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arxiv: 2605.13189 · v1 · submitted 2026-05-13 · 🌌 astro-ph.SR · astro-ph.GA

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The Accretion Process on Protostars

Eleonora Fiorellino , Alice Somigliana
Authors on Pith no claims yet

Pith reviewed 2026-05-14 18:36 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords protostellar accretionyoung stellar objectsClass 0/Imass assemblyobservational techniquesnumerical simulationsplanet formation
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The pith

Accretion onto protostars assembles most stellar mass in Class 0/I phases but lacks the unified understanding achieved for later stages.

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

The paper reviews recent observational and numerical results on mass accretion onto young stellar objects to deliver an updated assessment focused on the protostellar phases. It presents measurement techniques, analyzes how methodological choices affect rate estimates, and discusses challenges in aligning data with simulations. By bridging these approaches the work identifies gaps and proposes concrete next steps toward a more complete picture. This matters because accretion sets final stellar masses and the initial conditions for planet formation.

Core claim

The accretion process on protostars assembles the bulk of stellar mass during the Class 0 and I phases through envelope infall and disk accretion, with observational estimates from luminosity and spectral diagnostics requiring careful comparison to numerical models while accounting for methodological differences and parameter-estimation caveats.

What carries the argument

Techniques to measure accretion rates on protostars, including bolometric luminosity, veiling, and emission-line diagnostics, which are cross-checked against hydrodynamic simulations of collapse and accretion flows.

Where Pith is reading between the lines

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

  • The bridged view implies that accretion variability during the protostellar phase could shape the stellar initial mass function.
  • Future observations targeting specific envelope and disk structures could directly test the numerical predictions highlighted in the review.
  • Continuity between protostellar and classical T Tauri accretion mechanisms suggests evolutionary models could be linked more tightly across stages.

Load-bearing premise

Recent observational and numerical results on protostellar accretion can be meaningfully compared and synthesized despite acknowledged methodological differences and caveats in parameter estimation.

What would settle it

A large survey revealing systematic offsets in accretion rates between observations and current models that exceed all stated uncertainties would undermine the possibility of a coherent synthesis.

Figures

Figures reproduced from arXiv: 2605.13189 by Alice Somigliana, Eleonora Fiorellino.

Figure 1
Figure 1. Figure 1: Schematic representation of the accretion process in Class 0 and Class I protostars. Class 0 objects (left) are characterized by a massive, optically thick envelope dominating the system mass and feeding the disk and protostar, with accretion possibly occurring through non-magnetospheric inner-disk processes. In Class I sources (right), the envelope becomes progressively thinner and less massive, the disk … view at source ↗
Figure 2
Figure 2. Figure 2: Spectral index vs. bolometric temperature for young stars analysed with Spitzer in Perseus, Serpens, and Ophiuchus. The bold symbols indicate sources that are associated with 1.1 mm emission, and the thin symbols denote those with upper limits at 1.1 mm. Class divisions for both Tbol and αIR are shown. The two methods agree fairly well for Class II and “warmer” Class I sources, but very cold (Tbol ≲ 100 K)… view at source ↗
Figure 3
Figure 3. Figure 3: Comparisons of the CO (v = 2 → 1) (left) and Brγ (right) emission-line between Class 0 (red) and Class I (blue) protostars. The distribution of line parameter values is shown in the form of a CDF (normalized by the detection rate of the line in a given sample) and a histogram (shown in the sub-box on the right-hand side of the plot). Each point of the CDFs corresponds to one object’s measurement and uncert… view at source ↗
Figure 4
Figure 4. Figure 4: Lacc − L⋆ (left) and M˙ acc − M⋆ (right) distributions showing accretion being more intense in Class I and FS than in Class II for sources with the same stellar luminosity or mass. Colored points correspond to Class I and FS as described in the legend, while empty circles correspond to Class II. Triangles are upper limits. Adapted from Fiorellino et al. (2023). © AAS. Reproduced with permission. assumption… view at source ↗
Figure 5
Figure 5. Figure 5: Mass accretion rate vs. disk dust mass. Red and purple filled circles are the Class I sources. Empty circles are Class II from Lupus. The blue line corresponds to the best fit for the overall sample of Class I YSOs, while the light blue lines are a subsample of the results of some chains. The dashed grey shows the best fit for Class II YSOs (Manara et al., 2016). Adapted from Fiorellino et al. (2022b). © A… view at source ↗
Figure 6
Figure 6. Figure 6: Time evolution of the accretion rate in thin-disc approximation simulations. Adapted from Vorobyov and Basu (2005b, 2006, 2010) (panels from left to right). © AAS. Reproduced with permission. 4.2 Pure hydrodynamic simulations The first generation of cloud collapse simulations featured a pure hydrodynamical approach with self￾gravity, typically employing the thin disk approximation or SPH. 4.2.1 The Vorobyo… view at source ↗
Figure 7
Figure 7. Figure 7: Snapshots of the logarithm of the column density in a 1 pc × 1 pc region produced from the simulations of Bonnell et al. (2003) at four consequent times from left to right (1.9, 2.6, 3.4, and 4.5 ×105 yr). The color scale spans from a minimum of 0.025 (black) to a maximum of 250 (yellow) g cm−3 . Each dot indicates a star.. core to stellar densities was performed by Bate (1998), followed by several pieces … view at source ↗
Figure 8
Figure 8. Figure 8: Cumulative initial mass function produced by a barotropic equation of state (thin solid and dashed lines) and radiation hydrodynamical calculations (thick solid, dashed, and thin dot-dashed lines). Adapted from Bate (2009) with permission, CC BY 4.0. the natural improvement of simple hydrodynamical models is the coupling with radiative transfer to what is commonly referred to as radiation hydrodynamics (RH… view at source ↗
Figure 9
Figure 9. Figure 9: Density maps centered around selected sink particles (indicated by the black circles) in ideal (left) and non-ideal (right) MHD core-collapse simulations after 117 kyr of evolution. Adapted from Lebreuilly et al. (2021). © AAS. Reproduced with permission. 5 PROTOSTELLAR ACCRETION: THE EMERGING PICTURE 5.1 Uncertainties in the retrieval and comparison of observables from simulations The availability of a la… view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of the observed range of values (gray shaded region) with simulation-inferred mass accretion rates from two numerical setups. We indicate the mean value with a circle and the 16th and 84th percentile ranges with a solid line; the dashed lines represent the interval between the minimum and maximum values. and White and Hillenbrand (2004) show significantly lower fractions of such objects, rangin… view at source ↗
read the original abstract

The process of mass accretion onto Young Stellar Objects (YSOs) plays a fundamental role in determining the final stellar mass and setting the initial conditions for planet formation. Despite its critical role, our understanding of accretion remains fragmented, particularly for what concerns the earliest, protostellar phases (Class 0/I). While the community has consolidated a comprehensive knowledge of the accretion process of the later-stage Classical T Tauri Stars (CTTSs), a similar level of understanding is critically lacking for the protostellar phase, where the bulk of the mass is assembled. This work aims to review recent major results, both from the observational and numerical point of view, bridging the gap between the two approaches and providing an updated, complete assessment of accretion in protostellar sources. We present different techniques to measure accretion on protostars, analyze how methodological differences affect parameter estimation, discuss the caveats in comparing with numerical models, and suggest the next steps to take towards an ever more exhaustive picture of the protostellar phase.

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

0 major / 2 minor

Summary. This manuscript is a review that summarizes recent observational and numerical results on mass accretion onto protostars (Class 0/I young stellar objects). It examines techniques for measuring accretion rates, analyzes how methodological differences affect parameter estimation, discusses caveats when comparing observations with simulations, and suggests next steps toward a more complete picture of the protostellar accretion phase, building on established knowledge for classical T Tauri stars.

Significance. If the synthesis successfully qualifies comparisons between observations and simulations while explicitly addressing methodological differences and caveats, the review would provide a useful consolidated assessment for the field. Accretion during the protostellar phase determines final stellar mass and sets initial conditions for planet formation, so a careful bridging of fragmented knowledge could help guide future work without overclaiming unification.

minor comments (2)
  1. The manuscript would benefit from a summary table listing key observational techniques (e.g., line luminosities, veiling) alongside typical uncertainties and example accretion-rate values drawn from the cited studies; this would make the discussion of methodological differences more concrete and easier to reference.
  2. In the section on numerical models, clarify the range of initial conditions and resolutions used in the simulations being compared, as these directly influence the predicted accretion variability and could affect the strength of the claimed caveats.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive summary, significance assessment, and recommendation of minor revision. We appreciate the recognition of the manuscript's aim to bridge observational and numerical approaches to protostellar accretion. No specific major comments were provided in the report, so we have no point-by-point rebuttals. We will incorporate minor revisions as appropriate in the next version.

Circularity Check

0 steps flagged

Review synthesis with no derivations or fitted predictions

full rationale

The manuscript is explicitly a review paper whose goal is to summarize and compare existing observational and numerical results on protostellar accretion while cataloguing methodological differences and parameter-estimation caveats. No new equations, first-principles derivations, predictions, or fitted parameters are introduced that could reduce to the paper's own inputs. Self-citations, if present, serve only as pointers to prior literature and do not bear the load of any claimed unification or result. The central claim is therefore the provision of a qualified synthesis rather than any quantitative output that could be circular by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

As this is a review paper and only the abstract is available, no new free parameters, axioms, or invented entities are introduced by the authors. The work relies entirely on standard assumptions and results from the prior astrophysical literature on star formation.

pith-pipeline@v0.9.0 · 5473 in / 1075 out tokens · 36810 ms · 2026-05-14T18:36:10.857404+00:00 · methodology

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