pith. sign in

arxiv: 2607.00663 · v1 · pith:BK2UQW3Qnew · submitted 2026-07-01 · 🌌 astro-ph.SR

Constraining the model-based uncertainties of asteroseismic magnetic field measurements in red giants

L. Buchele (1) , L. Bugnet (1) , N. Muntean (1) , E. Hatt (1 , 2) ((1) Institute of Science , Technology Austria , (2) School of Physics & Astronomy , University of Birmingham) This is my paper

Pith reviewed 2026-07-02 06:16 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords red giantsasteroseismologymagnetic fieldsstellar modelsfrequency shiftsmetallicitymodel uncertaintycore structure
0
0 comments X

The pith

The global magnetic sensitivity in red giant models recovers to 10% uncertainty with precise metallicity data.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper examines how to turn observed shifts in red giant oscillation frequencies into internal magnetic field strengths. The conversion requires a global magnetic sensitivity value taken from stellar models, which introduces its own uncertainty. Grids of MESA models reveal that this sensitivity varies with mass and metallicity, and tests on synthetic stars show it can be recovered to 10% accuracy when high-quality metallicity measurements are included in the fit. The work then applies the approach to real stars that already have magnetic field estimates and concludes that a 10% model-based uncertainty is appropriate under those conditions.

Core claim

Using MESA models, the global magnetic sensitivity shows a stronger dependence on mass for higher mass models and a stronger metallicity dependence for lower metallicity models. Recovery tests on synthetic stars demonstrate that the parameter recovers well, with an uncertainty of 10% when precise metallicity measurements are used. For stars with existing magnetic field measurements the dominant uncertainty is usually observational, although precise modeling can reduce the magnetic field uncertainty for stars with exceptional data. The recommendation is to obtain the global magnetic sensitivity from both asteroseismic and high-quality spectroscopic data and to adopt a model-based uncertainty

What carries the argument

The global magnetic sensitivity (core structure parameter), the factor that converts an observed frequency shift into a radial magnetic field strength inside the asymptotic framework for red giant oscillations.

If this is right

  • The sensitivity depends more strongly on mass in higher-mass models and more strongly on metallicity in lower-metallicity models.
  • Recovery to 10% is possible when precise metallicity is supplied to the fitting process.
  • For stars with the best data, reducing the model uncertainty on sensitivity measurably tightens the final magnetic field error bar.
  • In most published cases the observational error remains larger than the 10% model contribution.
  • Future measurements should combine asteroseismic frequencies with high-quality spectroscopy to reach the 10% floor.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • A standard 10% model floor could be folded into error budgets for other red-giant asteroseismic quantities that also rely on core structure.
  • If unmodeled physics in real cores produces a larger scatter than the synthetic tests show, the adopted uncertainty would need to be increased.
  • High-precision spectroscopic metallicities become a high-leverage input for any magnetic-field campaign that uses this method.
  • The same recovery exercise could be repeated with alternate evolution codes to test whether the 10% figure is code-dependent.

Load-bearing premise

MESA models correctly reproduce the core structure that sets the true global magnetic sensitivity in real red giants, so that recovery tests on synthetic stars drawn from the same models bound the real model errors.

What would settle it

A systematic offset between the sensitivities recovered from MESA grids and the values required to bring model magnetic fields into agreement with independent field measurements on the same stars.

Figures

Figures reproduced from arXiv: 2607.00663 by 2) ((1) Institute of Science, (2) School of Physics & Astronomy, E. Hatt (1, L. Buchele (1), L. Bugnet (1), N. Muntean (1), Technology Austria, University of Birmingham).

Figure 1
Figure 1. Figure 1: Dependence of the global magnetic sensitivity, [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Connection between mean molecular weight profiles and [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Dependence of I on metallicity for three 1M⊙ models with the same ∆Π1. The top panel shows the cumulative integral of the numerator of Equation 4. The right-most value of each line shows the value of I for each model plotted here. The sec￾ond, third, and fourth panels show the N 3 /ρ, N 2 , and ρ profiles, respectively. Seismic: ∆ν, ∆Π1 Seismic + Spectro: ∆ν, ∆Π1, Teff, [Fe/H], σ[Fe/H] = 0.25 Seismic + HQ … view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of the error on our inferred value of [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Summary of δI/I distributions calculated using the Seismic + Spectro (top) and Seismic + HQ Spectro (bottom) sets of parameters binned by mass (left), [Fe/H] (center), and ∆Π1 (right). Each bin is plotted at the center of the bin, with a slight offset for visibility. The points correspond to the median of the distribution, and the error bars indicate the first and third quartiles. The gray lines show error… view at source ↗
Figure 6
Figure 6. Figure 6: Comparison between the values of I obtained using our grid and fitting method and the I values in previous works. There are several stars that are studied by both Li et al. (2023a) and Hatt et al. (2024). As each study uses different spectroscopic measurements and obtains different seismic parameters, we fit these stars twice. Once using the stellar parameters from Li et al. (2023a) (plotted as red triangl… view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of our inferred average magnetic field [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
read the original abstract

Magnetic fields inside red giants are measured using shifts to the oscillation frequencies. However, in the asymptotic framework, converting a frequency shift into a radial magnetic field strength requires knowing the global magnetic sensitivity. This parameter (also called the core structure parameter) must be inferred from stellar models, introducing a source of uncertainty. We seek to understand how the global magnetic sensitivity depends on stellar properties such as mass and metallicity, and to quantify the model-based uncertainty on magnetic field measurements. We also explore which stellar properties are key to finding a precise and accurate estimate of the global magnetic sensitivity. Using MESA models, we examine how the global magnetic sensitivity changes with mass, metallicity, and age. We then create a set of synthetic stars and test how well we recover the sensitivity parameter. We consider different grid construction approaches and the choice of which observables are used in the fitting process. We find that the global magnetic sensitivity shows a stronger dependence on mass for higher mass models and a stronger metallicity dependence for lower metallicity models. Our approach recovers the sensitivity parameter well, with an uncertainty of 10% when precise metallicity measurements are used. We apply our method to stars with existing magnetic field measurements. In most cases, the dominant source of uncertainty remains observational, although precise modeling can significantly reduce the magnetic field uncertainty for stars with exceptional data. With careful fitting, models yield accurate values for the global magnetic sensitivity. We recommend that future work obtain the global magnetic sensitivity using both asteroseismic and high-quality spectroscopic data. Under these conditions, we recommend adopting a model-based uncertainty of 10% on the sensitivity parameter.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The manuscript uses MESA stellar models to examine how the global magnetic sensitivity (core structure parameter) in red giants depends on mass, metallicity, and age. It constructs synthetic stars from the same model grid and performs recovery tests under varying grid approaches and observable choices, concluding that the parameter is recovered with 10% uncertainty when precise metallicity measurements are used. The paper recommends adopting a 10% model-based uncertainty on this parameter for asteroseismic magnetic field measurements and suggests combining asteroseismic and high-quality spectroscopic data.

Significance. If the central result holds, the work supplies a practical, quantitative prescription for model uncertainties in converting asteroseismic frequency shifts to magnetic field strengths, which could help standardize error budgets in the field. The finding that precise metallicity reduces the uncertainty and that observational errors often dominate is useful for observers. The internal consistency of the MESA-based pipeline is demonstrated, but the absence of external validation limits broader impact.

major comments (1)
  1. [Abstract and synthetic recovery tests] Abstract and synthetic star recovery tests: Recovery accuracy is demonstrated on synthetic stars generated from the identical MESA model grid used to compute the sensitivity values. This quantifies scatter from grid sampling and metallicity precision but tests only internal consistency of the modeling pipeline rather than accuracy of the core structure parameter against independent data or alternative stellar models (e.g., different codes or observed benchmarks). If MESA systematically offsets the sensitivity relative to nature, the quoted 10% figure underestimates the true model contribution to magnetic-field error.
minor comments (2)
  1. The abstract and methods description lack specifics on MESA grid resolution (e.g., mass and metallicity spacing), the exact set of fitting observables, and whether any post-hoc data cuts were applied; these details are required to evaluate the robustness of the 10% recovery claim.
  2. The dependence statements (stronger mass dependence at higher masses, stronger metallicity dependence at lower metallicities) are stated qualitatively; quantitative measures such as partial derivatives or tabulated trends with uncertainties would strengthen the presentation.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the constructive report. The primary concern is that our synthetic recovery tests demonstrate only internal consistency within the MESA grid rather than external accuracy. We address this point directly below and agree that clarification is warranted.

read point-by-point responses

  1. Referee: [Abstract and synthetic recovery tests] Abstract and synthetic star recovery tests: Recovery accuracy is demonstrated on synthetic stars generated from the identical MESA model grid used to compute the sensitivity values. This quantifies scatter from grid sampling and metallicity precision but tests only internal consistency of the modeling pipeline rather than accuracy of the core structure parameter against independent data or alternative stellar models (e.g., different codes or observed benchmarks). If MESA systematically offsets the sensitivity relative to nature, the quoted 10% figure underestimates the true model contribution to magnetic-field error.

    Authors: We agree that the recovery tests use synthetic stars drawn from the same MESA grid and therefore quantify internal consistency of the pipeline (grid sampling, observable selection, and metallicity precision) rather than absolute accuracy against independent stellar models or observations. This scope was chosen because the global magnetic sensitivity is itself a model-derived quantity; the 10% figure we recommend is the uncertainty arising from the modeling procedure within MESA when high-quality spectroscopic metallicity is available. We acknowledge that any systematic offset between MESA and nature (or other codes) would represent an additional, unquantified contribution to the total model uncertainty. We will revise the abstract and the final discussion paragraph to state explicitly that the quoted 10% uncertainty applies to the MESA-based recovery process and that external validation against other codes would be a valuable extension. revision: yes

Circularity Check

1 steps flagged

Recovery tests on synthetic stars from the same MESA grid quantify internal consistency of the sensitivity parameter rather than external model accuracy

specific steps
  1. fitted input called prediction [Abstract]
    "We then create a set of synthetic stars and test how well we recover the sensitivity parameter. ... Our approach recovers the sensitivity parameter well, with an uncertainty of 10% when precise metallicity measurements are used. ... We recommend adopting a model-based uncertainty of 10% on the sensitivity parameter."

    Synthetic stars are drawn from the same MESA grid used to compute the global magnetic sensitivity (core structure parameter). The recovery test therefore measures scatter due to grid sampling, observable choice, and metallicity precision within the model framework, making the 10% figure a measure of internal pipeline consistency rather than an independent bound on model error for real stars.

full rationale

The paper's recommendation of a 10% model-based uncertainty on the global magnetic sensitivity is derived from recovery experiments on synthetic stars generated from the identical MESA model grid used to compute the sensitivity values themselves. This tests how well the fitting procedure recovers known inputs under controlled conditions but does not validate the core structure parameter against real red giants or independent modeling frameworks. The derivation chain for the uncertainty figure therefore reduces to internal model consistency by construction. No other load-bearing steps exhibit the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the fidelity of MESA models for the core structure parameter and on the assumption that synthetic recovery tests bound real observational errors; these are standard domain assumptions rather than new free parameters or invented entities.

axioms (1)
  • domain assumption MESA stellar evolution models accurately reproduce the core properties that set the global magnetic sensitivity in real red giants
    Invoked throughout the model grid construction and recovery tests described in the abstract.

pith-pipeline@v0.9.1-grok · 5866 in / 1248 out tokens · 28753 ms · 2026-07-02T06:16:39.465492+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

82 extracted references · 81 canonical work pages · 19 internal anchors

  1. [1]

    The Astronomy and Astrophysics Review , author =

    Giant star seismology , volume =. The Astronomy and Astrophysics Review , author =. 2017 , note =. doi:10.1007/s00159-017-0101-x , abstract =

    work page doi:10.1007/s00159-017-0101-x 2017

  2. [2]

    Magnetic fields of 30 to 100

    Li, Gang and Deheuvels, Sébastien and Ballot, Jérôme and Lignières, François , month = oct, year =. Magnetic fields of 30 to 100. Nature , publisher =. doi:10.1038/s41586-022-05176-0 , abstract =

    work page doi:10.1038/s41586-022-05176-0

  3. [3]

    Astronomy & Astrophysics , author =

    Magnetic signatures on mixed-mode frequencies:. Astronomy & Astrophysics , author =. 2021 , pages =. doi:10.1051/0004-6361/202039159 , abstract =

    work page doi:10.1051/0004-6361/202039159 2021

  4. [4]

    Astronomy & Astrophysics , author =

    Internal magnetic fields in 13 red giants detected by asteroseismology , volume =. Astronomy & Astrophysics , author =. 2023 , pages =. doi:10.1051/0004-6361/202347260 , abstract =

    work page doi:10.1051/0004-6361/202347260 2023

  5. [5]

    Astronomy & Astrophysics , author =

    Strong magnetic fields detected in the cores of 11 red giant stars using gravity-mode period spacings , volume =. Astronomy & Astrophysics , author =. 2023 , pages =. doi:10.1051/0004-6361/202245282 , abstract =

    work page doi:10.1051/0004-6361/202245282 2023

  6. [6]

    Monthly Notices of the Royal Astronomical Society , author =

    Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2024 , pages =. doi:10.1093/mnras/stae2053 , abstract =

    work page doi:10.1093/mnras/stae2053 2024

  7. [7]

    The Astrophysical Journal Supplement Series , author =

    Asteroseismology of 16,000. The Astrophysical Journal Supplement Series , author =. 2018 , pages =. doi:10.3847/1538-4365/aaaf74 , abstract =

    work page doi:10.3847/1538-4365/aaaf74 2018

  8. [8]

    and Bildsten, L

    Paxton, B. and Bildsten, L. and Dotter, A. and Herwig, F. and Lesaffre, P. and Timmes, F. , month = jan, year =. Modules for. doi:10.1088/0067-0049/192/1/3 , journal =

    work page doi:10.1088/0067-0049/192/1/3

  9. [9]

    Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars

    Paxton, B. and Cantiello, M. and Arras, P. and Bildsten, L. and Brown, E. F. and Dotter, A. and Mankovich, C. and Montgomery, M. H. and Stello, D. and Timmes, F. X. and Townsend, R. , month = sep, year =. Modules for. doi:10.1088/0067-0049/208/1/4 , journal =

    work page internal anchor Pith review doi:10.1088/0067-0049/208/1/4

  10. [10]

    Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions

    Paxton, B. and Marchant, P. and Schwab, J. and Bauer, E. B. and Bildsten, L. and Cantiello, M. and Dessart, L. and Farmer, R. and Hu, H. and Langer, N. and Townsend, R. H. D. and Townsley, D. M. and Timmes, F. X. , month = sep, year =. Modules for. doi:10.1088/0067-0049/220/1/15 , journal =

    work page internal anchor Pith review doi:10.1088/0067-0049/220/1/15

  11. [11]

    Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions

    Paxton, B. and Schwab, J. and Bauer, E. B. and Bildsten, L. and Blinnikov, S. and Duffell, P. and Farmer, R. and Goldberg, J. A. and Marchant, P. and Sorokina, E. and Thoul, A. and Townsend, R. H. D. and Timmes, F. X. , month = feb, year =. Modules for. doi:10.3847/1538-4365/aaa5a8 , journal =

    work page internal anchor Pith review doi:10.3847/1538-4365/aaa5a8

  12. [12]

    , author =

    Modules for. , author =. 2019 , keywords =. doi:10.3847/1538-4365/ab2241 , number =

    work page doi:10.3847/1538-4365/ab2241 2019

  13. [13]

    , keywords =

    Modules for. , author =. 2023 , keywords =. doi:10.3847/1538-4365/acae8d , number =

    work page doi:10.3847/1538-4365/acae8d 2023

  14. [14]

    The Astrophysical Journal , author =

    Beyond. The Astrophysical Journal , author =. 2025 , pages =. doi:10.3847/1538-4357/ae0c1a , abstract =

    work page doi:10.3847/1538-4357/ae0c1a 2025

  15. [15]

    The evolution of AGB stars with convective overshoot

    The evolution of AGB stars with convective overshoot. , keywords =. doi:10.48550/arXiv.astro-ph/0007139 , archivePrefix =. astro-ph/0007139 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0007139

  16. [16]

    On the distribution of points in a cube and the approximate evaluation of integrals

    On the distribution of points in a cube and the approximate evaluation of integrals , journal =. 1967 , issn =. doi:https://doi.org/10.1016/0041-5553(67)90144-9 , url =

    work page doi:10.1016/0041-5553(67)90144-9 1967

  17. [17]

    2016 , pages =

    The Astrophysical Journal , author =. 2016 , pages =. doi:10.3847/0004-637X/830/1/31 , abstract =

    work page doi:10.3847/0004-637x/830/1/31 2016

  18. [18]

    2013 , pages =

    Monthly Notices of the Royal Astronomical Society , author =. 2013 , pages =. doi:10.1093/mnras/stt1533 , abstract =

    work page doi:10.1093/mnras/stt1533 2013

  19. [19]

    2013 , pages =

    The Astrophysical Journal , author =. 2013 , pages =. doi:10.1088/2041-8205/765/2/L41 , abstract =

    work page doi:10.1088/2041-8205/765/2/l41 2013

  20. [20]

    Astronomy & Astrophysics , author =

    Seismic signature of electron degeneracy in the core of red giants:. Astronomy & Astrophysics , author =. 2022 , pages =. doi:10.1051/0004-6361/202142094 , abstract =

    work page doi:10.1051/0004-6361/202142094 2022

  21. [21]

    and Kurtz, Donald W

    Takata, Masao and Murphy, Simon J. and Kurtz, Donald W. and Saio, Hideyuki and Shibahashi, Hiromoto , month = nov, year =. Asteroseismic detection of a predominantly toroidal magnetic field in the deep interior of the main-sequence. doi:10.48550/arXiv.2512.00786 , abstract =

    work page doi:10.48550/arxiv.2512.00786

  22. [22]

    , keywords =

    Angular momentum and chemical transport by azimuthal magnetorotational instability in radiative stellar interiors. , keywords =. doi:10.1051/0004-6361/202347672 , adsurl =

    work page doi:10.1051/0004-6361/202347672

  23. [23]

    Asteroseismology of evolved stars to constrain the internal transport of angular momentum. VI. Testing a parametric formulation for the azimuthal magneto-rotational instability. , keywords =. doi:10.1051/0004-6361/202245519 , archivePrefix =. 2302.07811 , primaryClass =

    work page doi:10.1051/0004-6361/202245519

  24. [24]

    , keywords =

    Rotation in stellar interiors: General formulation and an asteroseismic-calibrated transport by the Tayler instability. , keywords =. doi:10.1051/0004-6361/202243781 , archivePrefix =. 2309.17396 , primaryClass =

    work page doi:10.1051/0004-6361/202243781

  25. [25]

    , keywords =

    Angular momentum transport in a contracting stellar radiative zone embedded in a large-scale magnetic field. , keywords =. doi:10.1051/0004-6361/202141613 , archivePrefix =. 2201.02645 , primaryClass =

    work page doi:10.1051/0004-6361/202141613

  26. [26]

    Asteroseismology of evolved stars to constrain the internal transport of angular momentum. II. Test of a revised prescription for transport by the Tayler instability. , keywords =. doi:10.1051/0004-6361/201936348 , archivePrefix =. 2001.11525 , primaryClass =

    work page doi:10.1051/0004-6361/201936348 2001

  27. [27]

    Slowing the Spins of Stellar Cores

    Slowing the spins of stellar cores. , keywords =. doi:10.1093/mnras/stz514 , archivePrefix =. 1902.08227 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz514 1902

  28. [28]

    Angular momentum transport efficiency in post-main sequence low-mass stars

    Angular momentum transport efficiency in post-main sequence low-mass stars. , keywords =. doi:10.1051/0004-6361/201527591 , archivePrefix =. 1603.01119 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201527591

  29. [29]

    Angular momentum transport within evolved low-mass stars

    Angular Momentum Transport within Evolved Low-mass Stars. , keywords =. doi:10.1088/0004-637X/788/1/93 , archivePrefix =. 1405.1419 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/788/1/93

  30. [30]

    , keywords =

    Asteroseismic measurement of core and envelope rotation rates for 2006 red giant branch stars. , keywords =. doi:10.1051/0004-6361/202449882 , archivePrefix =. 2405.12116 , primaryClass =

    work page doi:10.1051/0004-6361/202449882 2006

  31. [31]

    , keywords =

    Seismic evidence for near solid-body rotation in two Kepler subgiants and implications for angular momentum transport. , keywords =. doi:10.1051/0004-6361/202038578 , archivePrefix =. 2007.02585 , primaryClass =

    work page doi:10.1051/0004-6361/202038578 2007

  32. [32]

    Core rotation braking on the red giant branch for various mass ranges

    Core rotation braking on the red giant branch for various mass ranges. , keywords =. doi:10.1051/0004-6361/201832822 , archivePrefix =. 1802.04558 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201832822

  33. [33]

    Internal rotation of 13 low-mass low-luminosity red giants in the Kepler field

    Internal rotation of 13 low-mass low-luminosity red giants in the Kepler field. , keywords =. doi:10.1051/0004-6361/201629186 , archivePrefix =. 1702.07910 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629186

  34. [34]

    Internal rotation of the red-giant star KIC 4448777 by means of asteroseismic inversion

    Internal Rotation of the Red-giant Star KIC 4448777 by Means of Asteroseismic Inversion. , keywords =. doi:10.3847/0004-637X/817/1/65 , archivePrefix =. 1511.06160 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/817/1/65

  35. [35]

    Seismic constraints on the radial dependence of the internal rotation profiles of six Kepler subgiants and young red giants

    Seismic constraints on the radial dependence of the internal rotation profiles of six Kepler subgiants and young red giants. , keywords =. doi:10.1051/0004-6361/201322779 , archivePrefix =. 1401.3096 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322779

  36. [36]

    Spin down of the core rotation in red giants

    Spin down of the core rotation in red giants. , keywords =. doi:10.1051/0004-6361/201220106 , archivePrefix =. 1209.3336 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220106

  37. [37]

    Fast core rotation in red-giant stars revealed by gravity-dominated mixed modes

    Fast core rotation in red-giant stars as revealed by gravity-dominated mixed modes. , keywords =. doi:10.1038/nature10612 , archivePrefix =. 1112.2825 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature10612

  38. [38]

    , keywords =

    The robustness of inferred envelope and core rotation rates of red giant stars from asteroseismology. , keywords =. doi:10.1051/0004-6361/202449901 , archivePrefix =. 2411.05515 , primaryClass =

    work page doi:10.1051/0004-6361/202449901

  39. [39]

    , keywords =

    The Astrophysical Journal Supplement Series , author =. 2025 , pages =. doi:10.3847/1538-4365/ad9fef , abstract =

    work page doi:10.3847/1538-4365/ad9fef 2025

  40. [40]

    Gaia Data Release 2: first stellar parameters from Apsis

    Gaia Data Release 2. First stellar parameters from Apsis. , keywords =. doi:10.1051/0004-6361/201732516 , archivePrefix =. 1804.09374 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201732516

  41. [41]

    Rogers, F. J. and Nayfonov, A. , month = sep, year =. Updated and. doi:10.1086/341894 , journal =

    work page doi:10.1086/341894

  42. [42]

    Irwin, Alan. W. , year =. The

  43. [43]

    , author =

    Skye:. , author =. 2021 , keywords =. doi:10.3847/1538-4357/abf48e , number =

    work page doi:10.3847/1538-4357/abf48e 2021

  44. [44]

    , keywords =

    Standard Solar Composition. , keywords =. doi:10.1023/A:1005161325181 , adsurl =

    work page doi:10.1023/a:1005161325181

  45. [45]

    Iglesias, C. A. and Rogers, F. J. , month = jun, year =. Updated. doi:10.1086/177381 , journal =

    work page doi:10.1086/177381

  46. [46]

    Iglesias, C. A. and Rogers, F. J. , month = aug, year =. Radiative opacities for carbon- and oxygen-rich mixtures , volume =. doi:10.1086/172958 , journal =

    work page doi:10.1086/172958

  47. [47]

    Ferguson, J. W. and Alexander, D. R. and Allard, F. and Barman, T. and Bodnarik, J. G. and Hauschildt, P. H. and Heffner-Wong, A. and Tamanai, A. , month = apr, year =. Low-. doi:10.1086/428642 , journal =

    work page doi:10.1086/428642

  48. [48]

    The Astrophysical Journal , author =

    An. The Astrophysical Journal , author =. 2024 , pages =. doi:10.3847/1538-4357/ad4355 , abstract =

    work page doi:10.3847/1538-4357/ad4355 2024

  49. [49]

    Cyburt, R. H. and Amthor, A. M. and Ferguson, R. and Meisel, Z. and Smith, K. and Warren, S. and Heger, A. and Hoffman, R. D. and Rauscher, T. and Sakharuk, A. and Schatz, H. and Thielemann, F. K. and Wiescher, M. , month = jul, year =. The. doi:10.1088/0067-0049/189/1/240 , journal =

    work page doi:10.1088/0067-0049/189/1/240

  50. [50]

    , author =

    A compilation of charged-particle induced thermonuclear reaction rates , volume =. , author =. 1999 , pages =. doi:10.1016/S0375-9474(99)00030-5 , number =

    work page doi:10.1016/s0375-9474(99)00030-5 1999

  51. [51]

    Fuller, G. M. and Fowler, W. A. and Newman, M. J. , month = jun, year =. Stellar weak interaction rates for intermediate-mass nuclei. doi:10.1086/163208 , journal =

    work page doi:10.1086/163208

  52. [52]

    and Hino, M

    Oda, T. and Hino, M. and Muto, K. and Takahara, M. and Sato, K. , month = mar, year =. Rate. doi:10.1006/adnd.1994.1007 , journal =

    work page doi:10.1006/adnd.1994.1007 1994

  53. [53]

    and Martínez-Pinedo, G

    Langanke, K. and Martínez-Pinedo, G. , month = jun, year =. Shell-model calculations of stellar weak interaction rates:. doi:10.1016/S0375-9474(00)00131-7 , journal =

    work page doi:10.1016/s0375-9474(00)00131-7

  54. [54]

    Studies in Stellar Evolution. III. The Calculation of Model Envelopes. , year = 1965, month = oct, volume =. doi:10.1086/148357 , adsurl =

    work page doi:10.1086/148357 1965

  55. [55]

    Exploring

    Buchele, Lynn , month = jul, year =. Exploring. Research Notes of the AAS , publisher =. doi:10.3847/2515-5172/adf06d , abstract =

    work page doi:10.3847/2515-5172/adf06d

  56. [56]

    , keywords =

    Characterization of the power excess of solar-like oscillations in red giants with Kepler. , keywords =. doi:10.1051/0004-6361/20111735210.1086/141952 , archivePrefix =. 1110.0980 , primaryClass =

    work page doi:10.1051/0004-6361/20111735210.1086/141952

  57. [57]

    , keywords =

    Asteroseismic fingerprints of stellar mergers. , keywords =. doi:10.1093/mnras/stab2528 , archivePrefix =. 2108.10322 , primaryClass =

    work page doi:10.1093/mnras/stab2528

  58. [58]

    Astronomy & Astrophysics , author =

    The role of stellar model input in correcting the asteroseismic scaling relations:. Astronomy & Astrophysics , author =. 2025 , pages =. doi:10.1051/0004-6361/202554089 , abstract =

    work page doi:10.1051/0004-6361/202554089 2025

  59. [59]

    Monthly Notices of the Royal Astronomical Society , author =

    A prescription for the asteroseismic surface correction , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2023 , pages =. doi:10.1093/mnras/stad1445 , abstract =

    work page doi:10.1093/mnras/stad1445 2023

  60. [60]

    arXiv e-prints , keywords =

    Seismic detection of core magnetic fields in red giants using the gravity offset. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.14570 , archivePrefix =. 2602.14570 , primaryClass =

    work page doi:10.48550/arxiv.2602.14570

  61. [61]

    Astronomy & Astrophysics , author =

    Improved asteroseismic inversions for red-giant surface rotation rates , volume =. Astronomy & Astrophysics , author =. 2022 , pages =. doi:10.1051/0004-6361/202142510 , abstract =

    work page doi:10.1051/0004-6361/202142510 2022

  62. [62]

    , keywords =

    Asteroseismology of 3642 Kepler Red Giants: Correcting the Scaling Relations Based on Detailed Modeling. , keywords =. doi:10.3847/1538-4357/ac4fbf , archivePrefix =. 2201.09577 , primaryClass =

    work page doi:10.3847/1538-4357/ac4fbf

  63. [63]

    Determining ages from detailed modelling

    Asteroseismology of 36 Kepler subgiants - II. Determining ages from detailed modelling. , keywords =. doi:10.1093/mnras/staa1350 , archivePrefix =. 2006.00901 , primaryClass =

    work page doi:10.1093/mnras/staa1350 2006

  64. [64]

    , keywords =

    Stellar Models are Reliable at Low Metallicity: An Asteroseismic Age for the Ancient Very Metal-poor Star KIC 8144907. , keywords =. doi:10.3847/1538-4357/ad7110 , archivePrefix =. 2407.17566 , primaryClass =

    work page doi:10.3847/1538-4357/ad7110

  65. [65]

    , keywords =

    TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones. , keywords =. doi:10.3847/1538-4357/ae0711 , archivePrefix =. 2509.12513 , primaryClass =

    work page doi:10.3847/1538-4357/ae0711

  66. [66]

    , keywords =

    Realistic Uncertainties for Fundamental Properties of Asteroseismic Red Giants and the Interplay between Mixing Length, Metallicity, and max. , keywords =. doi:10.3847/1538-4357/ad6c3e , archivePrefix =. 2407.09967 , primaryClass =

    work page doi:10.3847/1538-4357/ad6c3e

  67. [67]

    A new correction of stellar oscillation frequencies for near-surface effects

    A new correction of stellar oscillation frequencies for near-surface effects. , keywords =. doi:10.1051/0004-6361/201424325 , archivePrefix =. 1408.0986 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201424325

  68. [68]

    , keywords =

    PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators. , keywords =. doi:10.1093/mnras/stab2886 , archivePrefix =. 2110.03332 , primaryClass =

    work page doi:10.1093/mnras/stab2886

  69. [69]

    Astronomy & Astrophysics , author =

    Probing the internal magnetism of stars using asymptotic magneto-asteroseismology , volume =. Astronomy & Astrophysics , author =. 2021 , pages =. doi:10.1051/0004-6361/202039180 , abstract =

    work page doi:10.1051/0004-6361/202039180 2021

  70. [70]

    Astronomy & Astrophysics , author =

    Asymmetries of frequency splittings of dipolar mixed modes:. Astronomy & Astrophysics , author =. 2023 , pages =. doi:10.1051/0004-6361/202346832 , abstract =

    work page doi:10.1051/0004-6361/202346832 2023

  71. [71]

    The Astrophysical Journal , author =

    Detectability of. The Astrophysical Journal , author =. 2024 , pages =. doi:10.3847/1538-4357/ad4708 , abstract =

    work page doi:10.3847/1538-4357/ad4708 2024

  72. [72]

    Astronomy & Astrophysics , author =

    Unveiling complex magnetic field configurations in red giant stars , volume =. Astronomy & Astrophysics , author =. 2024 , pages =. doi:10.1051/0004-6361/202450918 , abstract =

    work page doi:10.1051/0004-6361/202450918 2024

  73. [73]

    Asteroseismology Can Reveal Strong Internal Magnetic Fields in Red Giant Stars

    Asteroseismology can reveal strong internal magnetic fields in red giant stars. Science , keywords =. doi:10.1126/science.aac6933 , archivePrefix =. 1510.06960 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.aac6933

  74. [74]

    , keywords =

    Effect of a strong magnetic field on gravity-mode period spacings in red giant stars. , keywords =. doi:10.1093/mnras/staa1823 , archivePrefix =. 2006.08635 , primaryClass =

    work page doi:10.1093/mnras/staa1823 2006

  75. [75]

    , keywords =

    Asteroseismic g-mode period spacings in strongly magnetic rotating stars. , keywords =. doi:10.1093/mnras/stad3461 , archivePrefix =. 2310.19873 , primaryClass =

    work page doi:10.1093/mnras/stad3461

  76. [76]

    , keywords =

    Perturbative analysis of the effect of a magnetic field on gravito-inertial modes. , keywords =. doi:10.1051/0004-6361/202348243 , archivePrefix =. 2311.13296 , primaryClass =

    work page doi:10.1051/0004-6361/202348243

  77. [77]

    Near-critical magnetic fields in Kepler red giants

    Deheuvels, S. and Ballot, J. and Lignières, F. and Li, G. and Villate, M. , month = apr, year =. Near-critical magnetic fields in. doi:10.48550/arXiv.2604.09901 , abstract =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.09901

  78. [78]

    Astronomy & Astrophysics , author =

    Magnetic signatures on mixed-mode frequencies:. Astronomy & Astrophysics , author =. 2022 , pages =. doi:10.1051/0004-6361/202243167 , abstract =

    work page doi:10.1051/0004-6361/202243167 2022

  79. [79]

    Astronomy & Astrophysics , author =

    Modeling of magneto-rotational stellar evolution:. Astronomy & Astrophysics , author =. 2021 , pages =. doi:10.1051/0004-6361/202039253 , abstract =

    work page doi:10.1051/0004-6361/202039253 2021

  80. [80]

    Surface rotation of Kepler red giant stars

    Surface rotation of Kepler red giant stars. , keywords =. doi:10.1051/0004-6361/201629884 , archivePrefix =. 1707.05989 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629884

Showing first 80 references.