{"total":13,"items":[{"citing_arxiv_id":"2607.00080","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"White dwarf planets in star clusters: gravitational scattering versus mass-loss effects","primary_cat":"astro-ph.EP","submitted_at":"2026-06-30T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"N-body simulations find stellar mass-loss effects dominate gravitational scattering in altering giant planet orbits around white dwarfs formed in star clusters, independent of density and initial conditions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31477","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multi-wavelength Emission Modeling from Accretion Flows around Isolated Black Holes Including Magnetic Flux Transport","primary_cat":"astro-ph.HE","submitted_at":"2026-06-30T10:53:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A 1D accretion model shows MAD formation for Pm ≳ 1, outer-disk IR emission missed by one-zone approximations, and Pm-dependent X-ray mechanisms that affect IBH detectability in dense clouds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26320","ref_index":234,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Probing the molecular gas content of galaxies in an over-dense group at z~0.7: a test case for environmental quenching","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T19:06:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"CO observations of the COSMOS-Gr30 group at z~0.7 show average molecular gas contents reduced by 0.5 dex relative to field galaxies, with gas fractions 20-40% of main-sequence values, plus an upper limit on cold gas in the extended ionized structure.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09979","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Planet or brown dwarf? Constraints on the formation of H-type objects in IC348","primary_cat":"astro-ph.EP","submitted_at":"2026-06-08T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"H-type objects in IC348 show spatial distributions matching stars and brown dwarfs, unlike the more dispersed distribution of simulated ejected planets, indicating a star-like formation origin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03261","ref_index":118,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A nine-member protostellar system forming via filament fragmentation in the high mass protocluster NGC 6334-43","primary_cat":"astro-ph.GA","submitted_at":"2026-06-02T07:25:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Serendipitous discovery of a bound nine-member protostellar system in NGC 6334-43 formed by filament fragmentation, with outflows from two sources and virial masses derived for three cores.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21672","ref_index":36,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Numerical simulations of shock-driven, supersonic turbulence in colliding three-temperature laboratory plasmas","primary_cat":"physics.plasm-ph","submitted_at":"2026-05-20T19:25:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Three-dimensional three-temperature simulations of colliding supersonic plasma flows from irradiated CH mesh targets produce a persistent shocked turbulent mixing layer that evolves toward an isothermal state with anisotropic Reynolds stress and effective Reynolds number around 200.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(a) Total spectrum,P u(k)/⟨u2⟩k −5/3. (b) Solenoidal and compressive spectra,P s(k) andP c(k). (c) Scale-dependent spectral ratio,P c(k)/Ps(k). At late time, the solenoidal component is energetically dominant over most resolved scales, while the rise at the largestkmarks numerical dissipation. 19 velocity field,δu i =u i − ⟨ui⟩V, Pij(k)≡ ˆ Ωk fδui(k)gδuj ∗ (k)k 2dΩk,(36) whose diagonal components,P xx(k),P yy(k), and Pzz(k), give the component-wise power spectra. From these we form the shell-wise anisotropy tensor bij(k) = Pij(k) tr[Pij(k)] − 1 3 δij,tr[P(k)] = X i Pii(k), (37) and characterize its shape through the invariants (I 2, I3). In the present analysis the off-diagonal shell contri- butions are neglected, so thatb ij(k) is approximated as"},{"citing_arxiv_id":"2605.14693","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Discovery of a Compact Hub-Filament System in G286.21+0.17 with JWST and ALMA: Insights into Protocluster Formation and Competitive Accretion","primary_cat":"astro-ph.GA","submitted_at":"2026-05-14T11:09:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multi-wavelength observations identify a compact hub-filament system in G286.21+0.17 whose core properties follow steep radial power laws consistent with competitive accretion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12604","ref_index":3,"ref_count":1,"confidence":0.88,"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":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"ℓ ·ln(r ini/r) \u00151/2 =−3.5 km s −1 · \u0012 M/ℓ 103 M⊙ pc−1 \u00131/2 · \u0012 ln \u0014 rini/r 2 \u0015\u00131/2 =−4.1 km s −1 · \u0012 M/ℓ 103 M⊙ pc−1 \u00131/2 ·J(r/r ini) (D11) (Heitsch 2013), assuming test particles start with zero inward velocity at the initial radiusr ini. The function J(r/r ini) = (ln[rini/r])1/2 (D12) 28 achieves valuesJ(x) = [1.52,1.23,1.10,0.96,0.83] at atx=r/r ini = [0.1,0.2,0.3,0.4,0.5], makingJ≈1 a good approximation for a range of situations. GivenM/ℓ≈4×10 3 M⊙ pc−1 (Sec. 2.4), free-fall velocitiesv≈ −8 km s −1 thus represent a meaningful characteristic infall speed for the DR21 Main Ridge. Free-fall motion following Eq. (D11) from a starting pointr ini to an end pointrtakes a transit timet trans =− R r rini dr′/v(r′), which evaluates to"},{"citing_arxiv_id":"2605.02637","ref_index":45,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Astrochemical Inheritance of Terrestrial Planets Water from Local Wet Silicates","primary_cat":"astro-ph.EP","submitted_at":"2026-05-04T14:21:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Water binding energy on silicate grains is twice that on ice, enabling local retention and inheritance for terrestrial planets without outer Solar System delivery.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00510","ref_index":71,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Scale-Aware Adversarial Analysis: A Diagnostic for Generative AI in Multiscale Complex Systems","primary_cat":"cs.LG","submitted_at":"2026-05-01T08:36:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A new scale-aware diagnostic framework shows that unconstrained diffusion generative models exhibit structural freezing and instability instead of smooth physical responses under multiscale perturbations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.27584","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dense cores and filaments in M16: Enhanced formation efficiency in the stellar feedback-driven shell","primary_cat":"astro-ph.GA","submitted_at":"2026-04-30T08:38:24+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Filament formation efficiency rises by a factor of 2.3 and core density by 1.5 inside the feedback-driven shell in M16, with fragmentation timescales matching the shell age and supporting positive feedback.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19413","ref_index":171,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Oort Cloud Ecology -- IV. Exchanging Asteroids","primary_cat":"astro-ph.EP","submitted_at":"2026-04-21T12:45:16+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19097","ref_index":117,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Investigation of Hourglass-shaped Magnetic fields in the G35.20-0.74 Star-Forming Complex","primary_cat":"astro-ph.GA","submitted_at":"2026-04-21T05:23:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"New observations confirm hourglass magnetic fields at clump scales in G35.20-0.74, with strengths of approximately 600 μG in G35N and 850 μG in G35S, supporting magnetically regulated collapse in G35N and feedback influence in G35S.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}