Jaime Klapp

Star formation efficiency in galaxy interactions and mergers: a statistical study

NGC 6240: merger-induced star formation and gas dynamics

Simulating star formation in molecular cloud cores

Multiple protostellar systems

Zero-metallicity stars

LAMMPS - a flexible simulation tool for particle-based materials modeling at the atomic, meso, and continuum scales

High Spatial Resolution Imaging of Pre–Main‐Sequence Binary Stars: Resolving the Relationship between Disks and Close Companions

Breast Density as a Predictor of Mammographic Detection: Comparison of Interval- and Screen-Detected Cancers

Financial integration and renewable energy consumption in China: do education and digital economy development matter?

Oscillation of viscous drops with smoothed particle hydrodynamics

Cosmology at low frequencies: The 21cm transition and the high-redshift Universe

SPH simulation of transition to turbulence for planar shear flow subjected to a streamwise magnetic field

Simulating star formation in molecular cloud cores I. The influence of low levels of turbulence on fragmentation and multiplicity

parsec: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code

Investigating Disk Evolution: A High Spatial Resolution Mid‐Infrared Survey of T Tauri Stars

Income inequality and renewable energy consumption: Time-varying non-parametric evidence

A one-parameter family of interpolating kernels for smoothed particle hydrodynamics studies

E pur si muove:Galilean-invariant cosmological hydrodynamical simulations on a moving mesh

On the SPH tensile instability in forming viscous liquid drops

A High Angular Resolution Multiplicity Survey of the Open Clusters α Persei and Praesepe

f(R)theories of gravity

Physics-informed neural networks for high-speed flows

Growth rate of 147 mammary carcinomas

THE IMPACT OF INTERACTIONS, BARS, BULGES, AND ACTIVE GALACTIC NUCLEI ON STAR FORMATION EFFICIENCY IN LOCAL MASSIVE GALAXIES

Smoothed Particle Hydrodynamics (SPH): an Overview and Recent Developments

SPH with the multiple boundary tangent method

What Can Pre-Main Sequence Binary Star Populations Tell Us about Binary Formation Mechanisms?

Observational Constraints on the Formation and Evolution of Binary Stars

A new multi-resolution parallel framework for SPH

SpitzerObservations of a 24 μm Shadow: Bok Globule CB 190

Comparison study of MPM and SPH in modeling hypervelocity impact problems

Modeling Transient Heat Transfer Using SPH and Implicit Time Integration

A Test of Pre–Main‐Sequence Evolutionary Models across the Stellar/Substellar Boundary Based on Spectra of the Young Quadruple GG Tauri

Energy-conserving dissipative particle dynamics with temperature-dependent properties

NICMOS Images of the GG Tauri Circumbinary Disk

A Multiwavelength Scattered Light Analysis of the Dust Grain Population in the GG Tauri Circumbinary Ring

Cosmological simulations using a static scalar-tensor theory

Zero-metallicity stars I. Evolution at constant mass

GG Tauri's Circumbinary Disk: Models for Near‐Infrared Scattered‐Light Images and¹³CO ( \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $J=1arrow 0$ \end{document} ) Line Profiles

Keck Diffraction‐limited Imaging of the Young Quadruple Star System HD 98800

Detecting Population III Stars through Observations of Near‐Infrared Cosmic Infrared Background Anisotropies

Coalescence of colliding van der Waals liquid drops

Adaptive kernel estimation and SPH tensile instability

Self‐gravitational Hydrodynamics with Three‐dimensional Adaptive Mesh Refinement: Methodology and Applications to Molecular Cloud Collapse and Fragmentation

Improving convergence in smoothed particle hydrodynamics simulations without pairing instability

An incompressible multi-phase SPH method

Cosmological Effects of the First Stars: Evolving Spectra of Population III

No Fossil Disk in the T Tauri Multiple System V773 Tauri

Dynamical Masses for Pre–Main‐Sequence Stars: A Preliminary Physical Orbit for V773 Tau A

Star Formation in the Milky Way and Nearby Galaxies

Protostellar collapse models of prolate molecular cloud cores

The influence of numerical parameters on tidally triggered bar formation

[Early diagnosis of breast cancer: control of risk groups or mass screening--who should be radiographed? Clinical, roentgenologic and thermographic risk groups in 14,000 patients with 582 breast cancers].

Collapse and Fragmentation Models of Tidally Interacting Molecular Cloud Cores. IV. Initial Slow Rotation and Magnetic Field Support

Very massive stars: Evolution with mass loss

SPH simulations of time-dependent Poiseuille flow at low Reynolds numbers

A shock-capturing SPH scheme based on adaptive kernel estimation

Towards a cleaner planet: energy for the future

Very massive stars: Evolution with mass loss

Collapse and Fragmentation Models of Prolate Molecular Cloud Cores. I. Initial Uniform Rotation