixing profiles in the envelope reveal the best asteroseismic performance.
Our results provide observational guidance for three-dimensional hydrodynamical simulations of transport processes in the deep interiors of stars.</p>
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<h3>Convective Boundary Mixing in Main-Sequence Stars: Theory and Empirical Constraints (Invited review)</h3>
<p><i>Anders & Pedersen 2023, Galaxies, Volume 11, Issue 2, id.56</i>
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<!-- <p><i>Anders & Pedersen 2023, Galaxies, Volume 11, Issue 2, id.56</i></p> -->
<p> <div style="float:right;width:50%;margin-left:15px;margin-top:10px"><img src="images/CBM_gradT_4panels.png" alt="" width="100%";/></div>
The convective envelopes of solar-type stars and the convective cores of intermediate- and high-mass stars share boundaries with stable radiative zones.
Through a host of processes we collectively refer to as "convective boundary mixing" (CBM), convection can drive efficient mixing in these nominally stable regions.
In this review, we discuss the current state of CBM research in the context of main-sequence stars through three lenses.
(1) We examine the most frequently implemented 1D prescriptions of CBM—exponential overshoot, step overshoot, and convective penetration—and we include a discussion of implementation degeneracies and how to convert between various prescriptions.
(2) Next, we examine the literature of CBM from a fluid dynamical perspective, with a focus on three distinct processes: convective overshoot, entrainment, and convective penetration.
(3) Finally, we discuss observational inferences regarding how much mixing should occur in the cores of intermediate- and high-mass stars as well as the implied constraints that these observations place on 1D CBM implementations.
We conclude with a discussion of pathways forward for future studies to place better constraints on this difficult challenge in stellar evolution modeling.</p>
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<h3>Stochastic low-frequency variability of 50 massive stars in the Cygnus OB associations and the Small Magellanic Cloud</h3>
<p><i>Pedersen & Bildsten 2025, Monthly Notices of the Royal Astronomical Society, Volume 539, Issue 3, pp. 2742-2764, 23 pp.</i>
</p>
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<p> <div style="float:right;width:50%;margin-left:15px;margin-top:10px"><img src="images/nu_char_vs_logLum_comp_v4_web.png" alt="" width="100%";/>
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In recent years, high-precision high-cadence space photometry has revealed that stochastic low-frequency (SLF) variability is common in the light curves of massive stars.
We use the data from the Transiting Exoplanet Survey Satellite to study and characterize the SLF variability found in a sample of 49 O- and B-type main-sequence stars across six Cygnus OB associations and one low-metallicity Small Magellanic Cloud star AV 232.
We compare these results to 53 previously studied SLF variables.
We adopt two different methods for characterizing the signal.
In the first, we follow earlier work and fit a Lorentzian-like profile to the power density spectrum of the residual light curve to derive the amplitude α<sub>0</sub>, characteristic frequency ν<sub>char</sub>, and slope γ of the variability.
In our second model-independent method, we calculate the root mean square (RMS) of the photometric variability as well as the frequency at 50% of the accumulated power spectral density, ν<sub>50%</sub>, and the width of the cumulative integrated power density, <i>w</i>.
For the full sample of 103 SLF variables, we find that α<sub>0</sub>, γ, <i>RMS</i>, ν<sub>50%</sub>, and w correlate with the spectroscopic luminosity of the stars.
Both α<sub>0</sub> and RMS appear to increase for more evolved stars, whereas ν<sub>char</sub> and ν<sub>50%</sub> both decrease.
Finally, we compare our results to 2D and 3D simulations of subsurface convection, core-generated internal gravity waves, and surface stellar winds, and find good agreement between the observed ν<sub>char</sub> of our sample and predictions from subsurface convection.
</p>
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<h3>Full list of talks</h3>
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<thead>
<tr>
<th>Year</th>
<th>Title</th>
<th>Location</th>
<th>Type</th>
<!-- <th>Recording</th> -->
</tr>
</thead>
<tbody>
<tr>
<td>2026</td>
<td><i>Insights from TESS on the variability of early-type stars in six Cygnus OB associations</i></td>
<td>ISSI-Beijing Workshop, International Space Science Institute Beijing, Beijing, China </td>
<td>Invited</td>
</tr>
<tr>
<td>2026</td>
<td><i>Introduction to the PLATO Guest Observer program</i></td>
<td>SPRIGS meeting, University of New South Wales, Sydney, Australia </td>
<td>Contributed</td>
</tr>
<tr>
<td>2025</td>
<td><i>Viewing stellar pulsations in colours with TESS, Gaia, PLATO, JWST, and Roman</i></td>
<td> Stars in Newcastle, Fort Scratchley, Newcastle, Australia </td>
<td>Contributed</td>
</tr>
<tr>
<td>2025</td>
<td><i>Viewing the interiors of O- and B-type stars using asteroseismology</i></td>
<td>Sydney Institute for Astronomy, University of Sydney, Australia</td>
<td>Seminar</td>
</tr>
<tr>
<td>2025</td>
<td><i>Viewing stellar interiors through the lens of asteroseismology</i></td>
<td>IAU Symposium 402, Ensenada, Mexico </td>
<td>Invited</td>
</tr>
<tr>
<td>2025</td>
<td><i>A study of stochastic low-frequency variability in 50 O- and B-type stars</i></td>
<td>TASC9/KASC16 Workshop, ISTA, Vienna, Austria </td>
<td>Contributed</td>
</tr>
<tr>
<td>2025</td>
<td><i>Stochastic low-frequency variability in O- and B-type stars</i></td>
<td>SPRIGS meeting, University of New South Wales, Sydney, Australia </td>
<td>Contributed</td>
</tr>
<tr>
<td>2024</td>
<td><i>Probing time dependent convective boundary mixing with gravity mode oscillations</i></td>
<td>Stars in Brisbane, University of Southern Queensland, Brisbane, Australia </td>
<td>Contributed</td>
</tr>
<tr>
<td>2024</td>
<td><i>Viewing the interiors of O- and B-type stars through the lens of asteroseismology</i></td>
<td>Monash University, Melbourne, Australia </td>
<td>Seminar</td>
<!-- <td><a href="https://www.youtube.com/watch?v=wIqYJafFS7c">Link</a></td> -->
</tr>
<tr>
<td>2024</td>
<td><i>What asteroseismology can tell us about O- and B-type stars</i></td>
<td>Institute of Astrophysics of the Canary Islands (IAC), Tenerife, Spain </td>
<td>Seminar</td>
<!-- <td><a href="https://iactalks.iac.es/talks/view/1785">Link</a></td> -->
</tr>
<tr>
<td>2024</td>
<td><i>Viewing stellar structure and evolution through the lens of asteroseismology</i></td>
<td>SONG 2024 Science Meeting, Tenerife, Spain </td>
<td>Invited</td>
</tr>
<tr>
<td>2024</td>
<td><i>What asteroseismology can tell us about O- and B-type stars</i></td>
<td>Macquarie University, Sydney, Australia </td>
<td>Seminar</td>
</tr>
<tr>
<td>2024</td>
<td><i>Asteroseismology of massive stars in the era of space telescopes</i></td>
<td>IAU Working Group on Active B Stars, Online </td>
<td>Seminar</td>
<!-- <td><a href="https://youtu.be/AG74PQ3rzoY">Link</a></td> -->
</tr>
<tr>
<td>2024</td>
<td><i>Stochastic low-frequency variability in O- and B-type stars</i></td>
<td>KITP Conference ”Stars with Lars”, KITP/UCSB, CA, USA </td>
<td>Invited</td>
</tr>
<tr>
<td>2023</td>
<td><i>Asteroseismology of massive stars in the era of space telescopes</i></td>
<td>Australian National University, Canberra, Australia </td>
<td>Colloquium</td>
</tr>
<tr>
<td>2023</td>
<td><i>Identifying contaminating sources in TESS light curves</i></td>
<td>TASC7/KASC14 Workshop, Honolulu, Hawaii, USA </td>
<td>Contributed</td>
</tr>
<tr>
<td>2023</td>
<td><i>Solving the puzzle of Fast Yellow Pulsating Supergiants</i></td>
<td>ASA Annual Science Meeting, Sydney, Australia </td>
<td>Contributed</td>
</tr>
<tr>
<td>2023</td>
<td><i>An asteroseismic view of internal mixing and angular momentum transport in B-type stars</i></td>
<td>University of New South Wales, Sydney, Australia </td>
<td>Seminar</td>
</tr>
<tr>
<td>2023</td>
<td><i>An asteroseismic view of internal mixing and angular momentum transport in B-type stars</i></td>
<td>IAU G2 online conference series </td>
<td>Seminar</td>
<!-- <td><a href="https://www.youtube.com/watch?v=N51tsafHU2o&t=2213s">Link</a></td> -->
</tr>
<tr>
<td>2022</td>
<td><i>Asteroseismology of O- and B-stars</i></td>
<td>ZTF Theory Meeting, Santa Margarita, California, USA </td>
<td>Contributed</td>
</tr>
<tr>
<td>2022</td>
<td><i>Assessing the interior mixing of B-type stars from gravity-mode asteroseismology</i></td>
<td>Canadian Institute for Theoretical Physics, University of Toronto, Canada </td>
<td>Seminar</td>
</tr>
<tr>
<td>2022</td>
<td><i>Asteroseismology in the TESS era</i></td>
<td>TESS AAS Splinter Session, USA </td>
<td>Invited</td>
</tr>
<tr>
<td>2021</td>
<td><i>Assessing the interior mixing of B-type stars from gravity-mode asteroseismology</i></td>
<td>Keele University, United Kingdom </td>
<td>Seminar</td>
</tr>
<tr>
<td>2021</td>
<td><i>Assessing the interior mixing of B-type stars using space photometry</i></td>
<td>NASA/Goddard Space Flight Center, USA </td>
<td>Colloquium</td>
</tr>
<tr>
<td>2021</td>
<td><i>An asteroseismic view on interior transport</i></td>
<td>KITP Conference ”Transport in Stellar Interiors”, KITP/UCSB, CA, USA </td>
<td>Invited</td>
<!-- <td><a href="https://www.youtube.com/watch?v=Hgdd9lQZzWc&t=1s">Link</a></td> -->
</tr>
<tr>
<td>2021</td>
<td><i>From stellar pulsations to stellar interiors</i></td>
<td>DTU Space, Denmark</td>
<td>Seminar</td>
</tr>
<tr>
<td>2021</td>
<td><i>An asteroseismic tour of the HR digram and new insights from TESS</i></td>
<td>TESS Science Conference II, Online (MIT/Cambridge) </td>
<td>Invited</td>
<!-- <td><a href="https://www.youtube.com/watch?v=GJK1TI4qwRM&t=475s">Link</a></td> -->
</tr>
<tr>
<td>2021</td>
<td><i>Probing the internal mixing of O- and B-type stars with asteroseismology</i></td>
<td>The European Astronomical Society Annual Meeting, Online </td>
<td>Invited</td>
</tr>
<tr>
<td>2021</td>
<td><i>From stellar pulsations to stellar interiors</i></td>
<td>Aspen Center for Physics, Colorado, USA</td>
<td>Seminar</td>
</tr>
<tr>
<td>2021</td>
<td><i>An asteroseismic view on internal mixing in B-type stars</i></td>
<td>Stellar Astophysics Centre (SAC), Aarhus University, Denmark </td>
<td>Seminar</td>
</tr>
<tr>
<td>2021</td>
<td><i>An asteroseismic view on internal mixing in B-type stars</i></td>
<td>Los Alamos National Laboratory, New Mexico, USA </td>
<td>Seminar</td>
</tr>
<tr>
<td>2021</td>
<td><i>An asteroseismic view on internal mixing in B-type stars</i></td>
<td>American Museum of National History Astrophysics Department, New York, USA</td>
<td>Seminar</td>
</tr>
<tr>
<td>2020</td>
<td><i>Combining Gaia, Kepler, and spectroscopic data in asteroseismic modelling of B stars: assessing interior mixing profiles</i></td>
<td>The European Astronomical Society Annual Meeting, Online (Leiden) </td>
<td>Contributed</td>
</tr>
<tr>
<td>2019</td>
<td><i>What TESS can do for massive stars</i></td>
<td>TASC5/KASC12 workshop, MIT/Cambridge, USA </td>
<td>Invited</td>
</tr>
<tr>
<td>2019</td>
<td><i>Mixing in B-type stars: From asteroseismology and spectroscopy</i></td>
<td>Stellar Hydro Days V, United Kingdom </td>
<td>Contributed</td>
</tr>
<tr>
<td>2018</td>
<td><i>Masses of cluster members from an asteroseismic point-of-view</i></td>
<td>Lorentz Center Workshop, Leiden, The Netherlands</td>
<td>Contributed</td>
</tr>
<tr>
<td>2018</td>
<td><i>Internal mixing in massive stars: From gravity modes, surface abundances, and Gaia astrometry</i></td>
<td>TASC4/KASC11 Workshop, Aarhus, Denmark </td>
<td>Contributed</td>
</tr>
<tr>
<td>2018</td>
<td><i>Parameter estimation and model selection in asteroseismology</i></td>
<td>Science Research Network (WOG) meeting of the FWO, Leuven, Belgium </td>
<td>Contributed</td>
</tr>
<tr>
<td>2018</td>
<td><i>Probing internal mixing from asteroseismology and surface abundances</i></td>
<td>Newcastle University, United Kingdom </td>
<td>Contributed</td>
</tr>
<tr>
<td>2018</td>
<td>1. <i>The shape of convective core overshooting and envelope mixing from gravity-mode asteroseismology</i>; 2. <i>The inclusion of a Gaia parallax in asteroseismic modelling of intermediate and high-mass stars</i></td>
<td>European Week of Astronomy and Space, Liverpool, United Kingdom </td>
<td>2 x Contributed</td>
</tr>
<tr>
<td>2017</td>
<td><i>What slowly pulsating B stars can tell us about internal mixing in massive stars</i></td>
<td>Stellar Astrophysics Center (SAC), Aarhus, Denmark </td>
<td>Seminar</td>
</tr>
<tr>
<td>2017</td>
<td><i>Constraining the shape of convective core overshooting using slowly pulsating B-type stars</i></td>
<td>Stellar Hydro Days IV, Victoria, Canada</td>
<td>Contributed</td>
</tr>
<tr>
<td>2017</td>
<td><i>Unraveling the internal mixing processes of the chemical factories of the Universe</i></td>
<td>Nederlandse Astronomenconferentie (NAC), Nijmegen, The Netherlands </td>
<td>Contributed</td>
</tr>
<tr>
<td>2016</td>
<td><i>Investigating the origin of flares in A-type stars</i></td>
<td>TASC2/KASC9 Workshop - SPACEINN & HELAS8 Conference, Portugal </td>
<td>Contributed</td>
</tr>
<tr>
<td>2016</td>
<td><i>Revisiting the A-type flaring stars reported from Kepler photometry: a critical investigation</i></td>
<td>Institute of Astronomy, KU Leuven, Belgium </td>
<td>Seminar</td>
</tr>
<tr>
<td>2015</td>
<td><i>The Carrington Event</i></td>
<td>Aarhus University, Denmark </td>
<td>Colloquium</td>
</tr>
<tr>
<td>2014</td>
<td><i>Do A-type stars flare?</i></td>
<td>Aarhus University, Denmark </td>
<td>Seminar</td>
</tr>
</tbody>
</table>
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