HD163296 Archives

Dynamical excitation of the planetesimal disk at 0.75, 2 and 5 Myr in the four simulated scenarios. Dynamical excitation accounts for the contributions of both eccentricity and inclination and is defined as p e 2 + sin2 (i) (Petit et al. 2001). The colour bar indicates the region in the disk from which the planetesimals originated (in units of au). The dashed grey line at 40 au indicate the division between inner and outer disk. The rectangles in the rightmost panels mark the “fountain” feature we refer to in the main text, i.e. the damping of the orbital eccentricities of the excited planetesimals by aerodynamic drag that creates the implanted planetesimals. The light blue filled circles indicate the location of the four simulated planets in the disk. First row: High Disk Mass - High Planetary Mass; Second row: High Disk Mass - Low Planetary Mass; Third row: Low Disk - High Planetary Mass; Fourth row: Low Disk Mass - Low Planetary Mass -- astro-ph.EP

Astrochemistry, Astrogeology, Biochemistry & Organic Chemistry, Biogeochemical Cycles & Geobiology, Biosignatures & Paleobiology, Brown Dwarfs, Comets and Asteroids, Exoplanets, -moons, -comets, Gas Giants, Icy Worlds, Imaging & Spectroscopy, Interstellar, Status Report

HD 163296 And Its Giant Planets: Creation Of Exo-comets, Interstellar Objects And Transport Of Volatile Material

by Keith CowingMarch 11, 2025March 11, 2025

The birth of giant planets in protoplanetary disks is known to alter the structure and evolution of the disk environment, but most of our knowledge focuses on its effects on […]

HD163296

HD 163296 And Its Giant Planets: Creation Of Exo-comets, Interstellar Objects And Transport Of Volatile Material

Curiosity Mars Rover Discovers A Field Of Honeycomb Textures

Viking Science

Constraining The Lives And Times Of Exoplanets Through Evolutionary Bayesian Retrievals

Project Hephaistos — III. Characterizing Anomalous Infrared Sources Identified As Dyson-sphere Candidates

SCoRE: The Surface Composition Of Rocky Exoplanets