{"total":18,"items":[{"citing_arxiv_id":"2606.30089","ref_index":40,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Projection Is All You Need: Interpreting Polarization Measurements in the Orion Clouds with Sub-Alfv\\'enic MHD Simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-29T10:27:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Sub-Alfvénic MHD simulations with projection effects reproduce the range of observed polarization (μ, σ) values in Orion ISF, showing these statistics alone cannot constrain the 3D Alfvén Mach number.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27346","ref_index":78,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"3D Magnetic Field Vectors in Space: Bubbles, Clouds, and Filaments","primary_cat":"astro-ph.GA","submitted_at":"2026-06-25T17:51:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Reviews SKA techniques for reconstructing 3D magnetic field vectors in the ISM but presents no new data or derivations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26278","ref_index":128,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The 10-15 GHz radio continuum survey of the Galactic Plane with SKAO","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T18:19:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The paper outlines the goals for the SKA-Mid Galactic Plane survey at 10-15 GHz to deliver the first uniform high-resolution view of ionized structures and feedback in the Milky Way.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25580","ref_index":58,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The magnetic field in the Milky Way Galaxy: from large to small scales","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T08:54:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The paper describes the expected capabilities of the SKA-Mid survey to produce a complete map of the Milky Way's magnetic field in the southern hemisphere using rotation measures and polarized emission.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25291","ref_index":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Formation of a Protostellar Multiple System via Rotational Fragmentation","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T01:49:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Multi-scale observations of dense core G205.46-14.56-N2 show a quadruple protostellar system whose symmetry, outflows, and kinematics match simulations of rotational fragmentation, providing the first claimed evidence for this pathway in high-order multiples.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25158","ref_index":39,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Early phases of star formation with SKAO: synchrotron emission from dense starless cores in molecular clouds","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T20:45:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25077","ref_index":145,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Small-scale Magnetic Fields in the Milky Way and Nearby Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T18:35:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"Review chapter summarizing the importance of small-scale galactic magnetic fields and proposing SKA observation strategies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23802","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Characterising magnetic fields at the onset of star cluster formation: From giant molecular clouds to infrared dark clumps","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Polarization observations reveal scale-dependent differences in magnetic field morphology between molecular clouds and clumps, a velocity-dispersion correlation, and unreliable field-strength estimates that contradict flux conservation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"pseudovector angles, this is expected from what we can see in the distributionsinFigure2andourobservationsthatthePlanck𝐵-field tends to align strongly with the Galactic plane, while the POL-2 𝐵-field varies much more. The turbulent-to-total magnetic field strength ratio⟨𝐵 2 𝑡 ⟩ ⟨𝐵 2 POS ⟩ can be calculated using: ⟨𝐵2 𝑡 ⟩ ⟨𝐵2 POS⟩ = 1 1+ \u0010 ⟨𝐵 2 𝑡 ⟩ ⟨𝐵 2𝑜 ⟩ \u0011 −1 (11) According to Houde et al. (2009), the number of turbulent cells along the LOS,𝑁, should be calculated using the equation 𝑁= 𝛿2 +2𝑊 2\u0001 Δ′ √ 2𝜋𝛿 3 (12) whereΔ ′ istheLOSdepthofthecloud.Anothermethodtocalculate thenumberofturbulentcellsalongtheLOS,𝑁 LOS,waspresentedby Cho & Yoo (2016) - this method estimates𝑁LOS =( 𝛿𝑣 𝛿𝑉𝑐 )2, where 𝛿𝑣is the turbulent line-of-sight velocity dispersion and𝛿𝑉𝑐 is the"},{"citing_arxiv_id":"2606.22090","ref_index":125,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Measuring Magnetic Field Strengths in Galactic Star-forming Regions via the Zeeman Effect with the SKA","primary_cat":"astro-ph.GA","submitted_at":"2026-06-20T15:16:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The paper presents predictions and observational plans for Zeeman effect measurements with SKA to provide statistical data on magnetic field strengths across scales in molecular clouds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11359","ref_index":40,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Imprints of the Neutral Interstellar Medium on Polarized Synchrotron Emission and Faraday Rotation","primary_cat":"astro-ph.GA","submitted_at":"2026-06-09T18:38:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Correlations between HI velocity complexity and depolarization plus links between Faraday depth moments and neutral gas structure indicate neutral-dominated ISM regions contribute substantially to diffuse synchrotron emission and Faraday rotation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04713","ref_index":74,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Statistical analysis of the relative orientations between filaments and magnetic fields using Herschel and Planck data in star-forming regions","primary_cat":"astro-ph.GA","submitted_at":"2026-06-03T10:46:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Low-column-density filaments align parallel to magnetic fields while high-column-density wide filaments align perpendicular, with transition at roughly 0.8-8 x 10^21 cm^-2; projection effects analyzed statistically.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21101","ref_index":25,"ref_count":1,"confidence":0.9,"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":165,"ref_count":1,"confidence":0.9,"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":"2605.17708","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"BISTRO Survey: Gravity-Dominated and Magnetically Regulated Star Formation in M17 SW","primary_cat":"astro-ph.GA","submitted_at":"2026-05-18T00:07:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"High-resolution magnetic field maps of M17 SW reveal gravity-dominated energy budget with magnetic fields regulating collapse and accretion channels in a near-equipartition state.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12604","ref_index":82,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"SIMPLIFI -- Study of Interstellar Magnetic Polarization: a Legacy Investigation of Filaments. I. Magnetically-Guided Accretion onto the DR21 Ridge","primary_cat":"astro-ph.GA","submitted_at":"2026-05-12T18:00:07+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Magnetic fields remain aligned with projected gravity throughout the DR21 ridge and sub-filaments, indicating guided accretion at rates that can build the ridge in about one million years.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05377","ref_index":220,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Impact of Radiation Environment on the Evolution and Fragmentation of Protostellar Discs","primary_cat":"astro-ph.SR","submitted_at":"2026-05-06T19:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Stronger radiation environments produce more massive, hotter protostellar discs whose fragments are large and disruptive rather than planetary-mass.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.09770","ref_index":55,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Magnetic field alignment with dense cores in the transition between cloud and core scales","primary_cat":"astro-ph.GA","submitted_at":"2026-04-10T18:00:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Core-scale magnetic fields in star-forming regions are more disordered than cloud-scale fields and align randomly with core orientations and velocity gradients.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2501.10280","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Evidence for the gravity-driven and magnetically-regularized gas flows feeding the massive protostellar cluster in Cepheus A","primary_cat":"astro-ph.GA","submitted_at":"2025-01-17T16:15:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"High-resolution dust polarization and C18O observations in Cepheus A show gravity driving gas accretion while magnetic tension regulates turbulence, producing ordered flows at 2.1e-4 solar masses per year with coherent B-field alignment across scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}