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arxiv: 2605.23515 · v1 · pith:EST3HFHEnew · submitted 2026-05-22 · 🌌 astro-ph.SR

Ensemble asteroseismology: An ensemble approach to detecting signatures of solar-like oscillations in K-dwarfs

William J. Chaplin , Tiago L. Campante , Mikkel N. Lund , Martin B. Nielsen , Guy R. Davies , Emily Hatt , Rachel Howe , Amalie Stokholm This is my paper

Pith reviewed 2026-05-25 03:02 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords asteroseismologyK-dwarfssolar-like oscillationsensemble detectionpower spectraPLATO missiongranulation
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The pith

Stacking weighted power spectra from many similar K-dwarfs detects their shared oscillation envelope.

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

The paper proposes combining frequency power spectra from hundreds of K-dwarfs in narrow effective temperature ranges through weighted stacking. This ensemble approach improves detectability of the composite oscillation power envelope even when individual stars yield no usable signal. The resulting envelope supplies diagnostics of granulation, magneto-convection, and magnetic activity effects on the modes. Numerical predictions from the PLATO Input Catalogue and an analytical approximation both indicate that solid detections remain feasible well into the K-dwarf regime.

Core claim

By weighting and stacking frequency power spectra from K-dwarfs lying in constrained ranges of effective temperature, the ensemble method detects and measures the characteristics of the composite envelope of oscillation power, providing diagnostics of granulation and magneto-convection and the impact of magnetic activity on the modes, even though individual oscillation frequencies cannot be extracted.

What carries the argument

Weighted stacking of frequency power spectra from an ensemble of stars with similar effective temperatures to form a composite oscillation power envelope.

If this is right

  • PLATO can deliver solid ensemble detections of oscillations well into the K-dwarf regime.
  • The composite envelope yields diagnostics of granulation, magneto-convection, and magnetic activity effects on the modes.
  • An analytical approximation derived from the method allows quick predictions for other future or planned missions without discrete numerical sampling.
  • The approach extends the reach of asteroseismology beyond the modest number of individual K-dwarf detections possible with PLATO or prior missions.

Where Pith is reading between the lines

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

  • The method could be tested first on existing Kepler or TESS fields containing many K-dwarfs to validate the stacking before PLATO data arrive.
  • If successful, similar ensemble stacking might apply to other stellar types or to ground-based radial-velocity surveys where individual signals remain marginal.
  • The composite envelope measurements could feed into models of how magnetic activity scales with stellar mass and rotation in the K-dwarf domain.

Load-bearing premise

K-dwarfs in narrow effective temperature ranges have oscillation power envelopes similar enough that weighted stacking does not smear or dilute the composite signal.

What would settle it

A stacked spectrum from PLATO data on K-dwarfs in a chosen temperature bin that shows no statistically significant power excess above the background in the frequency range expected for solar-like oscillations.

Figures

Figures reproduced from arXiv: 2605.23515 by Amalie Stokholm, Emily Hatt, Guy R. Davies, Martin B. Nielsen, Mikkel N. Lund, Rachel Howe, Tiago L. Campante, William J. Chaplin.

Figure 1
Figure 1. Figure 1: An HR diagram showing stars in the PIC on the lower [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The median M, R, νmax (top row), Ptot and σhr (bottom row) of each PIC subsample as a function of the central temperature of the bin. The shaded regions bound the 16th and 84th percentiles. For the Ptot plot, the shading is associated to the s = 1.5 predictions. in [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Prediction results using data from the PIC, for three temperature bins (by row); di [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Estimated sPSD and pfinal from the analytical predictions for the 4300 ≤ Teff < 4700 K temperature bin, with different rows showing predictions for different numbers of PLATO cameras. of detectability for individual stars. The cumulative gains given by combining data on different stars are much easier to predict in the cluster scenario, since all member stars lie at essentially the same distance, unlike th… view at source ↗
Figure 5
Figure 5. Figure 5: Maximum sPSD (left-hand panels) and pfinal (right-hand panels) to which the predictions asymptote as more stars are included in the combination, plotted as a function of the central temperature of each bin. Predictions are shown for observations of length T = 2, 4 and 8 yr. Colours denote different values of the amplitude exponent s, and are as per previous figures, i.e., s = 1.2 in blue, s = 1.3 in orange… view at source ↗
Figure 6
Figure 6. Figure 6: Artificial PLATO spectra for the 4300 ≤ Teff < 4700 K temperature bin, calculated assuming s = 1.2 and observation lengths of T = 2 yr (top panels), and T = 4 yr (bottom panels). The left-hand panels show the combined, weighted spectra for all 357 stars in this bin (rendered in grey), after applying a 5 µHz boxcar to smooth the spectrum. The orange lines correspond to the underlying combined limit spectrum… view at source ↗
read the original abstract

Solar-like oscillations have to date been observed in hundreds of main-sequence and sub-giant stars. However, only a handful of detections have been made in K-type dwarfs, using ground-based extreme precision radial velocity observations and space-based photometric observations made by the NASA \emph{Kepler} and TESS missions. Whilst the upcoming ESA PLATO Mission promises to add to these individual detections, it will do so only in a similar, modest number of stars. Here, we propose a new ensemble strategy to exploit the PLATO data, in which frequency power spectra on hundreds of K-dwarfs lying in constrained ranges of effective temperature are combined in a weighted manner to significantly improve the detectability of the oscillations. Whilst this approach means it is not possible to extract usable constraints on individual oscillation frequencies, it provides a way to detect and measure the characteristics of the composite envelope of oscillation power given by the ensemble, which in turn provides diagnostics of granulation and magneto-convection and the impact of magnetic activity on the modes. We use data in the PLATO Input Catalogue (PIC) to make discrete numerical predictions of the detectability of the ensemble spectra. We also derive a simple analytical approximation of our method that obviates the need to perform numerical calculations over a discrete sample of targets, and which serves as a useful tool to make quick predictions for other future or planned missions. Our predictions indicate that PLATO has the potential to provide solid ensemble detections well into the K-dwarf regime. In summary, PLATO offers an ideal opportunity to exploit this new approach.

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

3 major / 2 minor

Summary. The paper proposes an ensemble asteroseismology strategy for detecting solar-like oscillations in K-dwarfs by weighted stacking of frequency power spectra from hundreds of stars in constrained effective-temperature ranges, using PLATO data. It derives numerical detectability predictions from the PLATO Input Catalogue and a simple analytical approximation of the method, concluding that PLATO can yield solid ensemble detections of composite oscillation power envelopes well into the K-dwarf regime, enabling diagnostics of granulation, magneto-convection, and magnetic activity effects.

Significance. If the central assumptions hold, the approach would extend asteroseismic diagnostics to a regime where individual detections remain modest even with PLATO, providing ensemble-level constraints on oscillation envelopes that are otherwise inaccessible. The analytical approximation is a practical strength for rapid mission planning.

major comments (3)
  1. [Abstract] Abstract (paragraph on ensemble strategy): the claim that weighted stacking of spectra from K-dwarfs in constrained Teff ranges yields detectable composite signals rests on the untested assumption that nu_max, envelope width, and amplitude are sufficiently similar within bins; no quantitative tolerance on scatter (e.g., 10-15% in nu_max) or Monte-Carlo validation against Kepler K-dwarf properties is supplied, leaving the detectability predictions vulnerable to dilution.
  2. [Analytical approximation] Section describing the analytical approximation: the derivation assumes identical power envelopes across the ensemble; it is not shown to remain valid when realistic variations in envelope shape (due to activity or metallicity) are introduced, which directly affects the claimed PLATO detectability threshold.
  3. [Numerical predictions] Section on numerical predictions from PIC: the discrete sample predictions lack any cross-check against real Kepler or TESS K-dwarf power spectra to confirm that the weighting scheme preserves signal amplitude rather than smearing it below threshold.
minor comments (2)
  1. [Abstract] Clarify the exact definition of 'constrained ranges of effective temperature' with explicit bin widths and selection criteria.
  2. Add a reference to prior ensemble methods in red giants or subgiants for context on the novelty of the K-dwarf application.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We are grateful to the referee for their detailed and constructive feedback on our manuscript. We have carefully considered each major comment and outline our responses below, along with proposed revisions to the manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract (paragraph on ensemble strategy): the claim that weighted stacking of spectra from K-dwarfs in constrained Teff ranges yields detectable composite signals rests on the untested assumption that nu_max, envelope width, and amplitude are sufficiently similar within bins; no quantitative tolerance on scatter (e.g., 10-15% in nu_max) or Monte-Carlo validation against Kepler K-dwarf properties is supplied, leaving the detectability predictions vulnerable to dilution.

    Authors: We agree that a quantitative assessment of the impact of scatter within the Teff bins is necessary to support the claims. In the revised manuscript, we will include Monte-Carlo simulations drawing from observed Kepler K-dwarf properties to determine the tolerance on variations in nu_max, envelope width, and amplitude (targeting 10-15% scatter) and demonstrate that the stacked signal remains above the detection threshold. This will strengthen the abstract's claims. revision: yes

  2. Referee: [Analytical approximation] Section describing the analytical approximation: the derivation assumes identical power envelopes across the ensemble; it is not shown to remain valid when realistic variations in envelope shape (due to activity or metallicity) are introduced, which directly affects the claimed PLATO detectability threshold.

    Authors: The analytical approximation is presented as a simplified model for rapid predictions. We acknowledge that its validity under realistic variations should be tested. We will add a subsection in the revised version that introduces perturbations to the envelope shapes based on activity levels and metallicity differences, showing that the approximation remains a useful estimator within acceptable error margins for mission planning purposes. revision: yes

  3. Referee: [Numerical predictions] Section on numerical predictions from PIC: the discrete sample predictions lack any cross-check against real Kepler or TESS K-dwarf power spectra to confirm that the weighting scheme preserves signal amplitude rather than smearing it below threshold.

    Authors: We recognize the value of validating the weighting scheme against existing data. Although the predictions are derived from the PLATO Input Catalogue, we will incorporate a cross-validation using simulated power spectra modeled after Kepler K-dwarfs to verify that the weighted stacking preserves the composite signal amplitude. This will be added to the numerical predictions section. revision: yes

Circularity Check

0 steps flagged

No significant circularity; predictions use external PIC data and independent analytical derivation

full rationale

The paper's detectability predictions are computed numerically from the external PLATO Input Catalogue (PIC) and via a newly derived analytical approximation. No load-bearing step reduces by construction to a fitted parameter, self-citation chain, or redefinition of inputs. The ensemble-stacking assumption (similar envelopes within Teff bins) is stated as a premise rather than derived from the paper's own outputs. This satisfies the criterion of a self-contained analysis against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The proposal rests on the domain assumption that oscillation properties are uniform enough within narrow Teff bins for stacking to succeed; the PLATO Input Catalogue supplies the input stellar parameters.

axioms (1)
  • domain assumption Solar-like oscillations exist in K-dwarfs and share similar power-envelope characteristics within constrained effective-temperature ranges.
    Invoked to justify that weighted averaging will produce a detectable composite signal rather than noise.

pith-pipeline@v0.9.0 · 5848 in / 1301 out tokens · 33098 ms · 2026-05-25T03:02:01.068420+00:00 · methodology

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Reference graph

Works this paper leans on

51 extracted references · 51 canonical work pages · 23 internal anchors

  1. [1]

    Predicting the detectability of oscillations in solar-type stars observed by Kepler

    Predicting the Detectability of Oscillations in Solar-type Stars Observed by Kepler. , keywords =. doi:10.1088/0004-637X/732/1/54 , archivePrefix =. 1103.0702 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/732/1/54

  2. [2]

    , keywords =

    Predicted asteroseismic detection yield for solar-like oscillating stars with PLATO. , keywords =. doi:10.1051/0004-6361/202348111 , archivePrefix =. 2401.07984 , primaryClass =

    work page doi:10.1051/0004-6361/202348111

  3. [3]

    The Asteroseismic Target List (ATL) for solar-like oscillators observed in 2-minute cadence with the Transiting Exoplanet Survey Satellite (TESS)

    The Asteroseismic Target List for Solar-like Oscillators Observed in 2 minute Cadence with the Transiting Exoplanet Survey Satellite. , keywords =. doi:10.3847/1538-4365/ab04f5 , archivePrefix =. 1901.10148 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ab04f5 1901

  4. [4]

    The asteroseismic potential of TESS: exoplanet-host stars

    The Asteroseismic Potential of TESS: Exoplanet-host Stars. , keywords =. doi:10.3847/0004-637X/830/2/138 , archivePrefix =. 1608.01138 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/830/2/138

  5. [5]

    Asteroseismic Data Analysis: Foundations and Techniques

    work page

  6. [6]

    , keywords =

    Low-amplitude Solar-like Oscillations in the K5 V Star ϵ Indi A. , keywords =. doi:10.3847/1538-4357/ad25f2 , archivePrefix =. 2403.04509 , primaryClass =

    work page doi:10.3847/1538-4357/ad25f2

  7. [7]

    Detection of solar-like oscillations in the K5 dwarf ϵ Indi

    Expanding the frontiers of cool-dwarf asteroseismology with ESPRESSO. Detection of solar-like oscillations in the K5 dwarf ϵ Indi. , keywords =. doi:10.1051/0004-6361/202449197 , archivePrefix =. 2403.16333 , primaryClass =

    work page doi:10.1051/0004-6361/202449197

  8. [8]

    The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc. , keywords =. doi:10.3847/1538-3881/ab05dc , archivePrefix =. 1901.06364 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/ab05dc 1901

  9. [9]

    The Solar Neighborhood. I. Standard Spectral Types (K5-M8) for Northern Dwarfs Within Eight Parsecs. , keywords =. doi:10.1086/117167 , adsurl =

    work page doi:10.1086/117167

  10. [10]

    The Solar Neighborhood XLIV: RECONS Discoveries within 10 Parsecs

    The Solar Neighborhood XLIV: RECONS Discoveries within 10 parsecs. , keywords =. doi:10.3847/1538-3881/aac262 , archivePrefix =. 1804.07377 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aac262

  11. [11]

    , keywords =

    The Character of M Dwarfs. , keywords =. doi:10.1146/annurev-astro-052722-102740 , adsurl =

    work page doi:10.1146/annurev-astro-052722-102740

  12. [12]

    How to Constrain Your M Dwarf: measuring effective temperature, bolometric luminosity, mass, and radius

    How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius. , keywords =. doi:10.1088/0004-637X/804/1/64 , archivePrefix =. 1501.01635 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/804/1/64

  13. [13]

    On the use of empirical bolometric corrections for stars

    On the Use of Empirical Bolometric Corrections for Stars. , keywords =. doi:10.1088/0004-6256/140/5/1158 , archivePrefix =. 1008.3913 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/140/5/1158

  14. [14]

    Characterization of LOPS2, the first long-pointing field

    The PLATO field selection process: II. Characterization of LOPS2, the first long-pointing field. , keywords =. doi:10.1051/0004-6361/202452325 , archivePrefix =. 2501.07687 , primaryClass =

    work page doi:10.1051/0004-6361/202452325

  15. [15]

    The PLATO field selection process. I. Identification and content of the long-pointing fields. , keywords =. doi:10.1051/0004-6361/202142256 , archivePrefix =. 2110.13924 , primaryClass =

    work page doi:10.1051/0004-6361/202142256

  16. [16]

    , keywords =

    The all-sky PLATO input catalogue. , keywords =. doi:10.1051/0004-6361/202140717 , archivePrefix =. 2108.13712 , primaryClass =

    work page doi:10.1051/0004-6361/202140717

  17. [17]

    , year = 1968, month = feb, volume =

    Space Distribution and Luminosity Functions of Quasi-Stellar Radio Sources. , year = 1968, month = feb, volume =. doi:10.1086/149446 , adsurl =

    work page doi:10.1086/149446 1968

  18. [18]

    Experimental Astronomy , keywords =

    PLATO's signal and noise budget. Experimental Astronomy , keywords =. doi:10.1007/s10686-024-09948-6 , archivePrefix =. 2406.11556 , primaryClass =

    work page doi:10.1007/s10686-024-09948-6

  19. [19]

    A Homogeneous Catalog of Oscillating Solar-Type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity

    A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity. , keywords =. doi:10.3847/1538-3881/adf648 , archivePrefix =. 2503.15599 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/adf648

  20. [20]

    , keywords =

    Detections of solar-like oscillations in dwarfs and subgiants with Kepler DR25 short-cadence data. , keywords =. doi:10.1051/0004-6361/202141168 , archivePrefix =. 2109.14058 , primaryClass =

    work page doi:10.1051/0004-6361/202141168

  21. [21]

    Asteroseismic fundamental properties of solar-type stars observed by the NASA Kepler Mission

    Asteroseismic Fundamental Properties of Solar-type Stars Observed by the NASA Kepler Mission. , keywords =. doi:10.1088/0067-0049/210/1/1 , archivePrefix =. 1310.4001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/210/1/1

  22. [22]

    Ensemble Asteroseismology of Solar-Type Stars with the NASA Kepler Mission

    Ensemble Asteroseismology of Solar-Type Stars with the NASA Kepler Mission. Science , keywords =. doi:10.1126/science.1201827 , archivePrefix =. 1109.4723 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1201827

  23. [23]

    An ancient extrasolar system with five sub-Earth-size planets

    An Ancient Extrasolar System with Five Sub-Earth-size Planets. , keywords =. doi:10.1088/0004-637X/799/2/170 , archivePrefix =. 1501.06227 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/799/2/170

  24. [24]

    A sub-Mercury-sized exoplanet

    A sub-Mercury-sized exoplanet. , keywords =. doi:10.1038/nature11914 , archivePrefix =. 1305.5587 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature11914

  25. [25]

    Asteroseismic detections in naked-eye main-sequence and subgiant solar-like oscillators

    Luminaries in the sky: The TESS legacy sample of bright stars: I. Asteroseismic detections in naked-eye main-sequence and subgiant solar-like oscillators. , keywords =. doi:10.1051/0004-6361/202555485 , archivePrefix =. 2508.08699 , primaryClass =

    work page doi:10.1051/0004-6361/202555485

  26. [26]

    , keywords =

    Asteroseismology of the Nearby K Dwarf Draconis Using the Keck Planet Finder and TESS. , keywords =. doi:10.3847/1538-4357/ad76a9 , archivePrefix =. 2407.21234 , primaryClass =

    work page doi:10.3847/1538-4357/ad76a9

  27. [27]

    The connection between stellar granulation and oscillation as seen by the Kepler mission

    The connection between stellar granulation and oscillation as seen by the Kepler mission. , keywords =. doi:10.1051/0004-6361/201424313 , archivePrefix =. 1408.0817 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201424313

  28. [28]

    , 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

  29. [29]

    The Asteroseismic Potential of the NASA TESS satellite , author =

    work page

  30. [30]

    Summary of the content and survey properties

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    work page doi:10.1051/0004-6361/202243940

  31. [31]

    Planck-spectrum estimates

    Bolometric corrections of stellar oscillation mode amplitudes as observed by the PLATO mission: I. Planck-spectrum estimates. , keywords =. doi:10.1051/0004-6361/202558666 , archivePrefix =. 2603.12750 , primaryClass =

    work page doi:10.1051/0004-6361/202558666

  32. [32]

    Asteroseismic properties of solar-type stars observed with the NASA K2 mission: results from Campaigns 1-3 and prospects for future observations

    Asteroseismic Properties of Solar-type Stars Observed with the NASA K2 Mission: Results from Campaigns 1-3 and Prospects for Future Observations. , keywords =. doi:10.1088/1538-3873/128/970/124204 , archivePrefix =. 1608.07292 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/128/970/124204

  33. [33]

    Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters. , keywords =. doi:10.3847/1538-4357/835/2/172 , archivePrefix =. 1612.00436 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/835/2/172

  34. [34]

    , keywords =

    K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet Finder. , keywords =. doi:10.3847/1538-4357/adc737 , archivePrefix =. 2502.00971 , primaryClass =

    work page doi:10.3847/1538-4357/adc737

  35. [35]

    Amplitudes of stochastically excited oscillations in main-sequence stars

    Amplitudes of stochastically excited oscillations in main-sequence stars. , keywords =. doi:10.48550/arXiv.astro-ph/9909107 , archivePrefix =. astro-ph/9909107 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9909107

  36. [36]

    JA&A , keywords =

    Excitation of Solar-like Oscillations: From PMS to MS Stellar Models. JA&A , keywords =. doi:10.1007/BF02702325 , adsurl =

    work page doi:10.1007/bf02702325

  37. [37]

    Excitation of solar-like oscillations across the HR diagram

    Excitation of solar-like oscillations across the HR diagram. , keywords =. doi:10.1051/0004-6361:20041953 , archivePrefix =. astro-ph/0611762 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20041953

  38. [38]

    Amplitudes of Stellar Oscillations: The Implications for Asteroseismology

    Amplitudes of stellar oscillations: the implications for asteroseismology. , keywords =. doi:10.48550/arXiv.astro-ph/9403015 , archivePrefix =. astro-ph/9403015 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9403015

  39. [39]

    Experimental Astronomy , keywords =

    The PLATO mission. Experimental Astronomy , keywords =. doi:10.1007/s10686-025-09985-9 , archivePrefix =. 2406.05447 , primaryClass =

    work page doi:10.1007/s10686-025-09985-9

  40. [40]

    Kepler White Paper: Asteroseismology of Solar-Like Oscillators in a 2-Wheel Mission

    Kepler White Paper: Asteroseismology of Solar-Like Oscillators in a 2-Wheel Mission. arXiv e-prints , keywords =. doi:10.48550/arXiv.1309.0702 , archivePrefix =. 1309.0702 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1309.0702

  41. [41]

    Evidence for the impact of stellar activity on the detectability of solar-like oscillations observed by Kepler

    Evidence for the Impact of Stellar Activity on the Detectability of Solar-like Oscillations Observed by Kepler. , keywords =. doi:10.1088/2041-8205/732/1/L5 , archivePrefix =. 1103.5570 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/732/1/l5 2041

  42. [42]

    Frontiers in Astronomy and Space Sciences , keywords =

    Revisiting the impact of stellar magnetic activity on the detection of solar-like oscillations by Kepler. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2019.00046 , archivePrefix =. 1907.01415 , primaryClass =

    work page doi:10.3389/fspas.2019.00046 2019

  43. [43]

    Limits on surface gravities of Kepler planet-candidate host stars from non-detection of solar-like oscillations

    Limits on Surface Gravities of Kepler Planet-candidate Host Stars from Non-detection of Solar-like Oscillations. , keywords =. doi:10.1088/0004-637X/783/2/123 , archivePrefix =. 1401.6324 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/783/2/123

  44. [44]

    8th TESS/15th Kepler Asteroseismic Science Consortium Workshop , year = 2024, month = aug, eid =

    HAYDN High-precision AsteroseismologY of DeNse fields. 8th TESS/15th Kepler Asteroseismic Science Consortium Workshop , year = 2024, month = aug, eid =. doi:10.5281/zenodo.13696736 , adsurl =

    work page doi:10.5281/zenodo.13696736 2024

  45. [45]

    submitted to , keywords =

    EPRV Asteroseismology of the K dwarfs GJ 570 A and GJ 783 A\\ with ESPRESSO. submitted to , keywords =

    work page

  46. [46]

    , keywords =

    Selection and characterisation of the M dwarf targets in the PLATO Input Catalogue. , keywords =. doi:10.1051/0004-6361/202557757 , archivePrefix =. 2512.14593 , primaryClass =

    work page doi:10.1051/0004-6361/202557757

  47. [47]

    Asteroseismic diagrams from a survey of solar-like oscillations with Kepler

    Asteroseismic Diagrams from a Survey of Solar-like Oscillations with Kepler. , keywords =. doi:10.1088/2041-8205/742/1/L3 , archivePrefix =. 1110.1375 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/742/1/l3 2041

  48. [48]

    A synthetic sample of short-cadence solar-like oscillators for TESS

    A Synthetic Sample of Short-cadence Solar-like Oscillators for TESS. , keywords =. doi:10.3847/1538-4365/aaedbc , archivePrefix =. 1809.09108 , primaryClass =

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

  49. [49]

    , keywords =

    Determining the Inclination of the Rotation Axis of a Sun-like Star. , keywords =. doi:10.1086/374715 , adsurl =

    work page doi:10.1086/374715

  50. [50]

    Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-sequence Stars. , keywords =. doi:10.3847/1538-4365/ab3b56 , archivePrefix =. 1908.05222 , primaryClass =

    work page doi:10.3847/1538-4365/ab3b56 1908

  51. [51]

    , keywords =

    Modeling of Solar Oscillation Power Spectra. , keywords =. doi:10.1086/169452 , adsurl =

    work page doi:10.1086/169452