![Schematics of a HAeBe star accreting material from its protoplanetary disc with an ongoing giant planet formation. The giant planet opens a disc gap, preventing the larger dust grains from moving inwards. The HAeBe star has a convective core (red), a radiative envelope (blue), and the stellar photosphere (yellow).-- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/The-refractory.png?resize=1200%2C718&ssl=1)
[astro-ph.EP] Context. Phosphorus (P) is an essential element for life on Earth and a potential tracer of planet formation history. However, there has been no detection of P-bearing molecules in […]
Protoplanetary Disk
![[LEFT] The MIRI F2100W observation of the HD 107146 system, shown in logarithmic scaling with the corresponding intensity levels indicated in the colorbar. [RIGHT] Contours from the ALMA observations obtained within the ARKS program (S. Marino et al. 2026), overlaid on the combined F182M and F210M JWST/NIRCam observations for HD 107146. -- [astro-ph.SR]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/The-JWSTNIRCam.png?resize=1200%2C720&ssl=1)
Posted inAstrogeology
The JWST/NIRCam Scattered Light Disks GTO 2780 program: Panchromatic coronagraphic imaging of the HD 10647, HD 32297, HD 61005, HD 107146, and HD 181327 debris disk systems
[astro-ph.SR]. Debris disks, composed of rocks, boulders, planetesimals, and the dust produced in their collisions, present the most readily observable components of mature planetary systems.
![HAADF image and quantified EDX map (at%) of a GEMS-like assemblage in UCAMM DC06- 18, which is located at the top of the FIB section, probably close to the external surface of the UCAMM. - [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/STXM-XANES.png?resize=1200%2C711&ssl=1)
Posted inMeteorites & Asteroids
STXM-XANES And TEM Analysis Of UltraCarbonaceous Antarctic MicroMeteorites (UCAMMs)
[astro-ph.EP] The Concordia micrometeorite collection contains UltraCarbonaceous Antarctic MicroMeteorites (UCAMMs) of probable cometary origin. Eight FIB sections of UCAMMs were studied by Scanning Transmission X-ray Microscopy – X-ray Absorption Near […]
Posted inExoplanets, -moons, -comets
JWST Reveals A Race Against Time For Forming Planets
[SETI Institute] Planets form from disks of gas and dust around young stars, but the gas needed for growth does not last forever. New observations from NASA’s James Webb Space […]
![LOCO-CV predicted vs DFT binding energies for 13 adsorbate species on ASW12 clusters. Each point represents a single adsorbate–surface configuration, coloured by species identity; asterisks denote radical species. Pooled metrics across all leave-one-cluster-out folds: R2 = 0.896, RMSE = 574 K, MAE = 378 K. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/AstroBind.png?resize=1200%2C715&ssl=1)
Posted inAstrochemistry
AstroBind: Machine Learning Prediction Of Binding Energy Distributions On Interstellar Water Ice From Geometric Surface Descriptors
[astro-ph.GA] Binding energies on amorphous solid water regulate molecular desorption in molecular clouds and protoplanetary disks, but computing them from first principles across the heterogeneous binding sites of disordered ice […]
![Sunburst diagrams describing the evolution of the inner planets (top) and the outer giant planets (bottom) in the DAG simulations. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/Effects-of.png?resize=1200%2C717&ssl=1)
Posted inExoplanets, -moons, -comets
Effects Of Outer Giant Planets On In Situ Formation Of Inner Super-Earths
[astro-ph.EP] Recent studies have found an observational correlation between the presence of outer giant planets and inner super-Earths, which implies that outer giants do not suppress the formation of super-Earths.
Posted inExoplanets, -moons, -comets
ADORA: A Differentiable Optical Modeling And Astrometric Retrieval Framework For SHERA
[astro-ph.EP] Motivated by recent observations suggesting rings found in debris disks are wider than those in protoplanetary disks, we consider a picture in which planetesimals formed in radially narrow dust […]
![The timescale required for a 10 M⊕ring of planetesimals around a 1 M⊙ star to radially diffuse 0.1 M⊕ into the inner 0.5 au. The planetesimal density is assumed to be 4 g cm−3 . The black dashed line shows the boundary where the inner edge is just reachable by the radially diffusing disk, below which the escape velocity is less than the critical escape velocity (v0.5au) and planetesimals are not deliverable at this level. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/Substructure.png?resize=1200%2C715&ssl=1)
Posted inExoplanets, -moons, -comets
Substructure Evolution From Protoplanetary To Debris Disks Driven By Mutually Gravitating Planetesimals And Implications On Kepler Resonances And Free-floating Planets
[astro-ph.EP]. Motivated by recent observations suggesting rings found in debris disks are wider than those in protoplanetary disks, we consider a picture in which planetesimals formed in radially narrow dust […]
![Mechanisms that contribute to dust growth just beyond the snow line. Many-seed icy aggregates grow in the outer disk’s regions due to the high sticking efficiency of water ice and disintegrate as they cross the water snow line (green-to-blue interface) into silicate monomers and water vapor. Both diffuse back across the snow line due to turbulence, facilitating further accumulation of icy water and the growth of icy aggregates just behind the snow line, effects found in our numerical model as well (see Figs. 7 and E.2).-- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/Hydrodynamics.png?resize=1200%2C721&ssl=1)
Posted inAstrogeology
Hydrodynamics Modeling Of The Water Snow Line In Young Protoplanetary Disks With Dust-size-dependent Opacities
[astro-ph.EP] Aims. We investigated the properties of the water snow line during the early stages of disk evolution, paying particular attention to the effects of gravitational instability and dust growth […]
![Ni, Cu and Zn elemental maps of three chondrules from Paris, that show microspherule regions partitioned by zones enriched in siderophile elements (i.e., Fe, Ni, Co, Cu; pink arrows). The color bars reflect μg/g concentrations of the elements. While in BSE mode and lithophile element space, these would appear as single ~300 μm diameter chondrules, they represent aggregates of ~100 μm grape-bunch chondrules (pink spheres), where these microchondrules contained metal-rich rims. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/Chondrule.png?resize=1200%2C714&ssl=1)
Posted inAstrogeology
Chondrule Formation In The Outer Disk From The Primary Three-dimensional Chemical Composition Of CM Chondrules
[astro-ph.EP] Chondrules and their associated fine-grained rims record key processes in the early protoplanetary disk, yet the links between chondrule chemistry, morphology, and matrix complementarity remain poorly constrained.