Z. M. Leinhardt
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View article: A ‘New Hope’ for Moon formation: presenting a multiple-impact pathway
A ‘New Hope’ for Moon formation: presenting a multiple-impact pathway Open
The leading hypothesis for the origin of the Moon, that of a single giant impact, faces significant challenges. These include either the need for an impactor with a near-identical composition to Earth or an extremely high mass or high ener…
View article: Fractal Aggregate Aerosols in the Virga Cloud Code. I. Model Description and Application to a Benchmark Cloudy Exoplanet
Fractal Aggregate Aerosols in the Virga Cloud Code. I. Model Description and Application to a Benchmark Cloudy Exoplanet Open
We introduce new functionality to treat fractal aggregate aerosol particles within the Virga cloud modeling framework. Previously, the open-source cloud modeling code Virga , the Python version of EddySed , assumed spherical particles to c…
View article: Fractal Aggregate Aerosols in the Virga Cloud Code I: Model Description and Application to a Benchmark Cloudy Exoplanet
Fractal Aggregate Aerosols in the Virga Cloud Code I: Model Description and Application to a Benchmark Cloudy Exoplanet Open
We introduce new functionality to treat fractal aggregate aerosol particles within the Virga cloud modeling framework. Previously, the open source cloud modeling code Virga (Batalha et al. 2025), the Python version of EddySed (Ackerman & M…
View article: Identifying the collisions that make extreme debris disks
Identifying the collisions that make extreme debris disks Open
A subset of debris disks are bright and show evidence of variability on short timescales, flux increasing or decreasing over months/years and in some cases oscillations on timescales of days (e.g. Su et al., 2019). These extreme debris dis…
View article: Analysing Optical Thickness in Simulated Giant Impacts to Determine Observational Signatures of Post-Impact Bodies
Analysing Optical Thickness in Simulated Giant Impacts to Determine Observational Signatures of Post-Impact Bodies Open
IntroductionGiant impacts are a crucial stage of planet formation, capable of altering the properties of planets and the structure of planetary systems [Raymond et al., 2018]. As such, garnering a better understanding of the dynamics of th…
View article: Atmospheric loss during giant impacts: mechanisms and scaling of near- and far-field loss
Atmospheric loss during giant impacts: mechanisms and scaling of near- and far-field loss Open
Introduction: How the Earth and other terrestrial planets acquire their volatile element budgets (e.g., N, C, H, noble gases) remains a fundamental unanswered question. Large fractions of planetary volatiles are believed to have been acqui…
View article: Forming Super-Mercuries by Giant Impact
Forming Super-Mercuries by Giant Impact Open
Exoplanet missions such as Kepler and TESS have been tremendously successful detecting thousands of exoplanets with a diverse range of physical and dynamical parameters. However, even as the number of exoplanets reaches into the many thous…
View article: Asteroids Fail to Retain Cometary Impact Signatures
Asteroids Fail to Retain Cometary Impact Signatures Open
A bombardment of comets is thought to have occurred in the inner solar system as a result of a dynamical instability among the giant planets after gas disk dispersal. Vesta, the second largest asteroid in the main asteroid belt, likely dif…
View article: Atmospheric Loss during Giant Impacts: Mechanisms and Scaling of Near- and Far-field Loss
Atmospheric Loss during Giant Impacts: Mechanisms and Scaling of Near- and Far-field Loss Open
The primary epoch of planetary accretion concludes with giant impacts—highly energetic collisions between protoplanets that can play a key role in shaping a planet’s inventory of volatile elements. Previous work has shown that single giant…
View article: Atmospheric loss during giant impacts: mechanisms and scaling of near- and far-field loss
Atmospheric loss during giant impacts: mechanisms and scaling of near- and far-field loss Open
The primary epoch of planetary accretion concludes with giant impacts - highly energetic collisions between proto-planets that can play a key role in shaping a planet's inventory of volatile elements. Previous work has shown that single gi…
View article: Asteroids fail to retain cometary impact signatures
Asteroids fail to retain cometary impact signatures Open
The inner solar system experienced a period of intense cometary bombardment following a dynamical instability among the giant planets, which occurred after the dispersal of the gas disk. Vesta, the second-largest asteroid in the main aster…
View article: A super-massive Neptune-sized planet
A super-massive Neptune-sized planet Open
View article: Author Correction: A super-massive Neptune-sized planet
Author Correction: A super-massive Neptune-sized planet Open
View article: <tt>MANTA-Ray</tt>: Supercharging Speeds for Calculating the Optical Properties of Fractal Aggregates in the Long-wavelength Limit
MANTA-Ray: Supercharging Speeds for Calculating the Optical Properties of Fractal Aggregates in the Long-wavelength Limit Open
Correctly modelling the absorptive properties of dust and haze particles is of great importance for determining the abundance of solid matter within protoplanetary discs and planetary atmospheres. Rigorous analyses such as the discrete dip…
View article: MANTA-Ray: Supercharging Speeds for Calculating the Optical Properties of Fractal Aggregates in the Long-Wavelength Limit
MANTA-Ray: Supercharging Speeds for Calculating the Optical Properties of Fractal Aggregates in the Long-Wavelength Limit Open
Correctly modelling the absorptive properties of dust and haze particles is of great importance for determining the abundance of solid matter within protoplanetary disks and planetary atmospheres. Rigorous analyses such as the discrete dip…
View article: Exploring the catastrophic regime: thermodynamics and disintegration in head-on planetary collisions
Exploring the catastrophic regime: thermodynamics and disintegration in head-on planetary collisions Open
Head-on giant impacts (collisions between planet-sized bodies) are frequently used to study the planet formation process as they present an extreme configuration where the two colliding bodies are greatly disturbed. With limited computing …
View article: Formation of super-Mercuries via giant impacts
Formation of super-Mercuries via giant impacts Open
During the final stage of planetary formation, different formation pathways of planetary embryos could significantly influence the observed variations in planetary densities. Of the approximately 5,000 exoplanets identified to date, a nota…
View article: Formation of super-Mercuries via giant impacts
Formation of super-Mercuries via giant impacts Open
During the final stage of planetary formation, different formation pathways of planetary embryos could significantly influence the observed variations in planetary densities. Of the approximately 5000 exoplanets identified to date, a notab…
View article: Aerosols are not spherical cows: using discrete dipole approximation to model the properties of fractal particles
Aerosols are not spherical cows: using discrete dipole approximation to model the properties of fractal particles Open
The optical properties of particulate-matter aerosols, within the context of exoplanet and brown dwarf atmospheres, are compared using three different models: Mie theory, modified mean field (MMF) theory, and discrete dipole approximation …
View article: Author Correction: A planetary collision afterglow and transit of the resultant debris cloud
Author Correction: A planetary collision afterglow and transit of the resultant debris cloud Open
View article: Post-giant impact planetesimals sustaining extreme debris discs
Post-giant impact planetesimals sustaining extreme debris discs Open
Extreme debris discs can show short-term behaviour through the evolution and clearing of small grains produced in giant impacts, and potentially a longer period of variability caused by a planetesimal population formed from giant impact ej…
View article: Post-Giant Impact Planetesimals Sustaining Extreme Debris Disks
Post-Giant Impact Planetesimals Sustaining Extreme Debris Disks Open
Extreme debris disks can show short term behaviour through the evolution and clearing of small grains produced in giant impacts, and potentially a longer period of variability caused by a planetesimal population formed from giant impact ej…
View article: Correction to: Atmosphere loss in oblique Super-Earth collisions
Correction to: Atmosphere loss in oblique Super-Earth collisions Open
View article: Author Correction: A super-massive Neptune-sized planet
Author Correction: A super-massive Neptune-sized planet Open
View article: A planetary collision afterglow and transit of the resultant debris cloud
A planetary collision afterglow and transit of the resultant debris cloud Open
Planets grow in rotating disks of dust and gas around forming stars, some of which can subsequently collide in giant impacts after the gas component is removed from the disk. Monitoring programs with the warm Spitzer mission have recorded …
View article: A planetary collision afterglow and transit of the resultant debris cloud
A planetary collision afterglow and transit of the resultant debris cloud Open
View article: A compact multi-planet system transiting HIP 29442 (TOI-469) discovered by TESS and ESPRESSO
A compact multi-planet system transiting HIP 29442 (TOI-469) discovered by TESS and ESPRESSO Open
Context. One of the goals of the Echelle Spectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO) Guaranteed Time Observations (GTO) consortium is the precise characterisation of a selected sample of planetary sys…
View article: ASASSN-21qj astronomical observations
ASASSN-21qj astronomical observations Open
Data from astronomical observatories looking at the star ASASSN-21qj.
View article: ASASSN-21qj astronomical observations
ASASSN-21qj astronomical observations Open
Data from astronomical observatories looking at the star ASASSN-21qj.
View article: A super-massive Neptune-sized planet
A super-massive Neptune-sized planet Open