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A dynamo model of magnetic activity in solar-like stars with different rotational velocities

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Bidya Binay Karak, Leonid L. Kitchatinov, Arnab Rai Choudhuri

Solar and Stellar Astrophysics · Submitted 8 Feb 2014

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We find that the dimensionless amplitude $f_m$ of the toroidal flux through the star increases with decreasing rotation period.

how it is stated · asserted 1.00 read the record →

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arXiv ID1402.1874 (version 3)
Pith ID6FJCCP7Z, Pith's permanent record of this paper and its review
CitationArnab Rai Choudhuri, Bidya Binay Karak, Leonid L. Kitchatinov. "A dynamo model of magnetic activity in solar-like stars with different rotational velocities." arXiv:1402.1874 (2014). https://pith.science/paper/6FJCCP7Z
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The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,611 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.98 · human participants 0.01 · controlled comparison 0.09 · randomized assignment 0.01 · states quantitative result 0.76 · compares with prior results 0.62 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v3. Results and the main claim are underlined; .

We attempt to provide a quantitative theoretical explanation for the observations that Ca II H/K emission and X-ray emission from solar-like stars increase with decreasing Rossby number (i.e., with faster rotation). Assuming that these emissions are caused by magnetic cycles similar to the sunspot cycle, we construct flux transport dynamo models of $1M_{\odot}$ stars rotating with different rotation periods. We first compute the differential rotation and the meridional circulation inside these stars from a mean-field hydrodynamics model. Then these are substituted in our dynamo code to produce periodic solutions. We find that the dimensionless amplitude $f_m$ of the toroidal flux through the star increases with decreasing rotation period. The observational data can be matched if we assume the emissions to go as the power 3-4 of $f_m$. Assuming that the Babcock-Leighton mechanism saturates with increasing rotation, we can provide an explanation for the observed saturation of emission at low Rossby numbers. The main failure of our model is that it predicts an increase of magnetic cycle period with increasing rotation rate, which is the opposite of what is found observationally. Much of our calculations are based on the assumption that the magnetic buoyancy makes the magnetic flux tubes to rise radially from the bottom of the convection zone. On taking account of the fact that the Coriolis force diverts the magnetic flux tubes to rise parallel to the rotation axis in rapidly rotating stars, the results do not change qualitatively.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 We attempt to provide a quantitative theoretical explanation for the observations that Ca II H/K emission and X-ray emission from solar-like stars increase with decreasing Rossby number (i.e., with faster rotation). background 0.64 0.12 0.09 hedged possibility 0.41
s1 Assuming that these emissions are caused by magnetic cycles similar to the sunspot cycle, we construct flux transport dynamo models of $1M_{\odot}$ stars rotating with different rotation periods. method 0.78 0.91 0.04 asserted 0.81
s2 We first compute the differential rotation and the meridional circulation inside these stars from a mean-field hydrodynamics model. method 1.00 0.91 0.02 asserted 0.97
s3 Then these are substituted in our dynamo code to produce periodic solutions. method 1.00 0.90 0.03 asserted 0.98
s4 We find that the dimensionless amplitude $f_m$ of the toroidal flux through the star increases with decreasing rotation period. result 1.00 0.97 0.32 asserted 1.00
s5 The observational data can be matched if we assume the emissions to go as the power 3-4 of $f_m$. interpretation 0.70 0.64 0.21 hedged possibility 0.79
s6 Assuming that the Babcock-Leighton mechanism saturates with increasing rotation, we can provide an explanation for the observed saturation of emission at low Rossby numbers. interpretation 0.74 0.81 0.13 hedged possibility 0.68
s7 The main failure of our model is that it predicts an increase of magnetic cycle period with increasing rotation rate, which is the opposite of what is found observationally. limitation 1.00 0.89 0.22 asserted 1.00
s8 Much of our calculations are based on the assumption that the magnetic buoyancy makes the magnetic flux tubes to rise radially from the bottom of the convection zone. method 0.73 0.47 0.02 asserted 0.86
s9 On taking account of the fact that the Coriolis force diverts the magnetic flux tubes to rise parallel to the rotation axis in rapidly rotating stars, the results do not change qualitatively. result 0.73 0.79 0.05 asserted 1.00

What kind of paper the classifier reports this is: simulation study 0.77 · evidence from simulation or computation 1.00.

What was examined, and what was not

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not examined
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  • figures and tables
  • references and citing sentences
  • relations to other papers
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  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

We attempt to provide a quantitative theoretical explanation for the observations that Ca II H/K emission and X-ray emission from solar-like stars increase with decreasing Rossby number (i.e., with faster rotation). Assuming that these emissions are caused by magnetic cycles similar to the sunspot cycle, we construct flux transport dynamo models of $1M_{\odot}$ stars rotating with different rotation periods. We first compute the differential rotation and the meridional circulation inside these stars from a mean-field hydrodynamics model. Then these are substituted in our dynamo code to produce periodic solutions. We find that the dimensionless amplitude $f_m$ of the toroidal flux through the star increases with decreasing rotation period. The observational data can be matched if we assume the emissions to go as the power 3-4 of $f_m$. Assuming that the Babcock-Leighton mechanism saturates with increasing rotation, we can provide an explanation for the observed saturation of emission at low Rossby numbers. The main failure of our model is that it predicts an increase of magnetic cycle period with increasing rotation rate, which is the opposite of what is found observationally. Much of our calculations are based on the assumption that the magnetic buoyancy makes the magnetic flux tubes to rise radially from the bottom of the convection zone. On taking account of the fact that the Coriolis force diverts the magnetic flux tubes to rise parallel to the rotation axis in rapidly rotating stars, the results do not change qualitatively.

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References
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6 arXiv papers cite this in 9 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 6 sentences without a confident label

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Cites it as support 1 paper
  • So, when we want to vary our dynamo parameters over a wide range or when we use unusual parameter specifications (such as a multi-cell meridional circulation), we are often unable to obtain results with the local $α$ parameterization procedure and are forced to use the more robust non-local procedure described in 3.1 [ref] .

    The treatment of magnetic buoyancy in flux transport dynamo models · Comparison between the non-local and local methods · 0.97

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