arxiv: 2605.06872 · v1 · submitted 2026-05-07 · 🌌 astro-ph.SR · astro-ph.GA

Recognition: no theorem link

On the origin of the rotation of massive stars

Andr\'e Oliva , Facundo D. Moyano , Luca Sciarini , Sylvia Ekstr\"om , Patrick Eggenberger , Georges Meynet

Authors on Pith no claims yet

Pith reviewed 2026-05-11 01:09 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA

keywords massive star rotationprotostellar jetsangular momentum transportstar formationaccretion disksmagnetohydrodynamicspre-main sequence evolution

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The pith

Magnetically driven protostellar jets carry away enough angular momentum to keep forming massive stars below critical rotation at all times.

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

Massive stars lack the strong magnetic fields that brake low-mass stars, so the usual disk-locking mechanisms do not apply and the origin of their observed rotation rates has remained unclear. The authors perform two-dimensional radiation-gravito-magnetohydrodynamical simulations that follow the collapse of a molecular cloud core through disk formation and the launching of magnetically driven outflows. These simulations show that the jets extract sufficient angular momentum from the inner disk and protostar to prevent the central object from reaching critical rotation speed throughout the entire accretion phase. The final rotation rate at the end of accretion is directly tied to the strength of the jet, which in turn depends on the initial conditions of the parent cloud, naturally producing a range of spin rates.

Core claim

The angular momentum transported outwards by the magnetically-driven protostellar outflows is sufficient for keeping the protostar below the critical speed at all times. The strength of the jet, and thus the rotation rate at the end of the accretion epoch, can be linked to the initial conditions for star formation. Jet strength produces a variety of stellar rotation rates, suggesting that protostellar jets fix the rotation rate of massive stars.

What carries the argument

Magnetically-driven protostellar outflows that extract angular momentum from the protostar and inner accretion disk during the main accretion phase.

If this is right

Protostars remain sub-critical without needing internal magnetic braking during the main accretion phase.
Final stellar rotation rates vary according to the initial molecular cloud properties through differences in jet strength.
The observed distribution of rotation speeds among massive stars arises from variations in jet launching efficiency set at formation.
Accretion ends with the protostar spinning at a rate determined by the balance between accreted angular momentum and that removed by outflows.

Where Pith is reading between the lines

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

The mechanism may explain why massive stars typically rotate faster than low-mass stars, as the braking is less efficient.
Three-dimensional simulations would test whether non-axisymmetric effects change the net angular momentum transport efficiency.
Observational searches for correlations between jet properties in star-forming regions and the spins of nearby young massive stars could provide direct tests.
Differences in cloud turbulence or magnetic field geometry at formation would translate directly into scatter in main-sequence rotation rates.

Load-bearing premise

The two-dimensional axisymmetric simulations accurately represent the net angular momentum loss by jets in three-dimensional geometries and that no other significant braking mechanisms operate during accretion.

What would settle it

A massive protostar observed to reach or exceed critical rotation speed while still actively accreting, or a systematic mismatch between measured spins of young massive stars and the rotation rates predicted from jet strengths in their formation environments.

Figures

Figures reproduced from arXiv: 2605.06872 by Andr\'e Oliva, Facundo D. Moyano, Georges Meynet, Luca Sciarini, Patrick Eggenberger, Sylvia Ekstr\"om.

**Figure 1.** Figure 1: Overview of the angular momentum transport done by the streamlines of the magneto-centrifugal jet, using the data from [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗

**Figure 2.** Figure 2: (a) Evolution of the rotation criticality as a function of the instantaneous stellar mass under two different jet parametrizations. (b) Evolution of the surface and central angular velocity of the protostar as the structure changes from fully convective to fully radiative and then a convective core and radiative envelope. The opaque lines are running averages. naturally the kind of strong radial magnetic … view at source ↗

read the original abstract

We explore the origin of the rotation rates of massive stars. Contrary to their low-mass siblings, most massive stars do not have detectable magnetic fields, so that star-disk interaction models used for the formation of rotating low-mass stars do not apply. We investigate whether the magnetic fields of protostellar jets present in the parent molecular cloud prevent the protostar from reaching the critical angular velocity. Starting from the gravitational collapse of a molecular cloud, we run two two-dimensional radiation-gravito-magnetohydroynamical simulations to study the formation of an accretion disk and the launching of magnetically-driven protostellar outflows (of particular interest is the formation of a magnetocentrifugal jet originating from the protostar and inner disk). We then study the angular momentum transfer from the disk and jet onto the protostar. Finally, we compute one-dimensional stellar evolution models of the pre-main sequence including our results from the disk-jet simulations and follow the angular momentum redistribution within the structure of the protostar. We find that the angular momentum transported outwards by the magnetically-driven protostellar outflows is sufficient for keeping the protostar below the critical speed at all times. Moreover, we are able to link the strength of the jet, and thus the rotation rate at the end of the accretion epoch, to the initial conditions for star formation. Our results show that the jet strength produces a variety of stellar rotation rates, suggesting that protostellar jets fix the rotation rate of massive stars.

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.

Desk Editor's Note private letter to a colleague

2D MHD collapse runs give a plausible jet-based brake on massive protostar spin tied to initial conditions, but axisymmetry likely overstates the torque.

read the letter

This paper claims that magnetically driven protostellar jets remove enough angular momentum during accretion to keep massive stars below critical rotation, and that jet strength maps directly onto the final spin through the starting cloud conditions. They run two 2D radiation-gravito-MHD simulations from cloud collapse through disk and jet formation, extract the net torque on the protostar, and feed those numbers into standard 1D pre-main-sequence models to track internal angular-momentum redistribution up to the end of accretion. The simulations produce a spread in final rotation rates depending on the initial setup, which matches the observed range for massive stars. The work avoids assuming strong stellar magnetic fields, which fits the observational fact that most massive stars show none. The angular-momentum budget comes from the independent collapse runs rather than being tuned to match data afterward. That is the concrete advance: a quantitative chain from initial conditions to final spin via jet-mediated loss. The 1D evolution part follows established methods and shows how the external torque affects the star's internal profile. The main limitation is the 2D axisymmetric setup. In two dimensions the jet stays perfectly collimated and coherent, which can preserve magnetic field structure and inflate the time-integrated angular-momentum flux compared with 3D. Kink or current-driven instabilities that appear in three dimensions commonly weaken jet torque. With only two runs presented and no reported resolution studies, convergence checks, or sensitivity tests in the abstract, it is difficult to judge how much the numbers would shift. The coupling between the 2D outputs and the 1D code is described at a high level, so the exact boundary conditions and any hidden assumptions there also need checking. If the real 3D flux is substantially lower, the claim that jets alone set the rotation rate would not follow from these runs. This is aimed at people working on massive-star formation, angular-momentum transport, and the early phases that set later evolution. A reader who wants a concrete mechanism linking cloud properties to final spin will find the proposed link worth examining, even if the quantitative details require scrutiny. The paper shows honest engagement with the physics and the literature, so it deserves peer review to test the numerics and the dimensionality issue.

Referee Report

2 major / 1 minor

Summary. The manuscript presents two 2D radiation-gravito-MHD simulations starting from molecular cloud collapse to model the formation of accretion disks and magnetically-driven protostellar outflows, including magnetocentrifugal jets. These are used to derive angular momentum budgets that are then incorporated into 1D stellar evolution models to track the protostar's rotation during the pre-main sequence. The central claim is that the angular momentum transported by the outflows is sufficient to prevent the protostar from reaching critical rotation speed, and that variations in jet strength tied to initial conditions can account for the range of observed rotation rates in massive stars.

Significance. If the central claim holds, the work supplies a formation-based explanation for the rotation rates of massive stars that does not invoke internal magnetic braking or star-disk magnetic coupling (mechanisms less relevant for massive stars lacking detectable fields). The explicit link between initial cloud conditions, jet properties, and final stellar spin offers a predictive connection between star-formation physics and observable stellar properties.

major comments (2)

[Numerical setup and jet-launching analysis] The angular-momentum budget is obtained exclusively from two strictly 2D axisymmetric radiation-gravito-MHD runs. In 2D the jet is forced to remain perfectly coherent, which can artificially preserve magnetic-field collimation and overestimate the time-integrated outward angular-momentum flux relative to 3D geometries where kink or current-driven instabilities commonly disrupt jet structure and reduce net torque. Because the 1D stellar models inherit this budget directly and conclude that no additional braking is required, the central claim that outflows alone keep the protostar sub-critical is sensitive to this dimensionality limitation.
[Coupling of simulation outputs to 1D stellar models] No resolution study, convergence tests, or quantitative error estimates on the angular-momentum flux are reported for the 2D simulations. The final rotation rates in the 1D models are therefore presented without demonstrated numerical robustness, which is load-bearing for the assertion that the jet strength produces a variety of stellar rotation rates consistent with observations.

minor comments (1)

[Results and discussion] The abstract states that the jet strength is linked to initial conditions, but the manuscript should explicitly state which parameters (e.g., initial cloud rotation rate or magnetic-field strength) were varied between the two runs and how the resulting jet properties map onto the observed distribution of massive-star rotation rates.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments and for recognizing the potential significance of our results. We address each major comment below, indicating the revisions we will make to strengthen the manuscript.

read point-by-point responses

Referee: [Numerical setup and jet-launching analysis] The angular-momentum budget is obtained exclusively from two strictly 2D axisymmetric radiation-gravito-MHD runs. In 2D the jet is forced to remain perfectly coherent, which can artificially preserve magnetic-field collimation and overestimate the time-integrated outward angular-momentum flux relative to 3D geometries where kink or current-driven instabilities commonly disrupt jet structure and reduce net torque. Because the 1D stellar models inherit this budget directly and conclude that no additional braking is required, the central claim that outflows alone keep the protostar sub-critical is sensitive to this dimensionality limitation.

Authors: We agree that strictly 2D axisymmetric geometry suppresses non-axisymmetric instabilities that can disrupt jets in 3D, which may lead to an overestimate of the time-integrated angular-momentum flux. Our simulations were performed in 2D to reach the necessary resolution and evolutionary times while including radiation transport. Nevertheless, the magnetocentrifugal launching mechanism is active and extracts substantial angular momentum from the inner disk and protostar. In the revised manuscript we will add an explicit discussion of this limitation, stating that our angular-momentum budgets should be viewed as upper limits and that 3D effects could reduce the net torque. We will also note that even a substantial reduction would still leave the protostar sub-critical according to the budgets we obtain. Full 3D radiation-gravito-MHD collapse simulations remain beyond current computational reach for the parameter space explored here. revision: partial
Referee: [Coupling of simulation outputs to 1D stellar models] No resolution study, convergence tests, or quantitative error estimates on the angular-momentum flux are reported for the 2D simulations. The final rotation rates in the 1D models are therefore presented without demonstrated numerical robustness, which is load-bearing for the assertion that the jet strength produces a variety of stellar rotation rates consistent with observations.

Authors: We acknowledge that the original manuscript does not contain a formal resolution study or quantitative error estimates on the angular-momentum fluxes. The two simulations were performed with different initial magnetic-field strengths to demonstrate the dependence of jet properties on formation conditions. In the revised version we will add a new subsection describing the numerical grid, time-stepping criteria, and any internal sensitivity tests we performed on the jet mass and angular-momentum fluxes. We will also provide order-of-magnitude estimates of the uncertainty in the integrated angular-momentum budget that is passed to the 1D stellar models. These additions will make the numerical robustness of the reported rotation-rate variety more transparent. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper's derivation proceeds from two independent 2D radiation-gravito-MHD collapse simulations that compute the angular-momentum flux carried by the magnetocentrifugal jet; these fluxes are then supplied as boundary conditions to separate 1D stellar-evolution calculations. Neither step fits parameters to observed rotation rates, renames a known result, nor invokes a self-citation as the sole justification for a uniqueness claim. The final statement that jets suffice to keep the protostar sub-critical is therefore a direct numerical consequence of the reported simulation outputs rather than a tautology or self-referential fit.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the validity of the 2D MHD collapse simulations and their coupling to 1D stellar models; these rely on standard astrophysical assumptions rather than new free parameters or invented entities.

axioms (2)

domain assumption Ideal MHD approximation is valid throughout the collapse and jet-launching phase
Invoked by the radiation-gravito-magnetohydrodynamical simulations described in the abstract.
domain assumption Two-dimensional axisymmetric geometry captures the dominant angular-momentum transport by jets
The simulations are performed in 2D; the abstract does not discuss 3D corrections.

pith-pipeline@v0.9.0 · 5580 in / 1470 out tokens · 42477 ms · 2026-05-11T01:09:53.286797+00:00 · methodology

discussion (0)

Reference graph

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