JWST data on 3C305 shows the compact radio jet efficiently drives kiloparsec-scale multiphase outflows via shocks, with high coupling to the observed gas kinetic power and radiative losses.
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Nominal values for selected solar and planetary quantities: IAU 2015 Resolution B3
30 Pith papers cite this work. Polarity classification is still indexing.
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abstract
In this brief communication we provide the rationale for, and the outcome of the International Astronomical Union (IAU) resolution vote at the XXIX-th General Assembly in Honolulu, Hawaii, in 2015, on recommended nominal conversion constants for selected solar and planetary properties. The problem addressed by the resolution is a lack of established conversion constants between solar and planetary values and SI units: a missing standard has caused a proliferation of solar values (e.g., solar radius, solar irradiance, solar luminosity, solar effective temperature and solar mass parameter) in the literature, with cited solar values typically based on best estimates at the time of paper writing. As precision of observations increases, a set of consistent values becomes increasingly important. To address this, an IAU Working Group on Nominal Units for Stellar and Planetary Astronomy formed in 2011, uniting experts from the solar, stellar, planetary, exoplanetary and fundamental astronomy, as well as from general standards fields to converge on optimal values for nominal conversion constants. The effort resulted in the IAU 2015 Resolution B3, passed at the IAU General Assembly by a large majority. The resolution recommends the use of nominal solar and planetary values, which are by definition exact and are expressed in SI units. These nominal values should be understood as conversion factors only, not as the true solar/planetary properties or current best estimates. Authors and journal editors are urged to join in using the standard values set forth by this resolution in future work and publications to help minimize further confusion.
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Magnetized disk models lower the thermal-viscous instability threshold to Eddington ratios of 0.01-0.03 and yield limit-cycle timescales of months to years, jointly matching observations in five CLAGN only when the inner disk is strongly magnetized.
Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.
First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.
Bayesian framework with active-learning surrogate for MESA models constrains ages and α_MLT from 38 main-sequence DEBs, recovering some α_MLT values below the solar calibration.
An agnostic model using genetic algorithm optimization predicts photosynthetic viability declines linearly with orbital distance, expanding the photosynthetic habitable zone for M, K, and G stars beyond Earth-centric estimates.
A PINN approach learns galactic gravitational potentials from acceleration data, achieving sub-percent errors on simulations while outperforming analytic models and retaining interpretability via structured priors.
PRFM-vol is a new subgrid star formation model for cosmological simulations that computes SFR from ambient densities via PRFM theory and a modified effective EOS, producing taller stellar scale heights, slightly higher stellar mass, and morphology changes including Toomre-driven clumps compared to p
Medium-band imaging reveals red emission-line galaxies at z>5 including compact objects likely missed by classic Little Red Dot selection criteria.
Massive galaxies at z>3.5 assembled stars earlier than theoretical models predict and exhibit gray dust attenuation, especially at the highest masses.
Corrected empirical limits show the most massive galaxies never exceed the theoretical baryonic maximum of 0.16 times halo virial mass, keeping observations consistent with LambdaCDM at all redshifts.
Updated RM modeling framework in TLCM validated on nine systems and applied to TOI-135 to measure sky-projected obliquity λ = 55.6° with ~11° uncertainties.
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.
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.
A conditional variational autoencoder is trained on public kilonova light curves to enable rapid parameter inference for binary neutron star merger models in under three hours total.
Observational study of 100 LMC GMCs finds median 13CO(2-1)/12CO(2-1) line ratio of 0.078, nearly linear with luminosity, and higher in clouds hosting IR-bright young stellar objects.
Observational analysis of 21 giant stars shows Fe I+Fe II blend emission proportional to Ca II K with matching Teff power-law exponent and a slope break in the flux ratio at log g ≈ 2.5.
50 constrained simulations of Coma cluster analogues reproduce the observed radial X-ray surface brightness and Compton-y profiles within the scatter expected from environment and assembly history.
Bayesian fitting of an eccentric Keplerian orbit to the radio light curve of PKS 2131-021 gives e = 0.053 ± 0.015 without red noise but favors a circular orbit plus DRW noise with e < 0.15.
Reports results from two searches for new radio lenses in existing surveys and discusses the completeness of the population usable for constraining dark matter properties via astrometric perturbations.
JWST finds infrared counterparts for nearly all micro-Jy radio sources, with star formation explaining the radio output in roughly 79% of cases after accounting for non-linear luminosity relations.
Late-time radio rebrightening in SN 2012ap is consistent with either progenitor mass-loss variation producing a density enhancement or an off-axis energetic jet viewed at large angle, potentially reclassifying it as GRB-like rather than weakly engine-driven.
A single galaxy cluster lenses two quasars (one Type I at z=1.524, one dust-obscured Type II at z=1.939) into four images each, yielding a projected mass of ~3.3e14 solar masses within 500 kpc and time delays of hundreds to over 1000 days.
SSL model detects galaxy interaction signatures with recall 0.86 and low contamination while CAS at A>0.35 has recall 0.20 but higher precision, benchmarked on visual classification of 25.1% disturbed fraction.
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