Interstellar comet 3I/ATLAS is now on its way out of our solar system, never to return.
![[LEFT] Final planet mass vs pebble flux across the snowline at time of insertion. Plots A and B are coloured by the planet’s initial and final semi-major axes respectively. Plot C is coloured by the planet’s insertion time 𝑡0, and plot D is coloured by the characteristic disk radius 𝑅0. Plot E is coloured by the disk’s 𝛼 parameter, and plot F is coloured by the fragmentation velocity 𝑣frag. All plots contain outlined numbered points, which correspond to the points numbered in Fig. 2. [RIGHT Final planet mass vs pebble flux across the snowline at 1 Myr. Plots A and B are coloured by the planet’s final and initial semi-major axes respectively. Plot C is coloured by the planet’s insertion time 𝑡0, and plot D is coloured by the characteristic disk radius 𝑅0. Plot E is coloured by the disk’s 𝛼 parameter, and plot F is coloured by the fragmentation velocity 𝑣frag. All plots contain outlined numbered points, which correspond to the points numbered in Fig. 2. -- astro-ph.EP](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/04/Simulating-the-interplay.png?resize=1200%2C760&ssl=1)
Pebble drift plays a central role in modern planet formation models. In this work we carry out planet formation simulations (including pebble accretion and migration) for a range of disc […]
Protoplanetary disk ice lines shape a multitude of planet formation processes, setting the environmental composition through evolution.
Venus, often called Earth’s twin, is in fact a planet of extremes. Beneath its thick carbon dioxide atmosphere lie crushing surface temperatures and dense clouds of sulfuric acid. While the […]
Although Uranus and Neptune are commonly classified as ice giants, their exact compositions remain poorly constrained. Recent studies of outer Solar System bodies challenge the traditional view that these planets […]
The outgassing signatures of Io, Europa, Enceladus, Triton, and Io-like exomoons are the focus of this review chapter. The rocky volcanic world of Io is unique in our Solar System, […]
The study of meteorites is important for planetary sciences because, among other things, it can provide information about the geochemical composition of their celestial body of origin. Often, subsample preparation […]
Europa’s double ridges often display lower albedo and redder color than their surroundings. Their unique topography may cause sublimation-driven darkening due to illumination and self-heating, a process known as thermal […]
Overview Using a high-resolution atomic force microscope ( AFM ), we directly observed the skeletal structures of individual organic molecules extracted from the Ryugu sample. We discovered numerous gigantic organic […]
![[LEFT] Nano-FTIR measurement of Region 1 (belonging to the aliphatic-rich cluster). Color-coded nano-FTIR spectra (A) of spots shown in the SNOM topography (B), optical amplitude (C), and mechanical amplitude (D) images. [RIGHT] Region 2 (also belonging to the aliphatic-rich cluster). -- PNAS](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/04/Nanoscale-infrared-spectroscopy.png?resize=1200%2C720&ssl=1)
Asteroid Bennu preserves primitive material from the early solar system, and returned samples allow direct examination of how organics and minerals were assembled and altered. We applied nanoscale infrared spectroscopy […]
