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.
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Protostars and Planets VI , archivePrefix = "arXiv", eprint =
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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.
Water binding energy on silicate grains is twice that on ice, enabling local retention and inheritance for terrestrial planets without outer Solar System delivery.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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SIMPLIFI -- Study of Interstellar Magnetic Polarization: a Legacy Investigation of Filaments. I. Magnetically-Guided Accretion onto the DR21 Ridge
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.
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Numerical simulations of shock-driven, supersonic turbulence in colliding three-temperature laboratory plasmas
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.