Jacob B. Simon
YOU?
Author Swipe
View article: Bridging Unstratified and Stratified Simulations of the Streaming Instability for <i>τ</i> <sub> <i>s</i> </sub> = 0.1 Grains
Bridging Unstratified and Stratified Simulations of the Streaming Instability for <i>τ</i> <sub> <i>s</i> </sub> = 0.1 Grains Open
The streaming instability (SI), driven by aerodynamic coupling between solids and gas under a global radial pressure gradient, concentrates solids and facilitates planetesimal formation. Unstratified simulations are commonly used to study …
View article: Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall
Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall Open
There is growing evidence that planet formation begins early, within the ≲1 Myr Class 0/I phase, when infall dominates disk dynamics. Our goal is to determine if Class 0/I disks reach the conditions needed to form planetesimals (∼100 km pl…
View article: Turbulence Inhibits Early Planetesimal Formation
Turbulence Inhibits Early Planetesimal Formation Open
A major open question in planetary science and astrophysics is: when exactly does planet formation begin? Within the context of planetary science, it is known that CAIs formed 4.6 Gyr ago, but Kuiper Belt Objects (KBOs) may have formed mor…
View article: Planetesimal initial mass functions formed via the Streaming Instability agree with Cold Classical KBO size distributions
Planetesimal initial mass functions formed via the Streaming Instability agree with Cold Classical KBO size distributions Open
IntroductionPlanetesimals are small bodies held together by their own gravity, usually 1-1000 km in diameter. They can grow efficiently into planets by accreting pebbles and solid dust. The formation of planetesimals is an important open q…
View article: On Linking Planet Formation Models, Protoplanetary Disk Properties, and Mature Gas Giant Exoplanet Atmospheres
On Linking Planet Formation Models, Protoplanetary Disk Properties, and Mature Gas Giant Exoplanet Atmospheres Open
Measuring a single elemental ratio (e.g., carbon-to-oxygen) provides insufficient information for understanding the formation mechanisms and evolution that affect our observations of gas giant planet atmospheres. Although the fields of pla…
View article: Bridging Unstratified and Stratified Simulations of the Streaming Instability for $τ_s=0.1$ Grains
Bridging Unstratified and Stratified Simulations of the Streaming Instability for $τ_s=0.1$ Grains Open
The streaming instability (SI), driven by aerodynamic coupling between solids and the gas under a global radial pressure gradient, concentrates solids and facilitates planetesimal formation. Unstratified simulations are commonly used to st…
View article: Positive feedback: How a synergy between the streaming instability and dust coagulation forms planetesimals
Positive feedback: How a synergy between the streaming instability and dust coagulation forms planetesimals Open
Context. One of the most important open questions in planet formation is how dust grains in a protoplanetary disk manage to overcome growth barriers and form the ∼100 km planet building blocks that we call planetesimals. There appears to b…
View article: Probing Conditions for Strong Clumping by the Streaming Instability: Small Dust Grains and Low Dust-to-gas Density Ratio
Probing Conditions for Strong Clumping by the Streaming Instability: Small Dust Grains and Low Dust-to-gas Density Ratio Open
The streaming instability (SI) is a leading mechanism for concentrating solid particles into regions dense enough to form planetesimals. Its efficiency in clumping particles depends primarily on the dimensionless stopping time ( τ s , a pr…
View article: Probing Conditions for Strong Clumping by the Streaming Instability: Small Dust Grains and Low Dust-to-gas Density Ratio
Probing Conditions for Strong Clumping by the Streaming Instability: Small Dust Grains and Low Dust-to-gas Density Ratio Open
The streaming instability (SI) is a leading mechanism for concentrating solid particles into regions dense enough to form planetesimals. Its efficiency in clumping particles depends primarily on the dimensionless stopping time ($τ_s$, a pr…
View article: Magnetically Driven Turbulence in the Inner Regions of Protoplanetary Disks
Magnetically Driven Turbulence in the Inner Regions of Protoplanetary Disks Open
Given the important role turbulence plays in the settling and growth of dust grains in protoplanetary disks, it is crucial that we determine whether these disks are turbulent and to what extent. Protoplanetary disks are weakly ionized near…
View article: Exploring the Complex Ionization Environment of the Turbulent DM Tau Disk
Exploring the Complex Ionization Environment of the Turbulent DM Tau Disk Open
Ionization drives important chemical and dynamical processes within protoplanetary disks, including the formation of organics and water in the cold midplane and the transportation of material via accretion and magnetohydrodynamic flows. Un…
View article: Streaming Instability and Turbulence: Conditions for Planetesimal Formation
Streaming Instability and Turbulence: Conditions for Planetesimal Formation Open
The streaming instability (SI) is a leading candidate for planetesimal formation, which can concentrate solids through two-way aerodynamic interactions with the gas. The resulting concentrations can become sufficiently dense to collapse un…
View article: Rapid Protoplanet Formation in Vortices: Three-dimensional Local Simulations with Self-gravity
Rapid Protoplanet Formation in Vortices: Three-dimensional Local Simulations with Self-gravity Open
Disk vortices, seen in numerical simulations of protoplanetary disks and found observationally in Atacama Large Millimeter/submillimeter Array and Very Large Array images of these objects, are promising sites for planet formation given the…
View article: Exploring the Complex Ionization Environment of the Turbulent DM Tau Disk
Exploring the Complex Ionization Environment of the Turbulent DM Tau Disk Open
Ionization drives important chemical and dynamical processes within protoplanetary disks, including the formation of organics and water in the cold midplane and the transportation of material via accretion and magneto-hydrodynamic (MHD) fl…
View article: Rapid protoplanet formation in vortices: three-dimensional local simulations with selfgravity
Rapid protoplanet formation in vortices: three-dimensional local simulations with selfgravity Open
Disk vortices, seen in numerical simulations of protoplanetary disks and found observationally in ALMA and VLA images of these objects, are promising sites for planet formation given their pebble trapping abilities. Previous works have sho…
View article: Evidence for non-zero turbulence in the protoplanetary disc around IM Lup
Evidence for non-zero turbulence in the protoplanetary disc around IM Lup Open
The amount of turbulence in protoplanetary discs around young stars is critical for determining the efficiency, timeline, and outcomes of planet formation. It is also difficult to measure. Observations are still limited, but direct measure…
View article: Evidence for Non-zero Turbulence in the Protoplanetary disc around IM Lup
Evidence for Non-zero Turbulence in the Protoplanetary disc around IM Lup Open
The amount of turbulence in protoplanetary discs around young stars is critical for determining the efficiency, timeline, and outcomes of planet formation. It is also difficult to measure. Observations are still limited, but direct measure…
View article: The Limited Role of the Streaming Instability during Moon and Exomoon Formation
The Limited Role of the Streaming Instability during Moon and Exomoon Formation Open
It is generally accepted that the Moon accreted from the disk formed by an impact between the proto-Earth and impactor, but its details are highly debated. Some models suggest that a Mars-sized impactor formed a silicate melt-rich (vapor-p…
View article: Magnetically Driven Turbulence in the Inner Regions of Protoplanetary Disks
Magnetically Driven Turbulence in the Inner Regions of Protoplanetary Disks Open
Given the important role turbulence plays in the settling and growth of dust grains in protoplanetary disks, it is crucial that we determine whether these disks are turbulent and to what extent. Protoplanetary disks are weakly ionized near…
View article: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion Open
Kuiper Belt objects (KBOs) show an unexpected trend, whereby large bodies have increasingly higher densities, up to five times greater than their smaller counterparts. Current explanations for this trend assume formation at constant compos…
View article: A solution for the density dichotomy problem of Kuiper Belt objects with multi-species streaming instability and pebble accretion
A solution for the density dichotomy problem of Kuiper Belt objects with multi-species streaming instability and pebble accretion Open
Kuiper belt objects show an unexpected trend, whereby large bodies have increasingly higher densities, up to five times greater than their smaller counterparts. Current explanations for this trend assume formation at constant composition, …
View article: Streaming Instability and Turbulence: Conditions for Planetesimal Formation
Streaming Instability and Turbulence: Conditions for Planetesimal Formation Open
The streaming instability (SI) is a leading candidate for planetesimal formation, which can concentrate solids through two-way aerodynamic interactions with the gas. The resulting concentrations can become sufficiently dense to collapse un…
View article: Implications for Chondrule Formation Regions and Solar Nebula Magnetism from Statistical Reanalysis of Chondrule Paleomagnetism
Implications for Chondrule Formation Regions and Solar Nebula Magnetism from Statistical Reanalysis of Chondrule Paleomagnetism Open
Converging lines of evidence show that protoplanetary disks are complex environments hosting spatial and temporal variability at multiple scales. Here we reanalyze paleomagnetic estimates of solar nebula magnetic field strengths using a Ba…
View article: A declining major merger fraction with redshift in the local Universe from the largest-yet catalog of major and minor mergers in SDSS
A declining major merger fraction with redshift in the local Universe from the largest-yet catalog of major and minor mergers in SDSS Open
These tables are described in more detail in Section 4.1 of the accompanying paper. Table_1.txt provides the imaging predictor values and photometric flags for all SDSS photometric galaxies used in this study. Flags have a value of 1 when …
View article: Comets and Planetesimal Formation
Comets and Planetesimal Formation Open
In this chapter, we review the processes involved in the formation of planetesimals and comets. We will start with a description of the physics of dust grain growth and how this is mediated by gas-dust interactions in planet-forming disks.…
View article: Planetesimal Formation (or Lack Thereof) in Pressure Bumps and Implications for Early Planet Formation
Planetesimal Formation (or Lack Thereof) in Pressure Bumps and Implications for Early Planet Formation Open
<p>A crucial step in the planet formation process is the formation of smaller bodies known as planetesimals.<span>  </span>However, how these small bodies formed is one of the largest outstanding issues in planet…
View article: Using Bayesian Deep Learning to Infer Planet Mass from Gaps in Protoplanetary Disks
Using Bayesian Deep Learning to Infer Planet Mass from Gaps in Protoplanetary Disks Open
Planet-induced substructures, like annular gaps, observed in dust emission from protoplanetary disks, provide a unique probe for characterizing unseen young planets. While deep-learning-based models have an edge in characterizing a planet’…
View article: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps Open
We present evidence that it is unlikely that the streaming instability (SI) can form planetesimals from millimeter grains inside axisymmetric pressure bumps. We conducted the largest simulation of the SI so far (7 million CPU hours), consi…
View article: The Streaming Instability Cannot Form Planetesimals from mm-size Grains in Pressure Bumps
The Streaming Instability Cannot Form Planetesimals from mm-size Grains in Pressure Bumps Open
We present evidence that it is unlikely that the streaming instability (SI) can form planetesimals from mm grains inside axisymmetric pressure bumps. We conducted the largest simulation of the SI so far (7 million CPU hours), consisting of…
View article: Moon Formation via Streaming Instability
Moon Formation via Streaming Instability Open
<ul><li>The Apollo lunar samples reveal that Earth and the Moon have strikingly similar isotopic ratios, suggesting that these bodies may share the same source materials. This leads to the "standard" giant impact hypo…