Do accretion-powered stellar winds help spin down T Tauri stars?

Ann Marie Cody; Eric Gaidos; Laura Venuti; Lukas Gehrig; Neal J. Turner

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Do accretion-powered stellar winds help spin down T Tauri stars?

Lukas Gehrig, Eric Gaidos, Laura Venuti, Ann Marie Cody, Neal J. Turner

Solar and Stellar Astrophysics · Submitted 4 Apr 2025

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

The authors' main claim Newly developed lightcurve analysis methods enable measuring $\mathcal{R}$ for enough stars to distinguish the spin-down scenarios in the course of upcoming observing campaigns.

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arXiv ID2504.03374 (version 1)

Pith ID5UC2AWFA, Pith's permanent record of this paper and its review

CitationAnn Marie Cody, Eric Gaidos, Laura Venuti, Lukas Gehrig, Neal J. Turner. "Do accretion-powered stellar winds help spin down T Tauri stars?." arXiv:2504.03374 (2025). https://pith.science/paper/5UC2AWFA

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,655 input tokens.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.51 · human participants 0.02 · controlled comparison 0.13 · randomized assignment 0.02 · states quantitative result 0.96 · compares with prior results 0.33 · mentions code or data availability 0.03.

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How T Tauri stars remain slowly rotating while still accreting material is a long-standing puzzle. Current models suggest that these stars may lose angular momentum through magnetospheric ejections of disk material (MEs) and accretion-powered stellar winds (APSWs). The individual contribution of each mechanism to the stellar spin evolution, however, is unclear. We explore how these two scenarios could be distinguished by applying stellar spin models to near-term observations. We produce synthetic stellar populations of accreting Class II stars with spreads in the parameters governing the spin-down processes and find that an APSW strongly affects the ratio of the disk truncation radius to the corotation radius, $\mathcal{R} = R_\mathrm{t}/R_\mathrm{co}$. The ME and APSW scenarios are distinguished to high confidence when at least $N_\mathrm{crit}\gtrsim 250$ stars have values measured for $\mathcal{R}$. Newly developed lightcurve analysis methods enable measuring $\mathcal{R}$ for enough stars to distinguish the spin-down scenarios in the course of upcoming observing campaigns.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	How T Tauri stars remain slowly rotating while still accreting material is a long-standing puzzle.	background 0.98	0.03	0.02	asserted 0.99
s1	Current models suggest that these stars may lose angular momentum through magnetospheric ejections of disk material (MEs) and accretion-powered stellar winds (APSWs).	background 1.00	0.04	0.03	hedged possibility 1.00
s2	The individual contribution of each mechanism to the stellar spin evolution, however, is unclear.	gap 1.00	0.04	0.02	asserted 0.81
s3	We explore how these two scenarios could be distinguished by applying stellar spin models to near-term observations.	contribution 0.86	0.65	0.04	hedged possibility 0.87
s4	We produce synthetic stellar populations of accreting Class II stars with spreads in the parameters governing the spin-down processes and find that an APSW strongly affects the ratio of the disk truncation radius to the corotation radius, $\mathcal{R} = R_\mathrm{t}/R_\mathrm{co}$.	result 0.82	0.96	0.33	asserted 1.00
s5	The ME and APSW scenarios are distinguished to high confidence when at least $N_\mathrm{crit}\gtrsim 250$ stars have values measured for $\mathcal{R}$.	result 0.95	0.80	0.45	asserted 0.99
s6	Newly developed lightcurve analysis methods enable measuring $\mathcal{R}$ for enough stars to distinguish the spin-down scenarios in the course of upcoming observing campaigns.	interpretation 0.43	0.24	0.31	asserted 0.90

What kind of paper the classifier reports this is: simulation study 0.92 · evidence from simulation or computation 0.99.

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The paper

Original abstract

How T Tauri stars remain slowly rotating while still accreting material is a long-standing puzzle. Current models suggest that these stars may lose angular momentum through magnetospheric ejections of disk material (MEs) and accretion-powered stellar winds (APSWs). The individual contribution of each mechanism to the stellar spin evolution, however, is unclear. We explore how these two scenarios could be distinguished by applying stellar spin models to near-term observations. We produce synthetic stellar populations of accreting Class II stars with spreads in the parameters governing the spin-down processes and find that an APSW strongly affects the ratio of the disk truncation radius to the corotation radius, $\mathcal{R} = R_\mathrm{t}/R_\mathrm{co}$. The ME and APSW scenarios are distinguished to high confidence when at least $N_\mathrm{crit}\gtrsim 250$ stars have values measured for $\mathcal{R}$. Newly developed lightcurve analysis methods enable measuring $\mathcal{R}$ for enough stars to distinguish the spin-down scenarios in the course of upcoming observing campaigns.

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2 arXiv papers cite this in 10 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

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Uses its method or tool 1 paper

The spin population model by [ref] would be used to generate synthetic populations of CTTSs that reproduce the ($M_⋆$, $Ṁ_acc$, $P_rot$) composition of the observed sample and are assumed to be in rotational equilibrium with or without the assistance of winds.

Preparing for the Early eVolution Explorer: Photometric Diagnostics of Magnetospheric Accretion Geometry in Young Stellar Objects · Parameter determination and hypothesis testing · 0.99

Compares with it 1 paper

The fastness parameter of the ZTS resulting from these input values is $ω_S ≈0.72$, which matches the results of recent simulations [ref] and population models [ref] .

The effect of variable stellar magnetic fields on the spin state of T Tauri stars · List of parameters · 0.99

What it cites

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The measurement of $M_⋆$ is subject to uncertainties of 0.35 dex [ref] .

Demographics of young stars and their protoplanetary disks: lessons learned on disk evolution and its connection to planet formation · Results · 0.97

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