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arxiv: 2607.00077 · v1 · pith:ODB2AEKXnew · submitted 2026-06-30 · 🌌 astro-ph.GA · astro-ph.SR

Hot or Cold? Radial Redistribution of Stars in FIRE Simulations of Milky Way-Mass Galaxies and the Asymmetry of Inward versus Outward Migrators

Cecilia Steel , Andrew Wetzel , Rori Kang , Fiona McCluskey , Sarah Loebman , Kathryne J. Daniel This is my paper

Pith reviewed 2026-07-02 18:35 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords stellar migrationgalactic disksdynamical heatingorbital eccentricityFIRE simulationsMilky Wayradial redistributioninward versus outward migration
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The pith

Radial redistribution of stars in Milky Way-mass galaxies is typically not cold between birth and today.

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

The paper tests whether stars that radially migrate in galactic disks do so while preserving orbital eccentricity, as assumed in many cold-torquing models. Using FIRE zoom-in simulations of 12 Milky Way-mass galaxies, it selects star particles with large changes in angular momentum since birth and tracks their eccentricity changes. Outward migrators show smaller eccentricity shifts while inward migrators almost always heat, and the fraction that stays cold drops below 50 percent for stars older than about 2 Gyr. A population of stars that dynamically cool is also identified as the main route to circular orbits today. Migration direction, birth eccentricity, and age together set whether a star heats, cools, or stays unchanged.

Core claim

In the FIRE simulations, the cold-torqued fraction of star particles with |Δj_φ/j_φ,birth| > 0.2 that also satisfy |Δe| < 0.1 is generally low. For stars born on near-circular orbits the fraction falls rapidly with age and is typically under 50 percent beyond ~2 Gyr. Inward-migrating stars heat almost without exception while outward migrators experience smaller net eccentricity growth. Stars born with moderate eccentricity (~0.4) are likeliest to preserve their birth value. Earlier-forming or dynamically colder disks show higher cold fractions. A cooling population exists and is the primary way stars reach near-circular orbits today. Overall, migration direction, e_birth, and age determine t

What carries the argument

The cold-torqued fraction, which measures the share of significantly migrated star particles that preserve |Δe| < 0.1 since birth and thereby quantifies net dynamical heating versus preservation.

If this is right

  • Inward-migrating stars almost always experience net dynamical heating.
  • The cold-torqued fraction decreases rapidly with age for stars born on near-circular orbits.
  • Stars born on moderately eccentric orbits are the most likely to keep their birth eccentricity.
  • A population of stars that cool dynamically supplies most of the near-circular orbits observed today.
  • Earlier-forming and dynamically colder disks retain higher fractions of cold migrators.

Where Pith is reading between the lines

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

  • Models that rely on cold torquing alone will under-predict the heating of inward-migrated stars and mis-estimate the ages of stars on circular orbits.
  • The asymmetry between inward and outward migrators offers a testable signature in the eccentricity distribution of the Milky Way disk at different radii.
  • The cooling population implies that some old stars on circular orbits formed with higher eccentricity and later lost it rather than forming cold.
  • Applying the same birth-to-present tracking to lower-mass or higher-redshift disks would reveal how the balance of heating versus cooling changes with galaxy properties.

Load-bearing premise

The FIRE simulations correctly capture the combined heating and cooling effects on stellar orbits from birth to the present day.

What would settle it

A direct count in the Milky Way showing that most stars with large radial migration since birth have |Δe| < 0.1, especially among inward migrators older than 2 Gyr, would falsify the typical-not-cold result.

Figures

Figures reproduced from arXiv: 2607.00077 by Andrew Wetzel, Cecilia Steel, Fiona McCluskey, Kathryne J. Daniel, Rori Kang, Sarah Loebman.

Figure 2
Figure 2. Figure 2: — Median change in eccentricity, from birth to today, versus amount of radial redistribution (via fractional change in orbital angular momentum), for all stars (regardless of birth eccentricity). We separate populations of stars into the three eras of disk evolution in which they formed. We measure these eras separately for each galaxy, but they correspond to typical ages of: pre-disk (≳ 8 Gyr ago), early-… view at source ↗
Figure 3
Figure 3. Figure 3: — Left: Normalized distribution of eccentricity, 𝑒, at birth (solid) and today (dotted), for stars that experienced significant radial redistribution (|Δ𝑗𝜙/ 𝑗𝜙,birth | > 0.2). We separate stars born in the three eras of disk evolution, which we measure separately for each galaxy: pre-disk (typically 𝑒birth ≳ 0.9), early-disk (typically 𝑒birth ≈ 0.4), and late-disk (typically 𝑒birth ≈ 0.2). Lines show the m… view at source ↗
Figure 4
Figure 4. Figure 4: — Median change in orbital eccentricity from birth to today, Δ𝑒, versus eccentricity at birth (left) and today (right), for all stars (regardless of birth eccentricity) that redistributed significantly inward (dashed) or outward (solid). Different colored lines show stars born in the three eras of disk evolution. Lines show the mean, shaded regions show the 68th percentile scatter across the 12 galaxies. T… view at source ↗
Figure 5
Figure 5. Figure 5: — Median change in orbital eccentricity from birth to today, Δ𝑒, versus stellar age, for all stars (regardless of birth eccentricity) that redis￾tributed significantly outwards (solid) and inwards (dashed). The teal lines show the mean, shaded regions show the 68th percentile scatter across the 12 galaxies. The blue horizontal shaded region marks stars whose dynamical evolution from birth to today was ‘col… view at source ↗
Figure 6
Figure 6. Figure 6: — Left: Cold-torqued fraction versus stellar age, separately for outward and inward migrators. We define the cold-torqued fraction as the number of star particles that experienced minimal changes in orbital eccentricity relative to the total number that redistributed significantly (in the given direction). Lines show the mean, shaded regions show the 68th percentile scatter across the 12 galaxies. We show … view at source ↗
Figure 7
Figure 7. Figure 7: — Cold-torqued fraction versus orbital eccentricity at birth (left) and today (right), for stars separated into the three disk eras in which they were born, and separately for inward- and outward-migrating stars. The cold-torqued fraction is defined as the number of stars that experienced minimal change in eccentricity relative to all stars of a given eccentricity that were significantly radially redistrib… view at source ↗
Figure 8
Figure 8. Figure 8: — Cold-torqued fraction versus radius at birth (left) and today (right), for stars separated into the three disk eras in which they were born. The top row includes all stars, while the bottom row includes only stars formed on near-circular orbits (𝑒birth < 0.2). The cold-torqued fraction is defined as the fraction of stars that undergo significant radial redistribution while experiencing only minimal chang… view at source ↗
Figure 9
Figure 9. Figure 9: — Left: Cold-torqued fraction versus stellar age for stars with 𝑒birth < 0.2 and separated by migration direction. We show our four earliest-forming galaxies, which also have the highest 𝑣𝜙/𝜎v today, ordered from earliest to latest disk onset: m12q, Romeo, m12m, and m12b. The cold-torqued fraction is highest in m12q, which has the earliest disk onset, and decreases with later disk onset times. Right: The s… view at source ↗
Figure 10
Figure 10. Figure 10: — Left: Cold-torqued fraction of stars with ages < 2 Gyr and 𝑒birth < 0.2, shown separately for inward and outward migrators in each galaxy, versus the lookback time of the galaxy’s early disk onset (when 𝑣𝜙/𝜎𝑣,3D > 1) and late disk onset (when 𝑣𝜙/𝜎𝑣,3D > 3). Right: The same, versus the present-day 𝑣𝜙/𝜎𝑣,3D measured for stars with ages < 100 Myr, a metric for the galaxy’s current diskiness. Galaxies with … view at source ↗
Figure 12
Figure 12. Figure 12: — Dynamically cooled fraction versus orbital eccentricity today. This fraction is the number of stars that experienced a significant reduction in eccentricity (Δ𝑒 < −0.1) relative to all stars born in the given era. Lines show the mean, shaded regions show the 68th percentile scatter across the 12 galaxies. Most stars on circular orbits today (𝑒now ≲ 0.1) dynamically cooled (became more circular) since bi… view at source ↗
read the original abstract

Stars can radially redistribute (migrate) within galactic disks. The degree to which this occurs as dynamically `cold' (preserves orbital eccentricity) or `hot' (increases eccentricity) remains debated. Many models presume that radial redistribution occurs primarily via cold torquing, resulting in changes in angular momentum without dynamical heating. We test the net dynamical heating associated with redistribution over stellar lifetimes using the FIRE cosmological zoom-in simulations of 12 Milky Way-mass galaxies. We select star particles today that underwent significant changes in orbital angular momentum, j_phi, since birth. We investigate net changes in their orbital eccentricity, e, and we quantify the `cold-torqued' fraction of star particles with |Delta j_phi/j_phi,birth| > 0.2 that preserved eccentricity (|Delta e| < 0.1) since birth. The direction of radial redistribution is most critical: outward-migrating stars experienced smaller net changes in eccentricity, whereas inward-migrating stars almost always heat since birth. For stars born on near-circular orbits (e_birth < 0.2), the cold-torqued fraction decreases rapidly with age today and is generally < 50% at ages >~2 Gyr. Stars born on moderately eccentric orbits (e_birth ~ 0.4) are the most likely to preserve their birth eccentricity. However, the cold-torqued fraction is higher in earlier-forming and/or dynamically-colder disks. Significantly, we identify a population of stars that dynamically `cooled', decreasing in eccentricity since birth: this is the primary way that stars end up on near-circular orbits today. Overall, a star's migration direction, its e_birth, and its age primarily determine whether it was dynamically heated, cooled, or unchanged. In general, radial redistribution in FIRE is typically not cold between birth and today.

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

1 major / 2 minor

Summary. The paper analyzes star particles in 12 FIRE cosmological zoom-in simulations of Milky Way-mass galaxies, selecting those with significant angular momentum changes since birth (|Δj_φ/j_φ,birth| > 0.2). It reports that inward migrators almost always increase eccentricity while outward migrators show smaller net changes; for stars born on near-circular orbits (e_birth < 0.2), the cold-torqued fraction (|Δe| < 0.1) drops below 50% for ages ≳2 Gyr, with a population that cools dynamically; migration direction, birth eccentricity, and age determine net heating/cooling, leading to the conclusion that radial redistribution in FIRE is typically not cold.

Significance. If the reported Δe values are physical, the work provides direct evidence from multiple high-resolution cosmological simulations that challenges the common modeling assumption of primarily cold torquing during radial migration. It quantifies an asymmetry between inward and outward migrators, identifies dynamical cooling as a route to near-circular orbits today, and shows that birth conditions and age control outcomes. The approach of direct particle counts and fractions (no fitted parameters) across 12 galaxies offers a statistically grounded, falsifiable assessment of net dynamical effects over stellar lifetimes.

major comments (1)
  1. [Methods and Results (selection of migrators and Δe measurements)] The central claim that redistribution is typically not cold (cold-torqued fraction generally <50% for e_birth<0.2 at ages>2 Gyr) rests on measured Δe being physical rather than numerical. The manuscript reports results for the |Δj_φ/j_φ,birth|>0.2 sample across 12 galaxies but does not present resolution-convergence tests or softening-variation runs at the ~7000 M⊙ star-particle mass resolution; this is load-bearing because two-body scattering and potential fluctuations can artificially drive eccentricity growth, especially for inward migrators.
minor comments (2)
  1. [Abstract] The abstract states the main thresholds and conclusions but omits the simulation mass resolution and any discussion of selection effects on the migrator sample; adding these would improve clarity for readers.
  2. [Discussion] The paper credits direct particle tracking but could explicitly note the absence of free parameters or fitted models in the fraction calculations to highlight this strength.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and for emphasizing the need to establish that the measured Δe values reflect physical processes. We respond to the single major comment below.

read point-by-point responses

  1. Referee: [Methods and Results (selection of migrators and Δe measurements)] The central claim that redistribution is typically not cold (cold-torqued fraction generally <50% for e_birth<0.2 at ages>2 Gyr) rests on measured Δe being physical rather than numerical. The manuscript reports results for the |Δj_φ/j_φ,birth|>0.2 sample across 12 galaxies but does not present resolution-convergence tests or softening-variation runs at the ~7000 M⊙ star-particle mass resolution; this is load-bearing because two-body scattering and potential fluctuations can artificially drive eccentricity growth, especially for inward migrators.

    Authors: We agree that explicit demonstration that Δe is not dominated by numerical effects is essential for the central claim. The current manuscript does not include dedicated resolution or softening tests for this specific measurement. However, the FIRE-2 simulations at this resolution have been shown in prior work to produce converged orbital eccentricity distributions and radial migration statistics for Milky Way-mass galaxies (Hopkins et al. 2018; Garrison-Kimmel et al. 2018; Wetzel et al. 2023). More importantly, two aspects of the results are difficult to explain as numerical artifacts: (1) the strong directional asymmetry, with inward migrators systematically heating while outward migrators show smaller net changes, and (2) the existence of a dynamically cooling population that decreases in eccentricity. Two-body scattering and potential fluctuations would be expected to increase eccentricity isotropically rather than produce net cooling or a clear inward/outward asymmetry. We will add a concise subsection in the Methods section that summarizes these prior convergence results and explicitly notes the cooling population as supporting evidence that the trends are physical. We therefore view the requested tests as addressable via citation and discussion rather than new simulations. revision: yes

Circularity Check

0 steps flagged

No circularity: direct particle statistics from simulations

full rationale

The paper reports fractions of star particles satisfying explicit selection criteria (|Δj_φ/j_φ,birth| > 0.2 and |Δe| < 0.1) computed directly from tracked simulation outputs across 12 galaxies. No equations, fitted parameters, or self-citations are used to derive the central cold-torqued fractions or the inward/outward asymmetry; these are raw counts and binned statistics. The derivation chain consists solely of particle selection and histogram construction on the simulation data, with no reduction of outputs to inputs by construction. External concerns about numerical heating are validity issues, not circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the assumption that the simulations faithfully reproduce real dynamical evolution; no free parameters or invented entities are introduced in the abstract.

axioms (1)
  • domain assumption FIRE cosmological zoom-in simulations accurately represent the physics of stellar radial migration in Milky Way-mass galaxies.
    Conclusions about real galaxies depend on simulation fidelity.

pith-pipeline@v0.9.1-grok · 5910 in / 989 out tokens · 27943 ms · 2026-07-02T18:35:18.494093+00:00 · methodology

discussion (0)

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