The physical origin of the large cavities observed in transition disks remains unclear. This work analyzes multi-wavelength interferometric dust continuum observations to constrain the radial profiles of dust surface density, maximum grain size, and temperature, providing insights into the potential mechanisms responsible for the formation of these cavities.
By numerically integrating the trajectories of known interstellar objects like 'Oumuamua, Borisov, and IM1 in the gravitational potential of the Milky Way, the study constrains the likely birthplaces and ages of these objects within the Galaxy.
The ultraviolet luminosity functions of galaxies spanning redshift 4 to 10 provide insights into galaxy evolution, the epoch of reionization, and cosmological parameters such as the amplitude of matter perturbations (σ8).
Gravity torques exerted by bars and spirals efficiently drive gas infall towards the centers of Milky Way-like galaxies, fueling supermassive black holes and central star formation.
Varying the initial mass function and orbital parameter distributions significantly impacts the predicted rates and properties of compact object mergers, especially for black hole-black hole mergers, across cosmic time.
The HD 169142 protoplanetary disk exhibits only moderate depletion of volatile carbon and oxygen compared to their interstellar abundances, with the inner disk appearing enriched in volatile oxygen. The gas-phase sulfur abundance is heavily depleted by a factor of ~1000. Emission from SiS near the embedded protoplanet HD 169142 b vastly exceeds model predictions, suggesting its origin in shocked gas or a localized outflow.
The TODDLERS emission library, a physically motivated model of UV-mm emission from star-forming regions, is used to generate synthetic observations of 30 Milky Way-like galaxies from the Auriga simulation suite. The results demonstrate the potential of TODDLERS to improve the fidelity of simulated galaxy properties compared to existing sub-grid models.
Strongly warped accretion disks around black holes can undergo extreme vertical oscillations, leading to the formation of "nozzle shocks" that rapidly damp the warp and drive fast accretion.
The polarization of black hole jets exhibits distinct swings at characteristic distances from the black hole, which are strongly tied to the location of the light cylinder and thus the black hole's spin. Measuring these polarization swings provides a new method to infer the spin of black holes.
The authors propose a novel method to reconstruct the full posterior distribution of the star formation histories (SFHs) of galaxies from broad-band photometry using simulation-based inference (SBI) with a neural network trained on the Horizon-AGN hydrodynamical simulation.