Transient Faraday-complex spectropolarimetric structure detected during radio flaring of Swift J1727 implies internal Faraday rotation from electron-proton jet plasma with rotating mass ~10^21 g, a small fraction of accreted mass.
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JWST/MIRI survey of 2-6 Myr Upper Scorpius disks finds diverse chemotypes, 10-1000x lower water luminosities, and evidence that outer dust traps control inner-disk chemistry.
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Steady GRMHD jets exhibit a universal near-horizon polarization pattern set only by black hole spin, with large-radius polarization angle following a collimation-determined power law and intermediate scales modified by plasma loading.
Machine learning on simulated images identifies that flux eruption events cause more diffuse, polarized, lower-flux millimeter emission with decreased Q-U loop rotation rate, achieving ~80% accuracy with random forests on summary statistics.
VLBI observations of TXS 0506+056 show a spine-sheath jet with aligned inner and perpendicular outer EVPAs plus a new superluminal component near the IceCube neutrino detection.
Observations of the HK Tau binary with JWST reveal gas-phase molecular lines in the low-inclination primary and ice absorption features in the edge-on secondary, enabled by their differing inclinations.
Slim-disk self-shadowing plus accretion-rate-dependent BLR density enhancement explains the observed offsets of high-Eddington AGNs below the canonical R-L relation.
3D RMHD simulations with hybrid particle tracking reproduce the weak radio and strong X-ray redshift evolution in AGN jets via IC/CMB, including the (1+z)^4 X-ray scaling and the alpha-z relation.
Magnetically-driven protostellar jets transport sufficient angular momentum outward to prevent massive protostars from reaching critical rotation speeds, with jet strength linked to initial formation conditions producing a variety of final stellar rotation rates.
MHD wind-driven accretion in protoplanetary disks follows a power-law scaling with midplane plasma beta, effective ambipolar Elsasser number, and active-layer thickness, reproducing simulations to roughly a factor of 2–3 for most runs.
FUor masses inferred from Keplerian line broadening in H-band spectra match the solar neighborhood IMF, indicating a universal eruptive phase during star formation.
YSO jet diversity, including counter-rotating and choked jets, arises from a spine-tower balance controlled by stellar rotation and magnetospheric field strength.
Requiring thin-disk solutions to be thermally stable and single-valued imposes η_x ≡ dlnα/dlnX > 4/7, and a viscosity law α∝X^p with p>4/7 removes the radiation-pressure unstable branch.
Derives B*(d) and N*(d) for AGN jet cores from self-absorbed synchrotron emission model with power-law assumptions on Doppler factor, Lorentz factor, B, and N versus jet width d.
Biconical disk-wind models show that small acceleration length R_v plus high terminal velocity is required to produce detached blueshifted CIV absorption in synthetic spectra at intermediate inclinations.
Citizen science discovery of a bow-and-arrow radio galaxy with ~560 kpc bow-shock-like structure in a multi-halo environment at z=0.159.
Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.
High magnetization and flickering variability in relativistic MHD simulations create asymmetrical cocoons and broken jet morphologies in AGN jets.
Mass-scaled DRW damping timescales in AGNs follow a linear relation with black hole mass (slope 0.35-0.50) for both jetted and non-jetted sources, supporting universal accretion physics.
VLBI imaging detects a compact radio source with Tb > 10^7 K and flat spectrum in the northern core of UGC 2369S, confirming a buried low-luminosity AGN.
A sample of 69 HBLs yields intrinsic radio-X-ray correlation L_R,int ∝ L_X,int^0.68 and fundamental plane log L_R,int = 0.57 log L_X,int + 0.33 log M_BH + 12.65, consistent with synchrotron cooling model for X-ray emission.
Stellar spindown cannot trigger secular resonance crossings in regular peas-in-a-pod systems, requiring inner-planet migration instead, and resonance crossing times vary across stellar evolution tracks.
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Spectropolarimetric detection of baryonic mass loading in a transient relativistic jet: application to the black hole X-ray binary Swift J1727.8$-$1613
Transient Faraday-complex spectropolarimetric structure detected during radio flaring of Swift J1727 implies internal Faraday rotation from electron-proton jet plasma with rotating mass ~10^21 g, a small fraction of accreted mass.
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Chemical Divergence and Water Depletion: Gas Properties of Evolved Upper Scorpius Disks Revealed by JWST/MIRI
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A Retrieval Framework for Observationally Constraining the Parameters of Circumplanetary Disks
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Direct VLBI evidence for a buried AGN in the triple-merger LIRG UGC 2369S
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The Fundamental Planes of Black Hole Activity for High-Synchrotron-Peaked BL Lacertae Objects
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Peas and USPs: Can Stellar Spindown and Peas in a Pod Replicate Ultra-Short-Period Planet Characteristics?
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A 0.03 Hz Radio Quasi-periodic Oscillation During the 2025 Flare of GRS 1915+105
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Spectro-Polarimetric Observations of TeV Sources (SPOTS): First results
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A Synchronized Spin Model for Black-Hole Accretion Systems
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Influence of winds on shocked magnetized viscous accretion flows around rotating black holes
Winds in shocked magnetized viscous accretion flows around rotating black holes reduce luminosity, modify shock radius, compression, and strength, and impose a critical wind parameter p^crit above which steady shocks cease to exist.
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