{"total":14,"items":[{"citing_arxiv_id":"2607.01207","ref_index":23,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"No evidence of vorticity production from initially irrotational turbulent gravitational collapse","primary_cat":"physics.flu-dyn","submitted_at":"2026-07-01T17:46:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Direct numerical simulations find no vorticity generation attributable to the collapse flow itself when starting from irrotational turbulence in a barotropic, non-magnetized fluid.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27969","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Formation of Isotopically Heterogeneous Molecular Cloud Cores in Filamentary Molecular Clouds","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T11:17:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SPH simulations of filament fragmentation indicate isotopic inhomogeneities from 1 pc filaments survive in cores at reduced levels and potentially reach circumstellar disks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21989","ref_index":34,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Complex organic molecules in the young hot core RCW 120 S2","primary_cat":"astro-ph.GA","submitted_at":"2026-06-20T10:56:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"APEX 1.3 mm observations of RCW120 S2 detect COMs including CH3OH, CH3CHO, CH3OCHO and CH3OCH3, reveal a radially stratified envelope, and show modest abundance mismatches with hot-core chemical models attributed to unresolved filling factor.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21878","ref_index":95,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The efficiency per free-fall time as a ratio of the Star Formation Rate to the gas-infall rate in collapsing cores: dependence on the core definition, accretion, and radial structure","primary_cat":"astro-ph.SR","submitted_at":"2026-06-20T04:40:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations of collapsing cores find that ε_ff varies with core definition via density threshold, open vs closed boundaries, and initial density, with higher values in low-mass cores due to lower infall rates.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12536","ref_index":36,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Getting to know the Stellar Clusters in NGC 1569: Bayesian inference of stellar cluster properties in a dwarf starburst galaxy","primary_cat":"astro-ph.GA","submitted_at":"2026-06-10T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian IMF-aware inference on NGC 1569 clusters yields correlations between cluster mass-function truncation mass, galactocentric distance, metallicity, and gas ionization state.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00493","ref_index":75,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Non-linear Dynamical Stability of Magnetic Polytropes","primary_cat":"astro-ph.SR","submitted_at":"2026-05-30T02:49:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00205","ref_index":87,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Ultraviolet diversity of Little Red Dots as a probe for direct-collapse black hole ages","primary_cat":"astro-ph.GA","submitted_at":"2026-05-29T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Cosmological hydrodynamical simulations predict that UV diversity in Little Red Dots encodes direct-collapse black hole ages via a rapid transition from BH- to stellar-dominated emission after ~30 Myr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21101","ref_index":145,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T12:30:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20835","ref_index":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T07:26:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12595","ref_index":266,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Global and Local Infall in the ASHES Sample (GLASHES). II. Asymmetric Line Profiles around Dense Cores in 70 $\\mu$m Dark Massive Clumps","primary_cat":"astro-ph.GA","submitted_at":"2026-05-12T18:00:01+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Blue-asymmetric spectral lines appear in 50-60% of dense cores within massive dark clumps, showing that gravitational collapse operates at core scales from prestellar stages onward and supports hierarchical star formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07928","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Systematic Comparison between Constrained Transport and Mixed Divergence Cleaning Methods for Astrophysical Magnetohydrodynamic Simulations","primary_cat":"astro-ph.IM","submitted_at":"2026-05-08T16:01:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Constrained transport outperforms Dedner's divergence cleaning in MHD simulations by avoiding spurious artifacts when magnetic fields are localized or timesteps vary suddenly.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(2002)), and they recommendc r = 0.18. There are a few issues in their formulation. First, cr is not dimensionless, and therefore depends on units (D. J. Price & J. J. Monaghan 2005). In order to clarify its meaning, we should redefine it as the ratio between the advection and diffusion timescales at the scale ofL: Cr ≡ tadv tdiff = L/ch L2/c2p = c2 p chL ,(20) whereC r is dimensionless. Using this, the source term (17) can be rewritten as: ∂ψ ∂t =− ch CrL ψ=− 1 Crtadv ψ. The original formula corresponds to settingL= 1, but the choice of the scale is arbitrary 6. Some simu- lation codes such as PLUTO (A. Mignone et al. 2012; A. Mignone & P. Tzeferacos 2010) for example adopt L=h min. With adaptive mesh refinement (AMR), the"},{"citing_arxiv_id":"2605.03924","ref_index":107,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The slope of the power spectrum of the density field in isothermal supersonic compressible turbulence","primary_cat":"astro-ph.GA","submitted_at":"2026-05-05T16:17:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A model based on Chandrasekhar's 1951 time-invariant quantity quantitatively explains the Mach-number dependence of the density power spectrum slope in isothermal supersonic turbulence and demonstrates that the slope cannot reliably determine the Mach number.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02138","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Fragmentation in the Serpens/Aquila Star-forming Region","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T01:40:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"ALMA Cycle 6 data on Aquila dense cores identifies two starless sources and scale-dependent increases in multiplicity, consistent with turbulent core collapse simulations predicting 1.19 starless detections.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"self-gravity at large global scales (see M. Chevance et al. 2023, and the references therein). There exist several families of models describing the stability and evolution of dense cores. In some, cores evolve in a relatively slow and quasi-static fashion, grad- ually adjusting their structure while resisting collapse for several freefall timescales (R. B. Larson 1969; F. H. Shu 1977). In others, supersonic turbulence induces lo- cal compression, which leads to cores shaped by highly dynamic, turbulent processes that generate inhomo- geneities (e.g., M.-M. Mac Low 1999; L. Hartmann et al. 2001), where only a fraction of these overdensities be- comes gravitationally bound and proceed toward even- tual protostellar collapse (S."},{"citing_arxiv_id":"1907.08542","ref_index":34,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Numerical Methods for Simulating Star Formation","primary_cat":"astro-ph.IM","submitted_at":"2019-07-19T15:12:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review of MHD numerical methods for star formation, covering discretization techniques, divergence-free constraints, sink particles, and non-ideal effects like diffusion and the Hall effect.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}