Pith. sign in

REVIEW 3 major objections 6 minor 87 references

Analyses of features of magnetic cycles at different amounts of dynamo supercriticality: Solar dynamo is about two times critical

T0 review · 3 major / 6 minor · reviewed 2026-08-10 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Sun's magnetic dynamo runs only about twice past its critical threshold

desk verdict A plausible but not tightly pinned-down estimate that the solar dynamo is about two times critical, supported by multi-model consistency but limited by single runs and fixed noise levels. read the letter →

arxiv 2501.02262 v1 pith:KAC5BNXQ submitted 2025-01-04 astro-ph.SR physics.plasm-phphysics.space-ph

Sanket Wavhal , Pawan Kumar , Bidya Binay Karak This is my paper · ORCID
classification astro-ph.SRphysics.plasm-phphysics.space-ph
keywords solardynamosupercriticalityBabcock-LeightongrandminimaMaunderminimumcyclevariabilityalpha-effectfluctuations
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper asks how far the Sun's large-scale magnetic-field generator sits above the threshold needed for dynamo action, and it argues the answer is about a factor of two in the dynamo's driving strength. Using five Babcock-Leighton type models run at two, four, and eight times the critical α, it compares model cycles with observed behavior. The strongest evidence is the gradual recovery from the Maunder minimum and the counts and durations of grand minima and maxima over 11,000-year simulations, both of which favor the weakly supercritical case. If the conclusion holds, the Sun operates close to the transition where magnetic activity can shut down, which would explain why grand minima occur as often as they do.

What carries the argument

The quantity that carries the argument is $\hat{\alpha}_0 = \alpha_0/\alpha_0^{\rm crit}$, the amplitude of the Babcock-Leighton α effect normalized by the value at which each model first sustains a growing magnetic field. The models are axisymmetric flux-transport dynamos (Models I-III) and truncated time-delay dynamos (Models IV-V), all kinematic with prescribed nonlinear quenching and stochastic fluctuations in the α source. Each model is run at $\hat{\alpha}_0 = 2, 4, 8$ for 11,000 years, and the resulting cycle statistics are compared with reconstructed solar activity and with the observed recovery slope after the Maunder minimum. This comparison is what lets the authors translate cycle statistics into a statement about how far the Sun is from the dynamo threshold.

What would settle it

Measure the rise slope of every well-resolved grand-minimum recovery in the 11,000-year cosmogenic record and compare the distribution with the model slopes at $\hat{\alpha}_0=2,4,8$; a distribution centered above the $\hat{\alpha}_0=2$ predictions would falsify the claim.

Watch

Extended reading notes

Core claim

The central claim is that the solar dynamo's supercriticality, measured by $\hat{\alpha}_0 = \alpha_0/\alpha_0^{\rm crit}$, is only about 2 rather than a large value. In all four models that were tested for recovery, the rise of sunspot number after an imposed Maunder-like suppression matches the observed 1700-1730 recovery only at $\hat{\alpha}_0 = 2$; at higher values the model rebounds too quickly. The 11,000-year simulations also produce roughly the observed number of grand minima (27) and maxima (23) only near $\hat{\alpha}_0 = 2$, while higher supercriticality makes deep minima rarer and shorter. The paper also argues that the observed weak correlation between polar-field proxies and the amplitude of cycles two and three ahead, and the Gnevyshev-Ohl pairing statistics, are compatible with a two-times-critical dynamo rather than contradicting it.

Load-bearing premise

The inference assumes the Sun's fluctuation level in the α (poloidal-source) effect is the same as the fixed values inherited from earlier calibrations; if the real fluctuation amplitude differs, the inferred supercriticality of about two would shift.

Editorial extensions

If this is right

  • The Sun's dynamo is only weakly supercritical, so a modest further decline in rotation with age could push it below the threshold and end large-scale magnetic activity.
  • Grand minima like the Maunder minimum should be comparatively frequent and long at $\hat{\alpha}_0 \approx 2$, consistent with the historical record.
  • Recovery from any future deep minimum should be gradual, taking roughly 30 years, as in the 1700-1730 recovery.
  • Polar-field memory in the dynamo should extend only weakly beyond one cycle, so cycle prediction based on the polar field at minimum should not expect strong skill two or three cycles ahead.
  • The Gnevyshev-Ohl even-odd pattern should continue to hold with occasional violations, matching the observed pairing statistics.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Editorial inference: if $\hat{\alpha}_0 \approx 2$ is robust, stellar samples should show a relatively sharp drop in magnetic activity as rotation slows past the equivalent threshold, and stars slightly above it should show frequent Maunder-like minima.
  • Editorial inference: the paper's noise amplitudes are fixed; a testable extension would vary the fluctuation level jointly with $\hat{\alpha}_0$ to map the degeneracy and see whether the inferred factor of two broadens.
  • Editorial inference: the same comparison could be applied to the historical cosmogenic isotope records of other Sun-like stars once their dynamo numbers are constrained, offering a stellar check on weakly supercritical operation.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. The paper estimates the solar dynamo's supercriticality, defined as alpha_hat = alpha0 / alpha0_crit, by running five Babcock-Leighton type kinematic dynamo models (flux transport and time-delay variants) at alpha_hat = 2, 4, and 8 with fixed stochastic fluctuation amplitudes. It compares three diagnostics against observations: the recovery rate from a Maunder-like grand minimum, the number and duration of grand minima and maxima in 11,000-year simulations, and consistency checks using polar-field memory correlations and the Gnevyshev-Ohl rule. The authors conclude that the solar dynamo is only about two times critical. The manuscript is clearly written and makes an interesting, observationally grounded claim, but the central inference currently rests on statistical and degeneracy assumptions that are not fully addressed.

Significance. If correct, the conclusion that the solar dynamo operates at roughly twice the critical dynamo threshold would support a weakly supercritical regime consistent with frequent grand minima and gradual Maunder recovery, with implications for stellar activity evolution and gyrochronology. The study's strengths include the use of multiple independent dynamo models, long 11,000-year simulations comparable to cosmogenic reconstructions, and explicit matching to observed grand-minima counts. The authors also acknowledge kinematic limitations and their results align with several previous independent estimates. However, the significance is currently limited by the absence of ensemble statistics and by the fixed noise amplitudes inherited from prior calibrations, which are degenerate with supercriticality in controlling rare-event statistics.

major comments (3)
  1. [Section 3.2, Table 1] The central statistical comparison uses a single 11,000-year realization per (model, alpha_hat) cell, with no ensemble spread or error bars. For counting statistics, Poisson fluctuations of sqrt(N) are roughly 4-5 events, which is comparable to the differences between alpha_hat = 2 and alpha_hat = 4 in several models (e.g., Model I: 20 vs 8; Model II: 18 vs 8; Model III: 16 vs 9). Without multiple realizations or a properly propagated uncertainty estimate, the claim that alpha_hat = 2 is statistically preferred over alpha_hat = 4 is not supported by the presented data. This is a load-bearing issue for the main conclusion.
  2. [Section 2.1 and Table 1] The fluctuation amplitudes of the alpha effect are fixed at values inherited from previous calibrations (e.g., Gaussian sigma = 2.67 for Models I and II; 200%, 100%, and 70% uniform fluctuations for Models III, IV, and V) and are never varied. Grand-minima statistics depend jointly on supercriticality and noise amplitude, so the observed 27 grand minima in 11,000 years could plausibly be reproduced at alpha_hat = 4 with a somewhat lower noise level than assumed. Because the paper does not explore this degeneracy, the inference 'alpha_hat = 2' is not uniquely identified by the statistics. The sentence in Section 3, 'for each model, the level of fluctuations in alpha remains the same,' confirms the fixed-noise assumption but does not justify it for the supercriticality sweep.
  3. [Section 3.1, Figures 1-2] The Maunder-minimum recovery comparison is qualitative and based on a single observed event and a single imposed initial perturbation (multiplying the polar field by gamma_p = 0.1). No quantitative goodness-of-fit measure is given, the sensitivity to gamma_p is not explored, and the results for Models II, III, and IV are only asserted in the text with no figures or numerical values. The exclusion of Model V is explained, but the overall constraint from this diagnostic is weak and should be framed accordingly.
minor comments (6)
  1. [Section 3.1] The text states 'the robust result in all four models (I–VI)' — the parenthetical appears to be a typo for 'I–IV' (or 'I–V' with V excluded), and should be corrected.
  2. [Section 3.2] The phrase 'namely, Models III-VI' should read 'Models III-V', since only five models are used in total.
  3. [Table 2 and Section 3.2] For the time-delay models (IV and V), durations in Table 2 are not reported because the time unit is dimensionless; this makes comparison with the flux-transport models and observations difficult. A conversion or a clear statement of the cycle-length normalization would improve readability.
  4. [Section 3.3.1, Table 3] The correlation coefficients for Models I and II in Table 3 are taken from Kumar, Karak, and Vashishth (2021) at alpha_hat = 2 and are not computed in the present study; this should be stated in the table caption to avoid implying new calculations.
  5. [Section 3.3.2 and Figure 6] The Gnevyshev-Ohl comparison is based on Model IV alone and on observed data with large reconstruction uncertainties; the authors correctly note that the comparison is not robust. This section is appropriately cautious, but the caveat should also appear in the Conclusions where the GO rule is listed as a supporting feature.
  6. [Abstract and Introduction] The abstract contains a grammatical error: 'with that of observations and we show' should be 'with observations, we show'. Also, Eq. (1) defines the dynamo number D, but subsequent analysis uses alpha_hat = alpha0/alpha0_crit; the relationship between these two measures should be clarified earlier.

Circularity Check

1 steps flagged · score 4.0 of 10

The alpha_hat = 2 conclusion is partly degenerate with the fixed, previously calibrated alpha-fluctuation amplitude used to drive grand minima; other diagnostics are independent, so circularity is partial.

  1. fitted input called prediction [Section 1 (fluctuations explain grand minima), Section 2.1 (Gaussian sigma = 2.67), Section 3 and Section 3.2 / Table 1 (same fluctuation level for all alpha_hat0; grand-minima count comparison)]
    "These fluctuations in the Babcock–Leighton dynamo models explain majority of the irregular features of solar cycle, including long-term modulation and grand minima ... When we introduce fluctuations in these models, we multiply α0 by a Gaussian of unity mean and 2.67 standard deviation as inspired by the study of Olemskoy, Choudhuri, and Kitchatinov (2013) ... In our study, for each model, we perform a set of solar cycle simulations at ˆα0 = 2, 4, and 8, and for each model, the level of fluctuations in α remains the same."

    The central selection of alpha_hat = 2 rests on matching the 11,000-year grand-minima/maxima counts (observed 27/23) to models with fixed fluctuation amplitudes. But the grand-minima frequency is a joint function of supercriticality and noise amplitude, and the paper varies only alpha_hat while importing sigma from prior calibrations that, by the paper's own statement, were already used to reproduce 'long-term modulation and grand minima.' Thus the count comparison is not an independent test of supercriticality: a different sigma would shift the best-matching alpha_hat. The inference is partially degenerate with the inherited noise input, although the Maunder-recovery rate, duration statistics, and polar-field consistency checks provide separate evidence for weak supercriticality.

full rationale

The paper's main claim is that the solar dynamo is only about twice critical (alpha_hat = 2). The inference is drawn from several diagnostics, with the grand-minima/maxima counts in Section 3.2 acting as the strongest quantitative discriminator. Those counts are produced by models in which the stochastic alpha-fluctuation amplitude is a fixed input inherited from earlier studies, several by the same authors, and the paper explicitly states that these fluctuations were designed to explain 'long-term modulation and grand minima.' Consequently, the comparison of counts is partly circular: it constrains a combination of supercriticality and noise, not supercriticality alone. However, the paper also compares the Maunder-minimum recovery slope (Section 3.1) and grand-minima durations (Table 2), which are not governed by the same fitted noise parameter, and it uses the polar-field memory and Gnevyshev–Ohl assessments only as consistency checks. These independent diagnostics support the same conclusion, so the circularity is local to the count comparison and does not make the entire derivation tautological. The score of 4 reflects partial circularity of the central claim without full reduction by construction.

Assumptions & free parameters 8 free parameters · 5 assumptions · 0 invented entities

The central claim rests on model statistics that depend on inherited noise levels and on a single realization per parameter setting; the models themselves rely on the Babcock-Leighton paradigm and kinematic approximation.

free parameters (8)
  • Fluctuation amplitude of alpha effect (Models I and II) = Gaussian, sigma = 2.67
    Inherited from Olemskoy, Choudhuri, and Kitchatinov (2013); controls frequency of grand minima, which is the main diagnostic.
  • Fluctuation level (Model III) = 200% uniform
    From Passos et al. (2014); fixed across all supercriticality values.
  • Fluctuation level (Model IV) = 100% uniform
    From Hazra, Passos, and Nandy (2014); fixed across all supercriticality values.
  • Fluctuation level (Model V) = 70% uniform
    From Albert et al. (2021); fixed across all supercriticality values; produces chaotic solutions in some regimes.
  • Mean-field alpha amplitude (Model III) = alpha0MF = 0.4
    Fixed in Passos et al. (2014); contributes to recovery from grand minima.
  • Mean-field alpha amplitude (Model IV) = alpha_mf = 0.2
    Fixed in Hazra, Passos, and Nandy (2014); contributes to recovery from grand minima.
  • Polar-field suppression factor for Maunder recovery = gamma_p = 0.1
    Chosen by hand in Section 3.1 to mimic the Maunder minimum state; affects the recovery rate comparison.
  • Supercriticality grid = alpha_hat = 2, 4, 8
    Choice of discrete grid limits the precision of the inferred value to 'closer to 2 than 4 or 8'.
assumptions (5)
  • domain assumption The Babcock-Leighton mechanism, with observationally motivated fluctuations, is the dominant poloidal-field source for the solar dynamo.
    Adopted from prior literature; the entire model family rests on this mechanism (Sections 1 and 2.1).
  • domain assumption Kinematic dynamo models with prescribed nonlinear quenching capture the relevant dynamics for long-term cycle statistics.
    The paper uses kinematic models and states the nonlinearity is specified (Section 2 and Conclusion).
  • domain assumption The reconstructed grand-minima and maxima statistics from cosmogenic isotopes (27 minima, 23 maxima in 11,000 years) are accurate.
    Used as the observational benchmark in Section 3.2 and Table 1.
  • ad hoc to paper A single 11,000-year run per model and supercriticality is representative of the stochastic statistics.
    No ensemble or error bars are provided for the counts in Table 1; the comparison assumes convergence of the single realization.
  • ad hoc to paper The fluctuation amplitudes inherited from prior calibrations are applicable at all supercriticality values tested.
    The same noise level is used at alpha_hat = 2, 4, and 8, though the physical fluctuation level might depend on the dynamo regime.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Analyses of features of magnetic cycles at different amounts of dynamo supercriticality: Solar dynamo is about two times critical." pith.science (2026). https://pith.science/paper/KAC5BNXQ

@misc{pith2026250102262,
  author       = {Pith},
  title        = {Pith review of: Analyses of features of magnetic cycles at different amounts of dynamo supercriticality: Solar dynamo is about two times critical},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/KAC5BNXQ}},
  note         = {Machine review of arXiv:2501.02262}
}
read the original abstract

The growth of a large-scale magnetic field in the Sun and stars is usually possible when the dynamo number (D) is above a critical value Dc. As the star ages, its rotation rate and thus D decrease. Hence, the question is how far the solar dynamo is from the critical dynamo transition. To answer this question, we have performed a set of simulations using Babcock-Leighton type dynamo models at different values of dynamo supercriticality and analyzed various features of magnetic cycle. By comparing the recovery rates of the dynamo from the Maunder minimum and statistics (numbers and durations) of the grand minima and maxima with that of observations and we show that the solar dynamo is only about two times critical and thus not highly supercritical. The observed correlation between the polar field proxy and the following cycle amplitudes and Gnevyshev-Ohl rule are also compatible with this conclusion.

Figures

Figures reproduced from arXiv: 2501.02262 by the authors.

Figure 1
Figure 1. The plot depicting the comparison of recovery rates from Maunder minimum. The black line is the observational data of Maunder minimum (yearly mean group sunspot num￾ber available during 1610–2015 obtained from WDC-SILSO, Royal Observatory of Belgium, Brussels). The blue and red lines represent the model data at ˆα0 = 2, and ˆα0 = 4 from Model I [PITH_FULL_IMAGE:figures/full_fig_p008_1.png] view at source ↗
Figure 2
Figure 2. The plot compares the recovery rates from the Maunder Minimum. Black/triangles show the observed recovery rate, and blue/squares, red/circles, and dark magenta/asterisks (and connecting lines) represent model recovery rates at ˆα0 = 2, 4, and 8 respectively in Model I. SOLA: sola_example_6.tex; 7 January 2025; 1:22; p. 8 [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Temporal variation of the smoothed toroidal field of 11,000-year simulation of Model I. Blue-shaded regions below the horizontal blue line represent the grand minima, whereas red-shaded regions above the horizontal red line represent the grand maxima; (a) for ˆα0 = 2, and (b) for ˆα0 = 4. Insets show epochs around a grand minimum [PITH_FULL_IMAGE:figures/full_fig_p011_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Histograms for the durations of grand minima (a,b,c) and grand maxima (d, e, f) with increasing dynamo supercriticality ( ˆα0). SOLA: sola_example_6.tex; 7 January 2025; 1:22; p. 11 [PITH_FULL_IMAGE:figures/full_fig_p011_4.png]
Figure 5
Figure 5. Figure 5: Pearson Correlation coefficients between the polar flux at cycle n with the toroidal flux at cycle n+1 (blue/filled-circles), n+2 (red/squares), and n+3 (black/triangles) computed for a different number of cycles from Model II at ˆα0 = 2. The points show the average va…
Figure 6
Figure 6. Figure 6: PDF of the duration of the even-odd episodes measured at different values of ˆα0 from Model IV (time delay dynamo model). The observation PDF is computed using the last 10 cycles sunspot data and the reconstructed sunspot number of Usoskin et al. (2021) with error from…
Figure 7
Figure 7. Figure 7: (a): Red and blue curves show the α profile for non-local (for Models I and II), and local (Model III) prescription of Babcock–Leighton process. The black curve represents the mean-field α profile for Model III, as discussed in Section 2.1. (b) Variations of ηp (red) a…
Figure 8
Figure 8. Figure 8: Profiles of the α quenching function used in Models IV and V. Functions f0 and f1 correspond to Babcock–Leighton α (blue) and mean field α (red) used in Model IV. The quenching f ′ corresponds to Babcock–Leighton α in Model V is shown in black. Biswas, A., Karak, B.B.,…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

87 extracted references · 30 canonical work pages

  1. [1]

    , Ferriz-Mas , A

    barticle Albert , C. , Ferriz-Mas , A. , Gaia , F. , Ulzega , S. : 2021 , Can Stochastic Resonance Explain Recurrence of Grand Minima? 916 , L9 . https://doi.org/10.3847/2041-8213/ac0fd6 . 2021ApJ...916L...9A . barticle

    work page doi:10.3847/2041-8213/ac0fd6 2021

  2. [2]

    , Brun , A.S

    barticle Augustson , K. , Brun , A.S. , Miesch , M. , Toomre , J. : 2015 , Grand Minima and Equatorward Propagation in a Cycling Stellar Convective Dynamo . 809 , 149 . https://doi.org/10.1088/0004-637X/809/2/149 . 2015ApJ...809..149A . barticle

    doi:10.1088/0004-637x/809/2/149 2015

  3. [3]

    : 1961 , The Topology of the Sun's Magnetic Field and the 22-YEAR Cycle

    barticle Babcock , H.W. : 1961 , The Topology of the Sun's Magnetic Field and the 22-YEAR Cycle. 133 , 572 . https://doi.org/10.1086/147060 . 1961ApJ...133..572B . barticle

    doi:10.1086/147060 1961

  4. [4]

    , Nandy , D

    barticle Bhowmik , P. , Nandy , D. : 2018 , Prediction of the strength and timing of sunspot cycle 25 reveal decadal-scale space environmental conditions . Nature Communications 9 , 5209 . https://doi.org/10.1038/s41467-018-07690-0 . 2018NatCo...9.5209B . barticle

    doi:10.1038/s41467-018-07690-0 2018

  5. [5]

    , Karak , B.B

    barticle Biswas , A. , Karak , B.B. , Kumar , P. : 2023 , Exploring the reliability of polar field rise rate as a precursor for an early prediction of solar cycle . 526 , 3994 . https://doi.org/10.1093/mnras/stad2966 . 2023MNRAS.526.3994B . barticle

    work page doi:10.1093/mnras/stad2966 2023

  6. [6]

    , Karak , B.B

    barticle Biswas , A. , Karak , B.B. , Usoskin , I. , Weisshaar , E. : 2023 , Long-Term Modulation of Solar Cycles . 219 , 19 . https://doi.org/10.1007/s11214-023-00968-w . 2023SSRv..219...19B . barticle

    doi:10.1007/s11214-023-00968-w 2023

  7. [7]

    , Browning , M.K

    barticle Brun , A.S. , Browning , M.K. : 2017 , Magnetism, dynamo action and the solar-stellar connection . Living Reviews in Solar Physics 14 , 4 . https://doi.org/10.1007/s41116-017-0007-8 . 2017LRSP...14....4B . barticle

    doi:10.1007/s41116-017-0007-8 2017

  8. [8]

    , Miesch , M.S

    barticle Brun , A.S. , Miesch , M.S. , Toomre , J. : 2004 , Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope . 614 , 1073 . https://doi.org/10.1086/423835 . 2004ApJ...614.1073B . barticle

    doi:10.1086/423835 2004

Show all 87 references
  1. [9]

    , Strugarek , A

    barticle Brun , A.S. , Strugarek , A. , Varela , J. , Matt , S.P. , Augustson , K.C. , Emeriau , C. , DoCao , O.L. , Brown , B. , Toomre , J. : 2017 , On Differential Rotation and Overshooting in Solar-like Stars . 836 , 192 . https://doi.org/10.3847/1538-4357/aa5c40 . 2017ApJ...

    2017 doi

  2. [10]

    , Strugarek , A

    barticle Brun , A.S. , Strugarek , A. , Noraz , Q. , Perri , B. , Varela , J. , Augustson , K. , Charbonneau , P. , Toomre , J. : 2022 , Powering Stellar Magnetism: Energy Transfers in Cyclic Dynamos of Sun-like Stars . 926 , 21 . https://doi.org/10.3847/1538-4357/ac469b . 202...

    2022 doi

  3. [11]

    , Sch \"u ssler , M

    barticle Cameron , R. , Sch \"u ssler , M. : 2015 , The crucial role of surface magnetic fields for the solar dynamo . Science 347 , 1333 . https://doi.org/10.1126/science.1261470 . 2015Sci...347.1333C . barticle

    2015 doi

  4. [12]

    , Sch \"u ssler , M

    barticle Cameron , R.H. , Sch \"u ssler , M. : 2017 , Understanding Solar Cycle Variability . 843 , 111 . https://doi.org/10.3847/1538-4357/aa767a . 2017ApJ...843..111C . barticle

    2017 doi

  5. [13]

    , Sch \"u ssler , M

    barticle Cameron , R.H. , Sch \"u ssler , M. : 2019 , Solar activity: periodicities beyond 11 years are consistent with random forcing . 625 , A28 . https://doi.org/10.1051/0004-6361/201935290 . 2019A&A...625A..28C . barticle

    2019 doi

  6. [14]

    , Sch \"u ssler , M

    barticle Cameron , R.H. , Sch \"u ssler , M. : 2023 , Observationally Guided Models for the Solar Dynamo and the Role of the Surface Field . 219 , 60 . https://doi.org/10.1007/s11214-023-01004-7 . 2023SSRv..219...60C . barticle

    2023 doi

  7. [15]

    : 2020 , Dynamo models of the solar cycle

    barticle Charbonneau , P. : 2020 , Dynamo models of the solar cycle . Living Reviews in Solar Physics 17 , 4 . https://doi.org/10.1007/s41116-020-00025-6 . 2020LRSP...17....4C . barticle

    2020 doi

  8. [16]

    , Barlet , G

    barticle Charbonneau , P. , Barlet , G. : 2011 , The dynamo basis of solar cycle precursor schemes . Journal of Atmospheric and Solar-Terrestrial Physics 73 , 198 . https://doi.org/10.1016/j.jastp.2009.12.020 . 2011JASTP..73..198C . barticle

    2011 doi

  9. [17]

    , Dikpati , M

    barticle Charbonneau , P. , Dikpati , M. : 2000 , Stochastic Fluctuations in a Babcock-Leighton Model of the Solar Cycle . 543 , 1027 . https://doi.org/10.1086/317142 . 2000ApJ...543.1027C . barticle

    2000 doi

  10. [18]

    , Blais-Laurier , G

    barticle Charbonneau , P. , Blais-Laurier , G. , St-Jean , C. : 2004 , Intermittency and Phase Persistence in a Babcock-Leighton Model of the Solar Cycle . 616 , L183 . https://doi.org/10.1086/426897 . 2004ApJ...616L.183C . barticle

    2004 doi

  11. [19]

    , St-Jean , C

    barticle Charbonneau , P. , St-Jean , C. , Zacharias , P. : 2005 , Fluctuations in Babcock-Leighton Dynamos. I. Period Doubling and Transition to Chaos . 619 , 613 . https://doi.org/10.1086/426385 . 2005ApJ...619..613C . barticle

    2005 doi

  12. [20]

    , Nandy , D

    barticle Chatterjee , P. , Nandy , D. , Choudhuri , A.R. : 2004 , Full-sphere simulations of a circulation-dominated solar dynamo: Exploring the parity issue . 427 , 1019 . https://doi.org/10.1051/0004-6361:20041199 . 2004A\ barticle

    2004 doi

  13. [21]

    , Hazra , G

    barticle Choudhuri , A.R. , Hazra , G. : 2016 , The treatment of magnetic buoyancy in flux transport dynamo models . Advances in Space Research 58 , 1560 . https://doi.org/10.1016/j.asr.2016.03.015 . 2016AdSpR..58.1560C . barticle

    2016 doi

  14. [22]

    , Karak , B.B

    barticle Choudhuri , A.R. , Karak , B.B. : 2009 , A possible explanation of the Maunder minimum from a flux transport dynamo model . Res. Astron. Astrophys. 9 , 953 . https://doi.org/10.1088/1674-4527/9/9/001 . 2009RAA.....9..953C . barticle

    2009 doi

  15. [23]

    , Karak , B.B

    barticle Choudhuri , A.R. , Karak , B.B. : 2012 , Origin of Grand Minima in Sunspot Cycles . Phys. Rev. Lett. 109 , 171103 . barticle

    2012

  16. [24]

    , Chatterjee , P

    barticle Choudhuri , A.R. , Chatterjee , P. , Jiang , J. : 2007 , Predicting Solar Cycle 24 With a Solar Dynamo Model . Physical Review Letters 98 , 131103 . https://doi.org/10.1103/PhysRevLett.98.131103 . 2007PhRvL..98m1103C . barticle

    2007 doi

  17. [25]

    , Nandy , D

    barticle Choudhuri , A.R. , Nandy , D. , Chatterjee , P. : 2005 , Reply to the Comments of Dikpati et al. 437 , 703 . https://doi.org/10.1051/0004-6361:20052934 . 2005A&A...437..703C . barticle

    2005 doi

  18. [26]

    , Sch\"ussler , M

    barticle Choudhuri , A.R. , Sch\"ussler , M. , Dikpati , M. : 1995 , The solar dynamo with meridional circulation. 303 , L29 . 1995A\ barticle

    1995

  19. [27]

    , Solanki , S.K

    barticle Dasi-Espuig , M. , Solanki , S.K. , Krivova , N.A. , Cameron , R. , Pe \ n uela , T. : 2010 , Sunspot group tilt angles and the strength of the solar cycle . 518 , A7 . https://doi.org/10.1051/0004-6361/201014301 . 2010A\ barticle

    2010 doi

  20. [28]

    , Charbonneau , P

    barticle Dikpati , M. , Charbonneau , P. : 1999 , A Babcock-Leighton Flux Transport Dynamo with Solar-like Differential Rotation . 518 , 508 . https://doi.org/10.1086/307269 . 1999ApJ...518..508D . barticle

    1999 doi

  21. [29]

    : 1976 , The Maunder Minimum

    barticle Eddy , J.A. : 1976 , The Maunder Minimum . Science 192 , 1189 . https://doi.org/10.1126/science.192.4245.1189 . 1976Sci...192.1189E . barticle

    1976

  22. [30]

    , Fang , F

    barticle Fan , Y. , Fang , F. : 2014 , A Simulation of Convective Dynamo in the Solar Convective Envelope: Maintenance of the Solar-like Differential Rotation and Emerging Flux . 789 , 35 . https://doi.org/10.1088/0004-637X/789/1/35 . http://esoads.eso.org/abs/2014ApJ...789......

    2014 doi

  23. [31]

    , Karak , B.B

    botherref Garg , S. , Karak , B.B. , Egeland , R. , Soon , W. , Baliunas , S. : 2019, Waldmeier Effect in Stellar Cycles . arXiv e-prints, arXiv:1909.12148. 2019arXiv190912148G . botherref

    2019 arXiv

  24. [32]

    , Kumar , P

    barticle Ghosh , A. , Kumar , P. , Prasad , A. , Karak , B.B. : 2024 , Characterizing the Solar Cycle Variability Using Nonlinear Time Series Analysis at Different Amounts of Dynamo Supercriticality: Solar Dynamo is Not Highly Supercritical . 167 , 209 . https://doi.org/10.384...

    2024 doi

  25. [33]

    : 2015 , The Solar Cycle

    barticle Hathaway , D.H. : 2015 , The Solar Cycle . Living Reviews in Solar Physics 12 , 4 . https://doi.org/10.1007/lrsp-2015-4 . 2015LRSP...12....4H . barticle

    2015 doi

  26. [34]

    , Choudhuri , A.R

    barticle Hazra , G. , Choudhuri , A.R. : 2019 , A New Formula for Predicting Solar Cycles . 880 , 113 . https://doi.org/10.3847/1538-4357/ab2718 . 2019ApJ...880..113H . barticle

    2019 doi

  27. [35]

    , Nandy , D

    barticle Hazra , G. , Nandy , D. , Kitchatinov , L. , Choudhuri , A.R. : 2023 , Mean Field Models of Flux Transport Dynamo and Meridional Circulation in the Sun and Stars . 219 , 39 . https://doi.org/10.1007/s11214-023-00982-y . 2023SSRv..219...39H . barticle

    2023 doi

  28. [36]

    , Passos , D

    barticle Hazra , S. , Passos , D. , Nandy , D. : 2014 , A Stochastically Forced Time Delay Solar Dynamo Model: Self-consistent Recovery from a Maunder-like Grand Minimum Necessitates a Mean-field Alpha Effect . 789 , 5 . https://doi.org/10.1088/0004-637X/789/1/5 . 2014ApJ...78...

    2014 doi

  29. [37]

    , Kusano , K

    barticle Hotta , H. , Kusano , K. , Shimada , R. : 2022 , Generation of Solar-like Differential Rotation . 933 , 199 . https://doi.org/10.3847/1538-4357/ac7395 . 2022ApJ...933..199H . barticle

    2022 doi

  30. [38]

    , Karak , B.B

    barticle Jha , B.K. , Karak , B.B. , Mandal , S. , Banerjee , D. : 2020 , Magnetic Field Dependence of Bipolar Magnetic Region Tilts on the Sun: Indication of Tilt Quenching . 889 , L19 . https://doi.org/10.3847/2041-8213/ab665c . 2020ApJ...889L..19J . barticle

    2020 doi

  31. [39]

    , Cameron , R.H

    barticle Jiang , J. , Cameron , R.H. , Sch \"u ssler , M. : 2014 , Effects of the Scatter in Sunspot Group Tilt Angles on the Large-scale Magnetic Field at the Solar Surface . 791 , 5 . https://doi.org/10.1088/0004-637X/791/1/5 . 2014ApJ...791....5J . barticle

    2014 doi

  32. [40]

    a pyl \"a , M.J. , K \

    barticle K \"a pyl \"a , M.J. , K \"a pyl \"a , P.J. , Olspert , N. , Brandenburg , A. , Warnecke , J. , Karak , B.B. , Pelt , J. : 2016 , Multiple dynamo modes as a mechanism for long-term solar activity variations . 589 , A56 . https://doi.org/10.1051/0004-6361/201527002 . 2...

    2016 doi

  33. [41]

    , Browning , M.K

    barticle K \"a pyl \"a , P.J. , Browning , M.K. , Brun , A.S. , Guerrero , G. , Warnecke , J. : 2023 , Simulations of Solar and Stellar Dynamos and Their Theoretical Interpretation . 219 , 58 . https://doi.org/10.1007/s11214-023-01005-6 . 2023SSRv..219...58K . barticle

    2023 doi

  34. [42]

    : 2010 , Importance of Meridional Circulation in Flux Transport Dynamo: The Possibility of a Maunder-like Grand Minimum

    barticle Karak , B.B. : 2010 , Importance of Meridional Circulation in Flux Transport Dynamo: The Possibility of a Maunder-like Grand Minimum . 724 , 1021 . https://doi.org/10.1088/0004-637X/724/2/1021 . 2010ApJ...724.1021K . barticle

    2010 doi

  35. [43]

    : 2023 , Models for the long-term variations of solar activity

    barticle Karak , B.B. : 2023 , Models for the long-term variations of solar activity . Living Reviews in Solar Physics 20 , 3 . https://doi.org/10.1007/s41116-023-00037-y . 2023LRSP...20....3K . barticle

    2023 doi

  36. [44]

    , Choudhuri , A.R

    barticle Karak , B.B. , Choudhuri , A.R. : 2013 , Studies of grand minima in sunspot cycles by using a flux transport solar dynamo model . Res. Astron. Astrophys. 13 , 1339 . https://doi.org/10.1088/1674-4527/13/11/005 . 2013RAA....13.1339K . barticle

    2013 doi

  37. [45]

    , Miesch , M

    barticle Karak , B.B. , Miesch , M. : 2017 , Solar Cycle Variability Induced by Tilt Angle Scatter in a Babcock-Leighton Solar Dynamo Model . 847 , 69 . https://doi.org/10.3847/1538-4357/aa8636 . 2017ApJ...847...69K . barticle

    2017 doi

  38. [46]

    , Miesch , M

    barticle Karak , B.B. , Miesch , M. : 2018 , Recovery from Maunder-like Grand Minima in a Babcock--Leighton Solar Dynamo Model . 860 , L26 . https://doi.org/10.3847/2041-8213/aaca97 . 2018ApJ...860L..26K . barticle

    2018 doi

  39. [47]

    , Kitchatinov , L.L

    barticle Karak , B.B. , Kitchatinov , L.L. , Brandenburg , A. : 2015 , Hysteresis between Distinct Modes of Turbulent Dynamos . 803 , 95 . https://doi.org/10.1088/0004-637X/803/2/95 . http://esoads.eso.org/abs/2015ApJ...803...95K . barticle

    2015 doi

  40. [48]

    , Mandal , S

    barticle Karak , B.B. , Mandal , S. , Banerjee , D. : 2018 , Double Peaks of the Solar Cycle: An Explanation from a Dynamo Model . 866 , 17 . https://doi.org/10.3847/1538-4357/aada0d . 2018ApJ...866...17K . barticle

    2018 doi

  41. [49]

    , Miesch , M

    barticle Karak , B.B. , Miesch , M. , Bekki , Y. : 2018 , Consequences of high effective Prandtl number on solar differential rotation and convective velocity . Physics of Fluids 30 , 046602 . https://doi.org/10.1063/1.5022034 . 2018PhFl...30d6602K . barticle

    2018 doi

  42. [50]

    , Jiang , J

    barticle Karak , B.B. , Jiang , J. , Miesch , M.S. , Charbonneau , P. , Choudhuri , A.R. : 2014 , Flux Transport Dynamos: From Kinematics to Dynamics . 186 , 561 . https://doi.org/10.1007/s11214-014-0099-6 . 2014SSRv..186..561K . barticle

    2014 doi

  43. [51]

    a pyl \"a , P.J. , K \

    barticle Karak , B.B. , K \"a pyl \"a , P.J. , K \"a pyl \"a , M.J. , Brandenburg , A. , Olspert , N. , Pelt , J. : 2015 , Magnetically controlled stellar differential rotation near the transition from solar to anti-solar profiles . 576 , A26 . https://doi.org/10.1051/0004-636...

    2015 doi

  44. [52]

    , Nepomnyashchikh , A

    barticle Kitchatinov , L. , Nepomnyashchikh , A. : 2017 , How supercritical are stellar dynamos, or why do old main-sequence dwarfs not obey gyrochronology? 470 , 3124 . https://doi.org/10.1093/mnras/stx1473 . 2017MNRAS.470.3124K . barticle

    2017 doi

  45. [53]

    , Olemskoy , S.V

    barticle Kitchatinov , L.L. , Olemskoy , S.V. : 2010 , Dynamo hysteresis and grand minima of solar activity . Astron. Lett. 36 , 292 . barticle

    2010

  46. [54]

    , Olemskoy , S.V

    barticle Kitchatinov , L.L. , Olemskoy , S.V. : 2011 , Does the Babcock-Leighton mechanism operate on the Sun? Astronomy Letters 37 , 656 . https://doi.org/10.1134/S0320010811080031 . 2011AstL...37..656K . barticle

    2011 doi

  47. [55]

    , R \"a dler , K.H

    bbook Krause , F. , R \"a dler , K.H. : 1980 , Mean-field magneto\-hydro\-dynamics and dynamo theory , Oxford: Pergamon Press . bbook

    1980

  48. [56]

    , Biswas , A

    barticle Kumar , P. , Biswas , A. , Karak , B.B. : 2022 , Physical link of the polar field buildup with the Waldmeier effect broadens the scope of early solar cycle prediction: Cycle 25 is likely to be slightly stronger than Cycle 24 . 513 , L112 . https://doi.org/10.1093/mnra...

    2022 doi

  49. [57]

    , Karak , B.B

    botherref Kumar , P. , Karak , B.B. , Sreedevi , A. : 2024, Variabilities in the polar field and solar cycle due to irregular properties of Bipolar Magnetic Regions . . https://doi.org/10.1093/mnras/stae1052 . 2024MNRAS.tmp.1058K . botherref

    2024 doi

  50. [58]

    , Karak , B.B

    barticle Kumar , P. , Karak , B.B. , Vashishth , V. : 2021 , Supercriticality of the Dynamo Limits the Memory of the Polar Field to One Cycle . 913 , 65 . https://doi.org/10.3847/1538-4357/abf0a1 . 2021ApJ...913...65K . barticle

    2021 doi

  51. [59]

    , Nagy , M

    barticle Kumar , P. , Nagy , M. , Lemerle , A. , Karak , B.B. , Petrovay , K. : 2021 , The Polar Precursor Method for Solar Cycle Prediction: Comparison of Predictors and Their Temporal Range . 909 , 87 . https://doi.org/10.3847/1538-4357/abdbb4 . 2021ApJ...909...87K . barticle

    2021 doi

  52. [60]

    : 1969 , A Magneto-Kinematic Model of the Solar Cycle

    barticle Leighton , R.B. : 1969 , A Magneto-Kinematic Model of the Solar Cycle . 156 , 1 . https://doi.org/10.1086/149943 . 1969ApJ...156....1L . barticle

    1969 doi

  53. [61]

    , Egeland , R

    barticle Metcalfe , T.S. , Egeland , R. , van Saders , J. : 2016 , Stellar Evidence That the Solar Dynamo May Be in Transition . 826 , L2 . https://doi.org/10.3847/2041-8205/826/1/L2 . 2016ApJ...826L...2M . barticle

    2016 doi

  54. [62]

    : 1978 , Magnetic field generation in electrically conducting fluids

    bbook Moffatt , H.K. : 1978 , Magnetic field generation in electrically conducting fluids . 1978mfge.book.....M . bbook

    1978

  55. [63]

    , Karak , B.B

    barticle Mordvinov , A.V. , Karak , B.B. , Banerjee , D. , Golubeva , E.M. , Khlystova , A.I. , Zhukova , A.V. , Kumar , P. : 2022 , Evolution of the Sun's activity and the poleward transport of remnant magnetic flux in Cycles 21-24 . 510 , 1331 . https://doi.org/10.1093/mnras...

    2022 doi

  56. [64]

    , Dasi-Espuig , M

    barticle Mu \ n oz-Jaramillo , A. , Dasi-Espuig , M. , Balmaceda , L.A. , DeLuca , E.E. : 2013 , Solar Cycle Propagation, Memory, and Prediction: Insights from a Century of Magnetic Proxies . 767 , L25 . https://doi.org/10.1088/2041-8205/767/2/L25 . 2013ApJ...767L..25M . barticle

    2013 doi

  57. [65]

    , Hartmann , L.W

    barticle Noyes , R.W. , Hartmann , L.W. , Baliunas , S.L. , Duncan , D.K. , Vaughan , A.H. : 1984 , Rotation, convection, and magnetic activity in lower main-sequence stars . 279 , 763 . https://doi.org/10.1086/161945 . 1984ApJ...279..763N . barticle

    1984 doi

  58. [66]

    , Kitchatinov , L.L

    barticle Olemskoy , S.V. , Kitchatinov , L.L. : 2013 , Grand Minima and North-South Asymmetry of Solar Activity . 777 , 71 . barticle

    2013

  59. [67]

    , Choudhuri , A.R

    barticle Olemskoy , S.V. , Choudhuri , A.R. , Kitchatinov , L.L. : 2013 , Fluctuations in the alpha-effect and grand solar minima . Astronomy Reports 57 , 458 . https://doi.org/10.1134/S1063772913050065 . 2013ARep...57..458O . barticle

    2013 doi

  60. [68]

    : 1955 , Hydromagnetic Dynamo Models

    barticle Parker , E.N. : 1955 , Hydromagnetic Dynamo Models. 122 , 293 . https://doi.org/10.1086/146087 . 1955ApJ...122..293P . barticle

    1955 doi

  61. [69]

    , Nandy , D

    barticle Passos , D. , Nandy , D. , Hazra , S. , Lopes , I. : 2014 , A solar dynamo model driven by mean-field alpha and Babcock-Leighton sources: fluctuations, grand-minima-maxima, and hemispheric asymmetry in sunspot cycles . 563 , A18 . https://doi.org/10.1051/0004-6361/201...

    2014 doi

  62. [70]

    , Charbonneau , P

    barticle Racine , \'E . , Charbonneau , P. , Ghizaru , M. , Bouchat , A. , Smolarkiewicz , P.K. : 2011 , On the Mode of Dynamo Action in a Global Large-eddy Simulation of Solar Convection . 735 , 46 . https://doi.org/10.1088/0004-637X/735/1/46 . 2011ApJ...735...46R . barticle

    2011 doi

  63. [71]

    : 1984 , Age-rotation relationship for late-type main-sequence stars

    barticle Rengarajan , T.N. : 1984 , Age-rotation relationship for late-type main-sequence stars . 283 , L63 . barticle

    1984

  64. [72]

    , Nesme-Ribes , E

    barticle Ribes , J.C. , Nesme-Ribes , E. : 1993 , The solar sunspot cycle in the Maunder minimum AD1645 to AD1715 . 276 , 549 . 1993A\ barticle

    1993

  65. [73]

    , Scherrer , P.H

    barticle Schatten , K.H. , Scherrer , P.H. , Svalgaard , L. , Wilcox , J.M. : 1978 , Using dynamo theory to predict the sunspot number during solar cycle 21 . 5 , 411 . https://doi.org/10.1029/GL005i005p00411 . 1978GeoRL...5..411S . barticle

    1978 doi

  66. [74]

    , Wright , J.T

    barticle Shah , S.P. , Wright , J.T. , Isaacson , H. , Howard , A.W. , Curtis , J.L. : 2018 , HD 4915: A Maunder Minimum Candidate . 863 , L26 . https://doi.org/10.3847/2041-8213/aad40c . 2018ApJ...863L..26S . barticle

    2018 doi

  67. [75]

    : 1972 , Time Scales for CA II Emission Decay, Rotational Braking, and Lithium Depletion

    barticle Skumanich , A. : 1972 , Time Scales for CA II Emission Decay, Rotational Braking, and Lithium Depletion . 171 , 565 . https://doi.org/10.1086/151310 . 1972ApJ...171..565S . barticle

    1972 doi

  68. [76]

    , Jha , B.K

    barticle Sreedevi , A. , Jha , B.K. , Karak , B.B. , Banerjee , D. : 2024 , Analysis of BMR Tilt from AutoTAB Catalog: Hinting toward the Thin Flux Tube Model? 966 , 112 . https://doi.org/10.3847/1538-4357/ad34b8 . 2024ApJ...966..112S . barticle

    2024 doi

  69. [77]

    , Beaudoin , P

    barticle Strugarek , A. , Beaudoin , P. , Charbonneau , P. , Brun , A.S. : 2018 , On the Sensitivity of Magnetic Cycles in Global Simulations of Solar-like Stars . 863 , 35 . https://doi.org/10.3847/1538-4357/aacf9e . 2018ApJ...863...35S . barticle

    2018 doi

  70. [78]

    , Nandy , D

    barticle Tripathi , B. , Nandy , D. , Banerjee , S. : 2021 , Stellar mid-life crisis: subcritical magnetic dynamos of solar-like stars and the breakdown of gyrochronology . 506 , L50 . https://doi.org/10.1093/mnrasl/slab035 . 2021MNRAS.506L..50T . barticle

    2021 doi

  71. [79]

    : 2023 , A history of solar activity over millennia

    barticle Usoskin , I.G. : 2023 , A history of solar activity over millennia . Living Reviews in Solar Physics 20 , 2 . https://doi.org/10.1007/s41116-023-00036-z . 2023LRSP...20....2U . barticle

    2023 doi

  72. [80]

    , Solanki , S.K

    barticle Usoskin , I.G. , Solanki , S.K. , Kovaltsov , G.A. : 2007 , Grand minima and maxima of solar activity: new observational constraints . 471 , 301 . barticle

    2007

  73. [81]

    , Solanki , S.K

    barticle Usoskin , I.G. , Solanki , S.K. , Krivova , N.A. , Hofer , B. , Kovaltsov , G.A. , Wacker , L. , Brehm , N. , Kromer , B. : 2021 , Solar cyclic activity over the last millennium reconstructed from annual ^ 14 C data . 649 , A141 . https://doi.org/10.1051/0004-6361/202...

    2021 doi

  74. [82]

    , Solanki , S.K

    barticle Usoskin , I.G. , Solanki , S.K. , Krivova , N. , Hofer , B. , Kovaltsov , G.A. , Wacker , L. , Brehm , N. , Kromer , B. : 2022 , Solar cyclic activity over the last millennium reconstructedfrom annual ^ 14 C data (Corrigendum) . 664 , C3 . https://doi.org/10.1051/0004...

    2022 doi

  75. [83]

    , Karak , B.B

    barticle Vashishth , V. , Karak , B.B. , Kitchatinov , L. : 2021 , Subcritical dynamo and hysteresis in a Babcock-Leighton type kinematic dynamo model . Research in Astronomy and Astrophysics 21 , 266 . https://doi.org/10.1088/1674-4527/21/10/266 . 2021RAA....21..266V . barticle

    2021 doi

  76. [84]

    , Karak , B.B

    barticle Vashishth , V. , Karak , B.B. , Kitchatinov , L. : 2023 , Dynamo modelling for cycle variability and occurrence of grand minima in Sun-like stars: rotation rate dependence . 522 , 2601 . https://doi.org/10.1093/mnras/stad1105 . 2023MNRAS.522.2601V . barticle

    2023 doi

  77. [85]

    , Gregory , S.G

    barticle Vidotto , A.A. , Gregory , S.G. , Jardine , M. , Donati , J.F. , Petit , P. , Morin , J. , Folsom , C.P. , Bouvier , J. , Cameron , A.C. , Hussain , G. , Marsden , S. , Waite , I.A. , Fares , R. , Jeffers , S. , do Nascimento , J.D. : 2014 , Stellar magnetism: empiric...

    2014 doi

  78. [86]

    , Nandy , D

    barticle Wilmot-Smith , A.L. , Nandy , D. , Hornig , G. , Martens , P.C.H. : 2006 , A Time Delay Model for Solar and Stellar Dynamos . 652 , 696 . https://doi.org/10.1086/508013 . 2006ApJ...652..696W . barticle

    2006 doi

  79. [87]

    : 2016, Stellar Magnetic Activity Cycles, and Hunting for Maunder Minimum-like Events among Sun-like Stars

    botherref Wright , J.T. : 2016, Stellar Magnetic Activity Cycles, and Hunting for Maunder Minimum-like Events among Sun-like Stars . AGU Fall Meeting Abstracts, SH43D. 2016AGUFMSH43D2592W . botherref

    2016

Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.