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arxiv: 1907.01415 · v1 · pith:C6JIBTRGnew · submitted 2019-07-02 · 🌌 astro-ph.SR

Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler

S. Mathur , R. A. Garcia , L. Bugnet , A. R. G. Santos , N. Santiago , P. G. Beck This is my paper

Pith reviewed 2026-05-25 10:40 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords solar-like oscillationsKepler missionmagnetic activitymain-sequence starsphotometric variabilitymode amplitudesstellar rotation
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The pith

Stars with a photometric activity index above 2,000 ppm have a 98.3 percent probability of showing no detectable solar-like oscillations.

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

The paper reanalyzes non-detections of solar-like oscillations in Kepler data using a clean sample of 1,014 main-sequence stars, excluding classical pulsators and red giants. It computes predicted mode amplitudes and identifies 323 stars where detections should have occurred, then measures rotation periods and a photometric magnetic activity index for 684 stars overall. Among the 323, magnetic activity stronger than the Sun at maximum explains the absence in 32 percent of cases. For the remaining 68 percent, the analysis points to low metallicity as a possible suppressor while finding no clear link to inclination or binarity. The work also establishes a 20-30 ppm lower limit below which the activity index does not reliably detect rotation.

Core claim

In the cleaned sample, stars whose predicted mode amplitudes exceed the detection threshold show an amplitude-to-noise ratio above 0.94 when oscillations are seen. Of the 323 such stars with reliable rotation periods, 32 percent have activity levels exceeding solar maximum and therefore lack detectable p-modes. Magnetic activity cannot account for the non-detections in the other 68 percent. Spectroscopic checks on a subsample suggest low metallicity may reduce mode amplitudes. Stars whose photometric activity index exceeds 2,000 ppm have a 98.3 percent probability of non-detection.

What carries the argument

The photometric magnetic activity index, derived from measured rotation periods and light-curve variability, used to test correlation with predicted versus observed mode amplitudes.

If this is right

  • Magnetic activity above solar maximum accounts for non-detections in 32 percent of the 323 stars where modes were predicted to be visible.
  • A photometric activity index below 20-30 ppm marks the practical limit at which rotation and magnetic activity become undetectable in the light curves.
  • Low metallicity emerges as a candidate explanation for suppressed modes in the 68 percent of cases not explained by activity.
  • No systematic correlation appears between mode non-detection and either binary status or stellar inclination angle.

Where Pith is reading between the lines

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

  • Surveys could apply an activity-index threshold to deprioritize targets unlikely to yield oscillation detections.
  • The unexplained 68 percent of cases motivates refined models of how metallicity affects mode excitation or damping.
  • If low metallicity systematically reduces amplitudes, oscillation-based interior probes may be biased toward higher-metallicity solar analogs.

Load-bearing premise

The predicted mode amplitudes correctly identify the 323 stars in which oscillations should have been detectable without systematic bias from the amplitude formula or from how the main-sequence solar-like sample was defined.

What would settle it

Detection of solar-like oscillations in a statistically significant fraction of stars whose photometric activity index exceeds 2,000 ppm would falsify the claimed 98.3 percent non-detection probability.

Figures

Figures reproduced from arXiv: 1907.01415 by A. R. G. Santos, L. Bugnet, N. Santiago, P. G. Beck, R. A. Garcia, S. Mathur.

Figure 1
Figure 1. Figure 1: Hertzsprung-Russel Diagram for the different samples of stars mentioned in the paper. The grey circles represent KASC WG1 stars that were observed in short cadence during the survey phase. The red circles are the main-sequence stars with known oscillations from literature. The black circles correspond to the final set of 1,014 stars obtained as described in Section 2.2. The blue crosses are the new candida… view at source ↗
Figure 2
Figure 2. Figure 2: Ratio of the predicted maximum amplitude and the noise at high frequency as a function of the effective temperature (top panel) and as a function of surface gravity (bottom panel) for the stars without detected oscillations (black circles) and the stars with detected oscillations (red circles). Frontiers 21 [PITH_FULL_IMAGE:figures/full_fig_p021_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Hertzprung-Russel Diagram for the stars selected as described in Section 2.3, with Amax,pred/Noise > 0.94, Teff <6,800 K, and log g <4.3 dex. Stars without detected oscillations are represented with black circles and stars with detected oscillations in red circles. This is a provisional file, not the final typeset article 22 [PITH_FULL_IMAGE:figures/full_fig_p022_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: HR Diagram showing the hot dwarfs (red symbols), cool dwarfs (blue symbols), and subgiants (green symbols) as described in Section 4. Top panel: all the non oscillating stars with a measurement of rotation periods. Bottom panel: stars selected from the cut described in section 2.3 with a measurement of rotation period. Frontiers 23 [PITH_FULL_IMAGE:figures/full_fig_p023_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of the rotation periods for the full sample and the three categories of stars defined in Section 4: hot stars (left panel), cool dwarfs (middle panel), and subgiants (right panel). The black dash line in each panel represents the distribution for the full sample of stars with reliable rotation periods [PITH_FULL_IMAGE:figures/full_fig_p024_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of the < Sph > for the full sample and the three categories of stars as described in Section 4. Same legend as [PITH_FULL_IMAGE:figures/full_fig_p024_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Rotation distribution for the non-oscillating stars selected as in bottom panel of [PITH_FULL_IMAGE:figures/full_fig_p025_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Distribution of the < Sph > for the non-oscillating stars selected as in bottom panel of [PITH_FULL_IMAGE:figures/full_fig_p025_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Proxy of the magnetic activity, < Sph > as a function of the rotation period Prot for the full sample. The black symbols represent the non-oscillating stars while the red symbols represent the stars with detected oscillations from Garc´ıa et al. (2014). The dash lines are the < Sph > values at minimum and maximum activity of the Sun [PITH_FULL_IMAGE:figures/full_fig_p026_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p026_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Same as [PITH_FULL_IMAGE:figures/full_fig_p027_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Same as [PITH_FULL_IMAGE:figures/full_fig_p028_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: < Sph > as a function of the effective temperature from the DR25 stellar properties catalog. Same legend as [PITH_FULL_IMAGE:figures/full_fig_p029_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Histogram of metallicity for the non-oscillating stars using APOGEE DR14 for 158 stars (top) and LAMOST DR2 for 326 stars (bottom panel). The full sample in each panel is represented with the black solid line. Blue dot-dash line corresponds to the least active stars (Sph < Sph, ,max) while red dash line corresponds to the most active stars ( Sph > Sph, ,max). This is a provisional file, not the final type… view at source ↗
Figure 15
Figure 15. Figure 15: Distribution of inclination angles for stars with v sin i from APOGEE for stars with Amax,pred/Noise > 0.94. The red dash line represents the least active stars ( < Sph >< Sph, ,max ) while the blue dot-dash line represents the least active stars with a super-solar metallicity. Frontiers 31 [PITH_FULL_IMAGE:figures/full_fig_p031_15.png] view at source ↗
read the original abstract

Over 2,000 stars were observed for one month with a high enough cadence in order to look for acoustic modes during the survey phase of the Kepler mission. Solar-like oscillations have been detected in about 540 stars. The question of why no oscillations were detected in the remaining stars is still open. Previous works explained the non-detection of modes with the high level of magnetic activity. However, the studied stars contained some classical pulsators and red giants that could have biased the results. In this work, we revisit this analysis on a cleaner sample of 1,014 main-sequence solar-like stars. First we compute the predicted amplitude of the modes. We find that the stars with detected modes have an amplitude to noise ratio larger than 0.94. We measure reliable rotation periods and the associated photometric magnetic index for 684 stars and in particular for 323 stars where the mode amplitude is predicted to be high enough to be detected. We find that among these 323 stars 32% have a magnetic activity level larger than the Sun at maximum activity, explaining the non-detection of p modes. Interestingly, magnetic activity cannot be the primary reason responsible for the absence of detectable modes in the remaining 68% of the stars without p modes detected and with reliable rotation periods. Thus, we investigate metallicity, inclination angle, and binarity as possible causes of low mode amplitudes. Using spectroscopic observations for a subsample, we find that a low metallicity could be the reason for suppressed modes. No clear correlation with binarity nor inclination is found. We also derive the lower limit for our photometric activity index (of 20-30 ppm) below which rotation and magnetic activity are not detected. Finally with our analysis we conclude that stars with a photometric activity index larger than 2,000 ppm have 98.3% probability of not having oscillations detected.

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

2 major / 2 minor

Summary. The paper analyzes Kepler survey-phase observations of over 2000 stars to explain the non-detection of solar-like oscillations in the majority of cases. Using a cleaned sample of 1014 main-sequence solar-like stars, the authors compute predicted mode amplitudes via scaling relations, establish an empirical detection threshold of amplitude-to-noise ratio >0.94, derive rotation periods and a photometric magnetic activity index for 684 stars (including 323 with predicted detectable amplitudes), and conclude that activity levels exceeding the Sun at maximum (photometric index >2000 ppm) account for non-detections in 32% of the 323 stars while reporting a 98.3% probability of non-detection for stars above this activity threshold; the remaining 68% are attributed to factors such as low metallicity based on a spectroscopic subsample, with no clear role for inclination or binarity.

Significance. If the amplitude predictions hold without systematic bias, the work delivers a quantitative empirical constraint on activity suppression of p-modes that is directly useful for asteroseismic target selection and for interpreting non-detections in large surveys. The adoption of a strictly main-sequence solar-like sample removes contamination from classical pulsators and red giants that affected earlier studies, and the direct count yielding the 98.3% probability constitutes a falsifiable, parameter-light result.

major comments (2)
  1. [section computing predicted mode amplitudes and selection of the 323 stars] The attribution of non-detections to magnetic activity in 32% of the 323 stars (and the associated 98.3% probability statement) rests on the assumption that the predicted amplitudes correctly flag these stars as detectable in the absence of activity. The scaling relations for mode amplitudes and the definition of the main-sequence solar-like sample are not shown to be free of systematic offsets with metallicity or evolutionary state; a sensitivity test or comparison against an independent amplitude estimator is required to confirm that the high-activity subset is not preferentially misclassified.
  2. [section on measurement of rotation periods and photometric magnetic index] The photometric magnetic activity index threshold of 2000 ppm is presented as corresponding to the Sun at maximum activity, yet the precise calibration of this index against solar values, its uncertainty, and any post-selection cuts applied to the 684 stars with measured rotation periods are not detailed; this directly affects the robustness of the 98.3% probability quoted in the abstract and conclusion.
minor comments (2)
  1. [final analysis section] The lower limit of 20-30 ppm for the photometric activity index below which rotation and activity are undetectable should be shown with an explicit figure or table relating it to the noise properties of the Kepler light curves.
  2. [conclusions] Clarify whether the 98.3% probability is computed over the full 1014-star sample or restricted to the 323 stars with predicted detectable amplitudes, and state the exact denominator and numerator.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough and constructive review. The comments highlight important points regarding the robustness of our conclusions, and we address each major comment below. We will revise the manuscript to incorporate additional details and tests as outlined.

read point-by-point responses

  1. Referee: [section computing predicted mode amplitudes and selection of the 323 stars] The attribution of non-detections to magnetic activity in 32% of the 323 stars (and the associated 98.3% probability statement) rests on the assumption that the predicted amplitudes correctly flag these stars as detectable in the absence of activity. The scaling relations for mode amplitudes and the definition of the main-sequence solar-like sample are not shown to be free of systematic offsets with metallicity or evolutionary state; a sensitivity test or comparison against an independent amplitude estimator is required to confirm that the high-activity subset is not preferentially misclassified.

    Authors: We agree that explicit validation against potential systematics in the amplitude scaling relations would strengthen the attribution of the 32% fraction and the associated probability. In the revised manuscript we will add a sensitivity analysis in which the predicted amplitudes are perturbed by amounts representative of known uncertainties arising from metallicity and evolutionary state (drawing on published assessments of the scaling relations). We will also perform a limited comparison against an independent amplitude estimator for the spectroscopic subsample. These additions will confirm that the high-activity subset is not preferentially misclassified and will support the robustness of the quoted statistics. revision: yes

  2. Referee: [section on measurement of rotation periods and photometric magnetic index] The photometric magnetic activity index threshold of 2000 ppm is presented as corresponding to the Sun at maximum activity, yet the precise calibration of this index against solar values, its uncertainty, and any post-selection cuts applied to the 684 stars with measured rotation periods are not detailed; this directly affects the robustness of the 98.3% probability quoted in the abstract and conclusion.

    Authors: We thank the referee for noting the need for greater transparency on the activity-index calibration. The 2000 ppm value is obtained by applying the identical photometric index definition to solar observations at activity maximum. In the revised manuscript we will expand the relevant methods section to describe the solar calibration data set, the resulting uncertainty on the threshold, and the precise post-selection criteria applied to the 684 stars (including the 20-30 ppm lower limit for reliable rotation detection already mentioned in the text). This expanded description will directly underpin the robustness of the 98.3% probability. revision: yes

Circularity Check

0 steps flagged

No significant circularity; empirical counts after independent threshold

full rationale

The paper computes predicted mode amplitudes via scaling relations, determines an amplitude-to-noise threshold of 0.94 as the minimum observed among detected stars, and applies it to identify the 323-star subset. The central claim (98.3% non-detection probability for activity index >2000 ppm) is a direct empirical count over stars with measured rotation periods and activity indices versus detection status. No equation or step reduces this probability to a fitted parameter defined from the same data by construction, nor does any self-citation chain or ansatz make the result tautological. The derivation remains self-contained against the observed sample.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claims rest on standard stellar oscillation theory and Kepler photometry reduction; the two numerical thresholds (0.94 amplitude-to-noise and 2000 ppm activity index) are data-derived cutoffs rather than free parameters fitted to the target result.

free parameters (2)
  • amplitude-to-noise detection threshold = 0.94
    Value of 0.94 chosen because all detected-mode stars exceed it; used to define the 323-star subset.
  • photometric activity index threshold = 2000 ppm
    Value of 2000 ppm chosen because it yields the stated 98.3% probability of non-detection.
axioms (1)
  • domain assumption Predicted mode amplitudes computed from stellar parameters accurately forecast detectability in main-sequence solar-like stars.
    Invoked to isolate the 323 stars where non-detection must be explained by activity or other factors.

pith-pipeline@v0.9.0 · 5899 in / 1401 out tokens · 35856 ms · 2026-05-25T10:40:29.012098+00:00 · methodology

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