Anders Johansen
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View article: Magnetohydrodynamic simulation assessment of a potential near-ultraviolet early ingress in WASP-189b
Magnetohydrodynamic simulation assessment of a potential near-ultraviolet early ingress in WASP-189b Open
Context . Ultra-hot Jupiters (UHJs) in close orbits around early-type stars provide natural laboratories for studying atmospheric escape and star-planet interactions under extreme irradiation and wind conditions. The near-ultraviolet (NUV)…
View article: How stellar mass and disc size shape the formation and migration of super-Earths
How stellar mass and disc size shape the formation and migration of super-Earths Open
The occurrence rate of close-in super-Earths is higher around M-dwarfs compared to stars of higher masses. In this work, we aim to understand how the super-Earth population is affected by the stellar mass, the size of the protoplanetary di…
View article: The cosmic journey of dust grains – from nucleation to planetary system
The cosmic journey of dust grains – from nucleation to planetary system Open
Dust is essential to the evolution of galaxies and drives the formation of planetary systems. The challenge of inferring the origin of different pre-solar dust grains from meteoritic samples motivates forward modelling to understand the co…
View article: Formation of Planetesimals in the Outer Solar System
Formation of Planetesimals in the Outer Solar System Open
The Solar System hosts the most studied and best understood major and minor planetary bodies - and the only extraterrestrial bodies to have been visited by spacecraft. The Solar System therefore provides important constraints on both the i…
View article: Sublimating exocomets in the PDS 70 system
Sublimating exocomets in the PDS 70 system Open
Young star systems are used to study ongoing or recent planet formation processes, by observations of protoplanets, gas, and planetesimals in their disks. The young protostar PDS 70 hosts two gas giant planets and a disk containing gas and…
View article: Devolatilization during pebble accretion: A hybrid pathway in forming terrestrial planets
Devolatilization during pebble accretion: A hybrid pathway in forming terrestrial planets Open
Earth and Mars are both depleted in moderately volatile elements with sublimation temperatures between 400 K and 1300 K, such as F, Na and Li. A similar depletion pattern is observed in the spectra of both white dwarfs and Sun-like stars s…
View article: Devolatilization during rocky planet formation: Bridging theories and observations
Devolatilization during rocky planet formation: Bridging theories and observations Open
Devolatilization — depletion of volatile elements (e.g., C, O, N, S, Na and K) in rocky planets relative to their host stars — is a common feature that has been observed in both the Solar System and exoplanet systems. Competing mechanisms …
View article: Burned to ashes: How the thermal decomposition of refractory organics in the inner protoplanetary disc impacts the gas-phase C/O ratio
Burned to ashes: How the thermal decomposition of refractory organics in the inner protoplanetary disc impacts the gas-phase C/O ratio Open
The largest reservoir of carbon in protoplanetary discs is stored in refractory organics, which thermally decompose into the gas phase at the organics line located well into the interior of the water iceline. Because this region is so clos…
View article: The cosmochemistry of planetary systems
The cosmochemistry of planetary systems Open
View article: A primordial radius valley as a consequence of planet formation
A primordial radius valley as a consequence of planet formation Open
The radius distribution of close-in planets has been observed to have a bimodal distribution, with a dearth of planets around ~1.5–2.0 R ⊕ commonly referred to as the ‘radius valley’. The origin of the valley is normally attributed to mass…
View article: The influence of dust growth on the observational properties of circumplanetary discs
The influence of dust growth on the observational properties of circumplanetary discs Open
Dust growth is often indirectly inferred observationally in star-forming environments, is theoretically predicted to produce millimetresized particles in circumstellar discs, and has also acted on the predecessors of the terrestrial meteor…
View article: A primordial radius valley as a consequence of planet formation
A primordial radius valley as a consequence of planet formation Open
The radius distribution of close-in planets has been observed to have a bimodal distribution with a dearth of planets around ~1.5-2.0 $R_\oplus$ commonly referred to as the ''radius valley''. The origin of the valley is normally attributed…
View article: The evolution of the flux-size relationship in protoplanetary discs by viscous evolution and radial pebble drift
The evolution of the flux-size relationship in protoplanetary discs by viscous evolution and radial pebble drift Open
In this paper we study the evolution of radiative fluxes, flux radii and observable dust masses in protoplanetary discs, in order to understand how these depend on the angular momentum budget and on the assumed heat sources. We use a model…
View article: The influence of dust growth on the observational properties of circumplanetary discs
The influence of dust growth on the observational properties of circumplanetary discs Open
Dust growth is often indirectly inferred observationally in star-forming environments, theoretically predicted to produce mm-sized particles in circumstellar discs, and also presumably witnessed by the predecessors of the terrestrial meteo…
View article: The coexistence of the streaming instability and the vertical shear instability in protoplanetary disks
The coexistence of the streaming instability and the vertical shear instability in protoplanetary disks Open
The vertical shear instability and the streaming instability are two robust sources of turbulence in protoplanetary disks. The former has been found to induce anisotropic turbulence that is stronger in the vertical than in the radial dimen…
View article: The coexistence of the streaming instability and the vertical shear instability in protoplanetary disks: Scale-dependence of dust diffusion
The coexistence of the streaming instability and the vertical shear instability in protoplanetary disks: Scale-dependence of dust diffusion Open
The vertical shear instability and the streaming instability are two robust sources of turbulence in protoplanetary disks. The former has been found to induce anisotropic turbulence that is stronger in the vertical than in the radial dimen…
View article: The evolution of the flux-size relationship in protoplanetary discs by viscous evolution and radial pebble drift
The evolution of the flux-size relationship in protoplanetary discs by viscous evolution and radial pebble drift Open
In this paper we study the evolution of radiative fluxes, flux radii and observable dust masses in protoplanetary discs, in order to understand how these depend on the angular momentum budget and on the assumed heat sources. We use a model…
View article: Effects of reduced tillage on soil health indicators in organic and conventional agricultural systems
Effects of reduced tillage on soil health indicators in organic and conventional agricultural systems Open
View article: UV processing of icy pebbles in the outer parts of VSI-turbulent disks
UV processing of icy pebbles in the outer parts of VSI-turbulent disks Open
Icy dust particles emerge in star-forming clouds and are subsequently incorporated in protoplanetary disks, where they coagulate into larger pebbles up to millimeter in size. In the disk midplane, ices are shielded from UV radiation, but m…
View article: Plant growth-promoting bacteria and nanomaterials synergism to enhance Lolium perenne growth and phytoremediation in cadmium-contaminated soil
Plant growth-promoting bacteria and nanomaterials synergism to enhance Lolium perenne growth and phytoremediation in cadmium-contaminated soil Open
Innovative integrated approaches of nanoparticles (NP) and plant growth-promoting bacteria (PGPB) can accelerate plant growth and remediation of cadmium (Cd) contaminated soil. The effectiveness of the combination and interactions amongst …
View article: UV-processing of icy pebbles in the outer parts of VSI-turbulent disks
UV-processing of icy pebbles in the outer parts of VSI-turbulent disks Open
Icy dust particles emerge in star-forming clouds and are subsequently incorporated in protoplanetary disks, where they coagulate into larger pebbles up to mm in size. In the disk midplane, ices are shielded from UV radiation, but moderate …
View article: Comment on "Did the terrestrial planets of the Solar System form by pebble accretion?"
Comment on "Did the terrestrial planets of the Solar System form by pebble accretion?" Open
Morbidelli, Kleine & Nimmo (2024) (MKN) recently published a critical analysis on whether the terrestrial planets in the Solar System formed by rapid pebble accretion or by the classical route of multiple giant impacts between planetary em…
View article: Verifying Machine Unlearning with Explainable AI
Verifying Machine Unlearning with Explainable AI Open
We investigate the effectiveness of Explainable AI (XAI) in verifying Machine Unlearning (MU) within the context of harbor front monitoring, focusing on data privacy and regulatory compliance. With the increasing need to adhere to privacy …
View article: Large Interferometer For Exoplanets (LIFE)
Large Interferometer For Exoplanets (LIFE) Open
Context . The increased brightness temperature of young rocky protoplanets during their magma ocean epoch makes them potentially amenable to atmospheric characterization at distances from the Solar System far greater than thermally equilib…
View article: Large Interferometer For Exoplanets (LIFE). XIV. Finding terrestrial protoplanets in the galactic neighborhood
Large Interferometer For Exoplanets (LIFE). XIV. Finding terrestrial protoplanets in the galactic neighborhood Open
The increased brightness temperature of young rocky protoplanets during their magma ocean epoch makes them potentially amenable to atmospheric characterization to distances from the solar system far greater than thermally equilibrated terr…
View article: Evolution of gas envelopes and outgassed atmospheres of rocky planets that formed via pebble accretion
Evolution of gas envelopes and outgassed atmospheres of rocky planets that formed via pebble accretion Open
In this work, we present results of numerical simulations of the formation and early evolution of rocky planets through pebble accretion, with an emphasis on hydrogen envelope longevity and the composition of the outgassed atmosphere. We m…
View article: Thousands of planetesimals: Simulating the streaming instability in very large computational domains
Thousands of planetesimals: Simulating the streaming instability in very large computational domains Open
The streaming instability is a mechanism whereby pebble-sized particles in protoplanetary discs spontaneously come together in dense filaments, which collapse gravitationally to form planetesimals upon reaching the Roche density. The exten…
View article: Thousands of planetesimals: Simulating the streaming Instability in very large computational domains
Thousands of planetesimals: Simulating the streaming Instability in very large computational domains Open
The streaming instability is a mechanism whereby pebble-sized particles in protoplanetary discs spontaneously come together in dense filaments, which collapse gravitationally to form planetesimals upon reaching the Roche density. The exten…
View article: Evolution of gas envelopes and outgassed atmospheres of rocky planets formed via pebble accretion
Evolution of gas envelopes and outgassed atmospheres of rocky planets formed via pebble accretion Open
We present here results of numerical simulations of the formation and early evolution of rocky planets through pebble accretion, with an with an emphasis on hydrogen envelope longevity and the composition of the outgassed atmosphere. We mo…
View article: Self-oxidation of the atmospheres of rocky planets with implications for the origin of life
Self-oxidation of the atmospheres of rocky planets with implications for the origin of life Open
Rocky planets may acquire a primordial atmosphere by outgassing of volatiles from their magma ocean. The distribution of O between H$_2$O, CO and CO$_2$ in chemical equilibrium subsequently changes significantly with decreasing temperature…