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arxiv: 2604.19967 · v1 · submitted 2026-04-21 · 🌌 astro-ph.SR

Recognition: unknown

The curved jet in the young star FN Tau

M.A. Burlak , A.V. Dodin , A.V. Zharova , N.P. Ikonnikova , V.A. Kiryukhina , S.A. Lamzin , D.A. Lashin , B.S. Safonov
Authors on Pith no claims yet

Pith reviewed 2026-05-10 01:11 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords young starprotoplanetary diskstellar jetHerbig-Haro objectsprecessionFN Tauoutflow
0
0 comments X

The pith

The curved jet from FN Tau arises from precession of the inner protoplanetary disk.

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

This paper reports the detection of a microjet and four Herbig-Haro objects near the young star FN Tau that together trace a bipolar collimated outflow designated HH 1267. The jet does not follow a straight path even though it is collimated. The authors propose that the observed curvature results from precession of the inner regions of the protoplanetary disk around FN Tau. Because the jet axis lies at an angle of less than 20 degrees to the line of sight, even modest changes in launch direction produce a noticeable bend in the projected structure. They further link the start of the microjet activity to stellar outbursts that occurred about 60 years ago.

Core claim

In the vicinity of the young star FN Tau, a microjet and four Herbig-Haro objects have been detected whose positions and kinematics indicate the presence of a bipolar collimated outflow from the star, HH 1267. The stellar jet does not propagate rectilinearly, and the curved shape of the jet, whose axis is inclined to the line of sight at an angle less than 20 degrees, results from the precession of the inner regions of the FN Tau protoplanetary disk. Approximately 60 years ago the star underwent outbursts with an amplitude of about 2 magnitudes lasting several months, which are associated with the onset of the microjet.

What carries the argument

Precession of the inner regions of the protoplanetary disk, which steadily changes the orientation of the jet launch axis.

If this is right

  • The jet launch direction changes continuously as the inner disk precesses, producing the observed non-straight path.
  • The small inclination angle to the line of sight makes the curvature from precession especially visible in projection.
  • The microjet activity began during the star's outbursts roughly 60 years ago.

Where Pith is reading between the lines

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

  • If the precession interpretation holds, similar curved jets in other young stars could be examined for evidence of inner-disk wobble.
  • Repeated high-resolution observations could reveal the precession period directly from changes in jet morphology.
  • The link to past outbursts suggests that strong accretion events can initiate or reorient collimated outflows.

Load-bearing premise

The curvature of the jet is produced by precession of the inner disk rather than by interaction with ambient material or by projection effects.

What would settle it

Time-series imaging or spectroscopy that tracks the jet's position angle over multiple decades to test whether the bend evolves periodically in the manner expected for disk precession.

read the original abstract

In the vicinity of the young star FN Tau, we have detected a microjet and four Herbig-Haro objects, whose positions and kinematics indicate the presence of a bipolar collimated outflow from the star - HH 1267. The stellar jet does not propagate rectilinearly, and we discuss the possibility that the curved shape of the jet, whose axis is inclined to the line of sight at an angle $<20^\circ$, results from the precession of the inner regions of the FN Tau protoplanetary disk. Approximately 60 years ago, the star underwent outbursts with an amplitude of $\Delta m_{\rm pg} \sim 2^{\rm m}$ lasting several months, which we associate with the onset of the microjet.

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 / 1 minor

Summary. The manuscript reports the detection of a microjet and four Herbig-Haro objects near the young star FN Tau, whose positions and kinematics indicate a bipolar collimated outflow designated HH 1267. The stellar jet is observed to propagate non-rectilinearly, and the authors discuss the possibility that this curvature, for a jet axis inclined at less than 20 degrees to the line of sight, results from precession of the inner regions of the FN Tau protoplanetary disk. They also associate photometric outbursts of amplitude ~2 mag approximately 60 years ago with the onset of the microjet.

Significance. If the precession interpretation can be substantiated, the work would add a well-documented example of a curved microjet in a T Tauri star and strengthen the observational link between inner-disk dynamics and outflow morphology. The new positional and kinematic data on the microjet and HH objects would be a useful addition to the sample of young stellar outflows.

major comments (2)
  1. [Abstract / Discussion] Abstract and discussion section: The central suggestion that the observed curvature arises from inner-disk precession is presented without any quantitative forward model (e.g., a ballistic precessing jet with specified precession angle, period, and <20° inclination projected onto the sky and compared to the measured loci and radial velocities of the microjet and HH objects). No calculation is shown that reproduces the data or that rules out alternatives such as ram-pressure deflection or projection effects.
  2. [Abstract] The inclination of the jet axis (<20°) is stated without accompanying error analysis, derivation method, or reference to specific velocity or proper-motion measurements that constrain it.
minor comments (1)
  1. [Abstract] The abstract refers to 'the stellar jet' and 'the microjet' interchangeably; consistent terminology would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive review of our manuscript on the curved jet in FN Tau. We address each major comment below and indicate the revisions planned for the resubmitted version.

read point-by-point responses

  1. Referee: [Abstract / Discussion] Abstract and discussion section: The central suggestion that the observed curvature arises from inner-disk precession is presented without any quantitative forward model (e.g., a ballistic precessing jet with specified precession angle, period, and <20° inclination projected onto the sky and compared to the measured loci and radial velocities of the microjet and HH objects). No calculation is shown that reproduces the data or that rules out alternatives such as ram-pressure deflection or projection effects.

    Authors: We acknowledge that the precession interpretation would be strengthened by a quantitative forward model. The present work is observational in focus, reporting the detection, positions, and kinematics of the microjet and HH objects. Constructing a ballistic precession model that reproduces the observed loci and velocities would require additional free parameters (precession angle, period, jet velocity profile) that are not tightly constrained by the current dataset. In the revised manuscript we will expand the discussion to include a qualitative comparison of the observed curvature with simple precession expectations, explicitly note the limitations of the data for quantitative modeling, and state that alternatives such as ram-pressure deflection or projection effects cannot be ruled out. We will also cite examples from the literature where similar curved jets have been modeled. revision: partial

  2. Referee: [Abstract] The inclination of the jet axis (<20°) is stated without accompanying error analysis, derivation method, or reference to specific velocity or proper-motion measurements that constrain it.

    Authors: The <20° inclination is derived in the main text from the ratio of the measured radial velocities to the transverse proper motions of the jet knots, adopting a characteristic microjet speed of ~150 km s^{-1} for T Tauri stars. Uncertainties are propagated from the velocity measurement errors. We will revise the abstract to include a short clause referencing this method and directing readers to the relevant section and error analysis in the body of the paper. revision: yes

Circularity Check

0 steps flagged

No circularity: observational interpretation of jet curvature grounded in new data without reduction to fitted inputs or self-citations

full rationale

The manuscript reports positions, kinematics, and morphology of a newly detected microjet and four HH objects from imaging and spectroscopy. It notes non-rectilinear propagation and discusses precession of the inner disk as one possible explanation for curvature at inclination <20°, while associating past outbursts with jet onset. No equations, parameters, or forward models are introduced that would make the curvature equivalent to the precession hypothesis by construction. No self-citations are invoked as load-bearing uniqueness theorems or ansatzes. The central claim remains an interpretive possibility rather than a derived result that reduces to its own inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Observational astronomy paper with no explicit modeling; relies on standard assumptions about jet propagation and shock emission in star-forming regions.

axioms (2)
  • domain assumption Herbig-Haro objects trace shocks from collimated outflows
    Standard in YSO studies; invoked when associating the four objects with the bipolar outflow.
  • domain assumption Kinematic data can be used to infer outflow direction and inclination
    Used to conclude the axis is inclined <20° to the line of sight.

pith-pipeline@v0.9.0 · 5459 in / 1344 out tokens · 39955 ms · 2026-05-10T01:11:23.884811+00:00 · methodology

discussion (0)

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Reference graph

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