pith. machine review for the scientific record. sign in

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

Recognition: no theorem link

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
0
0 comments X

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

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

299 extracted references · 274 canonical work pages · 124 internal anchors

  1. [1]

    Article Title

    Author1 LastName1 and Author2 LastName2 and Author3 LastName3. Article Title. Frontiers in Neuroscience. 2013. doi:10.3389/fnins.2013.12345

    work page doi:10.3389/fnins.2013.12345 2013

  2. [2]

    Author Name , title =

  3. [3]

    The title of the book , publisher =

    Bauthor Surname , title =. The title of the book , publisher =

  4. [4]

    The title of the conference proceedings , year = 1996, publisher =

    Cauthor Name and Dauthor Surname and Fauthor LastName , title =. The title of the conference proceedings , year = 1996, publisher =

    1996

  5. [5]

    Gauthor Name1 , title =

  6. [6]

    Hauthor Surname1 , title =

  7. [7]

    Data Title

    Author1 LastName1 and Author2 LastName2 and Author3 LastName3. Data Title. 2011. doi:10.000/55555

    2011

  8. [8]

    VizieR Online Data Catalog , keywords =

    VizieR Online Data Catalog: AAVSO Photometric All Sky Survey (APASS) DR9 (Henden+, 2016). VizieR Online Data Catalog , keywords =

    2016

  9. [9]

    , keywords =

    New Insights on the Accretion Properties of Class 0 Protostars from 2 m Spectroscopy. , keywords =. doi:10.3847/1538-4357/ad2935 , archivePrefix =. 2401.16532 , primaryClass =

    work page doi:10.3847/1538-4357/ad2935

  10. [10]

    A case study of the classical T Tauri star DK Tau

    Correlation between the optical veiling and accretion properties. A case study of the classical T Tauri star DK Tau. , keywords =. doi:10.1051/0004-6361/202347231 , archivePrefix =. 2307.16561 , primaryClass =

    work page doi:10.1051/0004-6361/202347231

  11. [11]

    , keywords =

    Disk Accretion and Mass Loss from Young Stars. , keywords =. doi:10.1086/176344 , adsurl =

    work page doi:10.1086/176344

  12. [12]

    Stellar Properties of Pre-Main Sequence Stars from High Resolution Near-IR Spectra

    Stellar Properties of Pre-Main-Sequence Stars from High-Resolution Near-Infrared Spectra. , keywords =. doi:10.1086/378958 , archivePrefix =. astro-ph/0308522 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/378958

  13. [13]

    , keywords =

    Primordial Stellar Evolution: The Protostar Phase. , keywords =. doi:10.1086/164018 , adsurl =

    work page doi:10.1086/164018

  14. [14]

    , keywords =

    Bolometric Temperatures of Young Stellar Objects. , keywords =. doi:10.1086/186956 , adsurl =

    work page doi:10.1086/186956

  15. [15]

    Magnetic field strengths of hot Jupiters from signals of star-planet interactions

    Magnetic field strengths of hot Jupiters from signals of star-planet interactions. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0840-x , archivePrefix =. 1907.09068 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-019-0840-x 1907

  16. [16]

    Probing T Tauri Accretion and Outflow with 1 Micron Spectroscopy

    Probing T Tauri Accretion and Outflow with 1 Micron Spectroscopy. , keywords =. doi:10.1086/504832 , archivePrefix =. astro-ph/0604006 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/504832

  17. [17]

    , keywords =

    Hubble Space Telescope UV and H Measurements of the Accretion Excess Emission from the Young Giant Planet PDS 70 b. , keywords =. doi:10.3847/1538-3881/abeb7a , archivePrefix =. 2104.13934 , primaryClass =

    work page doi:10.3847/1538-3881/abeb7a

  18. [18]

    Indications of magnetospheric accretion

    Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b. Indications of magnetospheric accretion. , keywords =. doi:10.1051/0004-6361/202245424 , archivePrefix =. 2212.03207 , primaryClass =

    work page doi:10.1051/0004-6361/202245424

  19. [19]

    Evidence for magnetospheric accretion in the young isolated planetary-mass object 2MASS J11151597+1937266

    ExoplaNeT accRetion mOnitoring sPectroscopic surveY (ENTROPY): I. Evidence for magnetospheric accretion in the young isolated planetary-mass object 2MASS J11151597+1937266. , keywords =. doi:10.1051/0004-6361/202450881 , archivePrefix =. 2409.12187 , primaryClass =

    work page doi:10.1051/0004-6361/202450881

  20. [20]

    , keywords =

    A New Model of Jupiter's Magnetic Field From Juno's First Nine Orbits. , keywords =. doi:10.1002/2018GL077312 , adsurl =

    work page doi:10.1002/2018gl077312

  21. [21]

    Two accreting protoplanets around the young star PDS 70

    Two accreting protoplanets around the young star PDS 70. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0780-5 , archivePrefix =. 1906.01486 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-019-0780-5 1906

  22. [22]

    Summary of the contents and survey properties (Corrigendum)

    Gaia Early Data Release 3. Summary of the contents and survey properties (Corrigendum). , keywords =. doi:10.1051/0004-6361/202039657e , adsurl =

    work page doi:10.1051/0004-6361/202039657e

  23. [23]

    A Multiwavelength, Multiepoch Monitoring Campaign of Accretion Variability in T Tauri Stars from the ODYSSEUS Survey. I. HST Far-UV and Near-UV Spectra. , keywords =. doi:10.3847/1538-4357/ad4a62 , archivePrefix =. 2405.21038 , primaryClass =

    work page doi:10.3847/1538-4357/ad4a62

  24. [24]

    A Multiwavelength, Multiepoch Monitoring Campaign of Accretion Variability in T Tauri Stars from the ODYSSEUS Survey. III. Optical Spectra. , keywords =. doi:10.3847/1538-4357/ad65ed , archivePrefix =. 2408.04465 , primaryClass =

    work page doi:10.3847/1538-4357/ad65ed

  25. [25]

    Magnetic Coupling in the Disks Around Young Gas Giant Planets

    Magnetic Coupling in the Disks around Young Gas Giant Planets. , keywords =. doi:10.1088/0004-637X/783/1/14 , archivePrefix =. 1306.2276 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/783/1/14

  26. [26]

    The First Direct Measurements of Magnetic Fields on Very Low-Mass Stars

    The First Direct Measurements of Surface Magnetic Fields on Very Low Mass Stars. , keywords =. doi:10.1086/510304 , archivePrefix =. astro-ph/0610365 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/510304

  27. [27]

    Giant planet and brown dwarf formation

    Giant Planet and Brown Dwarf Formation. Protostars and Planets VI , year = 2014, editor =. doi:10.2458/azu_uapress_9780816531240-ch027 , archivePrefix =. 1401.7559 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.2458/azu_uapress_9780816531240-ch027 2014

  28. [28]

    Gaseous Planets, Protostars And Young Brown Dwarfs : Birth And Fate

    Gaseous Planets, Protostars, and Young Brown Dwarfs: Birth and Fate. Protostars and Planets V , year = 2007, editor =. doi:10.48550/arXiv.astro-ph/0602291 , archivePrefix =. astro-ph/0602291 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0602291 2007

  29. [29]

    , keywords =

    Occurrence Rates of Accreting Companions from a New Method for Computing Emission-line Survey Sensitivity: Application to the H Giant Accreting Protoplanet Survey. , keywords =. doi:10.3847/1538-3881/adc09d , archivePrefix =. 2408.01491 , primaryClass =

    work page doi:10.3847/1538-3881/adc09d

  30. [30]

    The Near-Infrared Outflow and Cavity of the proto-Brown Dwarf Candidate ISO-Oph 200

    The near-infrared outflow and cavity of the proto-brown dwarf candidate ISO-Oph 200. , keywords =. doi:10.1051/0004-6361/201732291 , archivePrefix =. 1801.08749 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201732291

  31. [31]

    X-Shooter observations of low-mass stars in the Eta Chamaeleontis association

    X-shooter observations of low-mass stars in the Chamaeleontis association. , keywords =. doi:10.1051/0004-6361/201630111 , archivePrefix =. 1709.03414 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201630111

  32. [32]

    arXiv e-prints , keywords =

    Coordinated Space and Ground-Based Monitoring of Accretion Bursts in a Protoplanetary Disk: Establishing Mid-Infrared Hydrogen Lines as Accretion Diagnostics for JWST-MIRI. arXiv e-prints , keywords =. doi:10.48550/arXiv.2504.08029 , archivePrefix =. 2504.08029 , primaryClass =

    work page doi:10.48550/arxiv.2504.08029

  33. [33]

    , keywords =

    Accretion and magnetism on young eccentric binaries: DQ Tau and AK Sco. , keywords =. doi:10.1093/mnras/stae383 , archivePrefix =. 2402.01419 , primaryClass =

    work page doi:10.1093/mnras/stae383

  34. [34]

    , keywords =

    Evolution of the relation between the mass accretion rate and the stellar and disk mass from brown dwarfs to stars. , keywords =. doi:10.1051/0004-6361/202348649 , archivePrefix =. 2402.10523 , primaryClass =

    work page doi:10.1051/0004-6361/202348649

  35. [35]

    , keywords =

    Accretion Funnel Reconfiguration during an Outburst in a Young Stellar Object: EX Lupi. , keywords =. doi:10.3847/1538-4357/ad4099 , archivePrefix =. 2404.05420 , primaryClass =

    work page doi:10.3847/1538-4357/ad4099

  36. [36]

    , keywords =

    H Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes. , keywords =. doi:10.3847/1538-3881/adb6a1 , archivePrefix =. 2502.14736 , primaryClass =

    work page doi:10.3847/1538-3881/adb6a1

  37. [37]

    Magnetospheric accretion onto the T Tauri star AA Tauri. I. Constraints from multisite spectrophotometric monitoring. , keywords =

  38. [38]

    Accretion of pre-main-sequence stars in NGC 3603

    Determining stellar accretion rates from Pa _ and Br _ emission lines with JWST NIRSpec. Accretion of pre-main-sequence stars in NGC 3603. , keywords =. doi:10.1051/0004-6361/202449282 , archivePrefix =. 2403.09568 , primaryClass =

    work page doi:10.1051/0004-6361/202449282

  39. [39]

    Temperaments of young stars: Rapid mass-accretion rate changes in T Tauri and Herbig Ae stars

    Temperaments of young stars: rapid mass accretion rate changes in T Tauri and Herbig Ae stars. , keywords =. doi:10.1093/mnras/stu529 , archivePrefix =. 1403.4088 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu529

  40. [40]

    The Astrophysical Journal Letters , author =

    The Time Evolution of \ M\ \_\ d\ / \ M\ in Protoplanetary Disks as a Way to Disentangle between Viscosity and MHD Winds. , keywords =. doi:10.3847/2041-8213/acf048 , archivePrefix =. 2309.04496 , primaryClass =

    work page doi:10.3847/2041-8213/acf048 2041

  41. [41]

    JWST study of the DG Tau B disk-wind candidate. I. Overview and nested H _ 2 -CO outflows. , keywords =. doi:10.1051/0004-6361/202449176 , archivePrefix =. 2403.19400 , primaryClass =

    work page doi:10.1051/0004-6361/202449176

  42. [42]

    Research Notes of the American Astronomical Society , keywords =

    Ultraviolet Legacy Library of Young Stars as Essential Standards (ULLYSES): Data Release I. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/abca2f , adsurl =

    work page doi:10.3847/2515-5172/abca2f

  43. [43]

    Linked accretion and ejection in a Class I protobinary system

    JWST Observations of Young protoStars (JOYS). Linked accretion and ejection in a Class I protobinary system. , keywords =. doi:10.1051/0004-6361/202348889 , archivePrefix =. 2402.04343 , primaryClass =

    work page doi:10.1051/0004-6361/202348889

  44. [44]

    Observatory Operations: Strategies, Processes, and Systems III , year = 2010, editor =

    The X-shooter pipeline. Observatory Operations: Strategies, Processes, and Systems III , year = 2010, editor =. doi:10.1117/12.857211 , adsurl =

    work page doi:10.1117/12.857211 2010

  45. [45]

    Cool Stars, Stellar Systems and the Sun , year = 1986, editor =

    Evidence for Magnetic Activity in T Tauri Stars. Cool Stars, Stellar Systems and the Sun , year = 1986, editor =. doi:10.1007/3-540-16763-3_158 , adsurl =

    work page doi:10.1007/3-540-16763-3_158 1986

  46. [46]

    Accreting Protoplanets in the LkCa 15 Transition Disk

    Accreting protoplanets in the LkCa 15 transition disk. , keywords =. doi:10.1038/nature15761 , archivePrefix =. 1511.07456 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature15761

  47. [47]

    Accretion in Brown Dwarfs: an Infrared View

    Accretion in brown dwarfs: An infrared view. , keywords =. doi:10.1051/0004-6361:20040356 , archivePrefix =. astro-ph/0406106 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20040356

  48. [48]

    , keywords =

    Magnetospheric Accretion as a Source of H Emission from Protoplanets around PDS 70. , keywords =. doi:10.3847/1538-4357/ab44c1 , archivePrefix =. 1909.06450 , primaryClass =

    work page doi:10.3847/1538-4357/ab44c1 1909

  49. [49]

    Large-scale alpha^2-dynamo in low-mass stars and brown dwarfs

    Large-scale \^2-dynamo in low-mass stars and brown dwarfs. , keywords =. doi:10.1051/0004-6361:20042475 , archivePrefix =. astro-ph/0510075 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20042475

  50. [50]

    Herschel/PACS Spectroscopic Survey of Protostars in Orion: The Origin of Far-Infrared CO Emission

    Herschel/PACS Spectroscopic Survey of Protostars in Orion: The Origin of Far-infrared CO Emission. , keywords =. doi:10.1088/0004-637X/763/2/83 , archivePrefix =. 1211.2234 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/763/2/83

  51. [51]

    Imaging the water-snow line during a protostellar outburst

    Imaging the water snow-line during a protostellar outburst. , keywords =. doi:10.1038/nature18612 , archivePrefix =. 1607.03757 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature18612

  52. [52]

    , keywords =

    The Rate, Amplitude, and Duration of Outbursts from Class 0 Protostars in Orion. , keywords =. doi:10.3847/2041-8213/ac46ae , archivePrefix =. 2201.04647 , primaryClass =

    work page doi:10.3847/2041-8213/ac46ae 2041

  53. [53]

    The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. VI. Insights from Radiative Transfer Modeling. , keywords =. doi:10.3847/1538-4357/ac574d , archivePrefix =. 2203.00029 , primaryClass =

    work page doi:10.3847/1538-4357/ac574d

  54. [54]

    Evolution of Mass Outflow in Protostars

    Evolution of Mass Outflow in Protostars. , keywords =. doi:10.3847/0004-637X/828/1/52 , archivePrefix =. 1511.04787 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/828/1/52

  55. [55]

    , keywords =

    The Evolution of Far-infrared CO Emission from Protostars. , keywords =. doi:10.3847/0004-637X/831/1/69 , adsurl =

    work page doi:10.3847/0004-637x/831/1/69

  56. [56]

    , keywords =

    On the protostellar mass-luminosity relation. , keywords =. doi:10.1093/mnras/staf1220 , archivePrefix =. 2507.18728 , primaryClass =

    work page doi:10.1093/mnras/staf1220

  57. [57]

    arXiv e-prints , keywords =

    Investigating the Nested Structure of the Outflow from the Low Luminosity Protostar IRAS 16253-2429 using JWST and ALMA. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.09837 , archivePrefix =. 2602.09837 , primaryClass =

    work page doi:10.48550/arxiv.2602.09837

  58. [58]

    F., Tychoniec , ., Rocha , W

    JWST Observations of Young protoStars (JOYS): Overview of program and early results. , keywords =. doi:10.1051/0004-6361/202554444 , archivePrefix =. 2505.08002 , primaryClass =

    work page doi:10.1051/0004-6361/202554444

  59. [59]

    , keywords =

    IPA: Class 0 Protostars Viewed in CO Emission Using JWST. , keywords =. doi:10.3847/1538-4357/ad6b92 , archivePrefix =. 2312.07807 , primaryClass =

    work page doi:10.3847/1538-4357/ad6b92

  60. [60]

    , keywords =

    Investigating Protostellar Accretion-driven Outflows across the Mass Spectrum: JWST NIRSpec Integral Field Unit 3 5 m Spectral Mapping of Five Young Protostars. , keywords =. doi:10.3847/1538-4357/ad2fa0 , archivePrefix =. 2310.03803 , primaryClass =

    work page doi:10.3847/1538-4357/ad2fa0

  61. [61]

    Passive irradiated circumstellar disks with an inner hole

    Passive Irradiated Circumstellar Disks with an Inner Hole. , keywords =. doi:10.1086/323057 , archivePrefix =. astro-ph/0106470 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/323057

  62. [62]

    , keywords =

    An Observational View of Structure in Protostellar Systems. , keywords =. doi:10.1146/annurev-astro-052920-103752 , archivePrefix =. 2403.15550 , primaryClass =

    work page doi:10.1146/annurev-astro-052920-103752

  63. [63]

    , keywords =

    Coevolution of Stars and Gas: Using an Analysis of Synthetic Observations to Investigate the Star-Gas Correlation in STARFORGE. , keywords =. doi:10.3847/1538-4357/ad03f1 , archivePrefix =. 2310.11544 , primaryClass =

    work page doi:10.3847/1538-4357/ad03f1

  64. [64]

    Protostellar half-life: new methodology and estimates

    Protostellar half-life: new methodology and estimates. , keywords =. doi:10.1051/0004-6361/201731584 , archivePrefix =. 1807.11262 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731584

  65. [66]

    Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs. , keywords =. doi:10.1086/508424 , archivePrefix =. astro-ph/0608234 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/508424

  66. [67]

    , keywords =

    Flat Spectrum T Tauri Stars: The Case for Infall. , keywords =. doi:10.1086/174731 , adsurl =

    work page doi:10.1086/174731

  67. [68]

    , keywords =

    An HST Survey of Protostellar Outflow Cavities: Does Feedback Clear Envelopes?. , keywords =. doi:10.3847/1538-4357/abded8 , archivePrefix =. 2102.06717 , primaryClass =

    work page doi:10.3847/1538-4357/abded8

  68. [69]

    Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds. , keywords =. doi:10.3847/1538-4365/acbfac , archivePrefix =. 2209.12090 , primaryClass =

    work page doi:10.3847/1538-4365/acbfac

  69. [70]

    Luminosity Functions of Spitzer Identified Protostars in Nine Nearby Molecular Clouds

    Luminosity Functions of Spitzer-identified Protostars in Nine Nearby Molecular Clouds. , keywords =. doi:10.1088/0004-6256/144/2/31 , archivePrefix =. 1204.1535 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/144/2/31

  70. [71]

    , keywords =

    Formation and evolution of a protoplanetary disk: Combining observations, simulations, and cosmochemical constraints. , keywords =. doi:10.1051/0004-6361/202451388 , archivePrefix =. 2409.06342 , primaryClass =

    work page doi:10.1051/0004-6361/202451388

  71. [72]

    Can we predict the global magnetic topology of a pre-main sequence star from its position in the Hertzsprung-Russell diagram?

    Can We Predict the Global Magnetic Topology of a Pre-main-sequence Star from Its Position in the Hertzsprung-Russell Diagram?. , keywords =. doi:10.1088/0004-637X/755/2/97 , archivePrefix =. 1206.5238 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/755/2/97

  72. [73]

    Simulations of dynamo action in fully convective stars

    Simulations of Dynamo Action in Fully Convective Stars. , keywords =. doi:10.1086/527432 , archivePrefix =. 0712.1603 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/527432

  73. [74]

    A global correlation linking young stars, clouds, and galaxies. Towards a unified view of star formation

    A global correlation linking young stars, clouds, and galaxies. Towards a unified view of star formation. , keywords =. doi:10.1051/0004-6361/201833166 , archivePrefix =. 1808.07297 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833166

  74. [75]

    , keywords =

    Hydrogen Recombination Line Luminosities and Variability from Forming Planets. , keywords =. doi:10.3847/1538-4357/abb5a2 , archivePrefix =. 2002.09918 , primaryClass =

    work page doi:10.3847/1538-4357/abb5a2 2002

  75. [76]

    Magnetospheric Accretion or Boundary Layer?

    On the Mass Accretion Rates of Herbig Ae/Be Stars. Magnetospheric Accretion or Boundary Layer?. Galaxies , keywords =. doi:10.3390/galaxies8020039 , archivePrefix =. 2005.01745 , primaryClass =

    work page doi:10.3390/galaxies8020039 2005

  76. [77]

    A multiwavelength interferometric, spectropolarimetric, and photometric observing campaign

    Investigating the magnetospheric accretion process in the young pre-transitional disk system DoAr 44 (V2062 Oph). A multiwavelength interferometric, spectropolarimetric, and photometric observing campaign. , keywords =. doi:10.1051/0004-6361/202038892 , archivePrefix =. 2010.00887 , primaryClass =

    work page doi:10.1051/0004-6361/202038892 2010

  77. [78]

    The GRAVITY young stellar object survey. X. Probing the inner disk and magnetospheric accretion region of CI Tau. , keywords =. doi:10.1051/0004-6361/202346446 , archivePrefix =. 2305.08170 , primaryClass =

    work page doi:10.1051/0004-6361/202346446

  78. [79]

    On the existence of accretion-driven bursts in massive star formation

    On the existence of accretion-driven bursts in massive star formation. , keywords =. doi:10.1093/mnrasl/slw187 , archivePrefix =. 1609.03402 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slw187

  79. [80]

    Formation of giant planets and brown dwarfs on wide orbits

    Formation of giant planets and brown dwarfs on wide orbits. , keywords =. doi:10.1051/0004-6361/201220601 , archivePrefix =. 1302.1892 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220601

  80. [81]

    , archivePrefix = "arXiv", eprint =

    The Jeans mass as a fundamental measure of self-gravitating disc fragmentation and initial fragment mass. , keywords =. doi:10.1111/j.1365-2966.2011.19380.x , archivePrefix =. 1107.0831 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19380.x 2011

Showing first 80 references.