R
Richard I. Klein
Researcher at University of California, Berkeley
Publications - 132
Citations - 10343
Richard I. Klein is an academic researcher from University of California, Berkeley. The author has contributed to research in topics: Star formation & Molecular cloud. The author has an hindex of 52, co-authored 129 publications receiving 9663 citations. Previous affiliations of Richard I. Klein include Lawrence Berkeley National Laboratory & Princeton University.
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Journal ArticleDOI
The Jeans Condition: A New Constraint on Spatial Resolution in Simulations of Isothermal Self-gravitational Hydrodynamics
J. Kelly Truelove,J. Kelly Truelove,Richard I. Klein,Richard I. Klein,Christopher F. McKee,John H. Holliman,John H. Holliman,Louis H. Howell,Jeffrey A. Greenough +8 more
TL;DR: In this paper, it was shown that perturbations arising from discretization of the equations of self-gravitational hydrodynamics can grow into fragments in multiple-grid simulations, a process referred to as artificial fragmentation.
Journal ArticleDOI
On the hydrodynamic interaction of shock waves with interstellar clouds. 1: Nonradiative shocks in small clouds
TL;DR: In this paper, the authors present a comprehensive numerical study of the simplest case of the interaction between a shock wave and a spherical cloud, in which the shock far from the cloud is steady and planar, and in which radiative losses, thermal conduction, magnetic fields, and gravitational forces are all neglected.
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The formation of massive star systems by accretion.
Mark R. Krumholz,Richard I. Klein,Richard I. Klein,Christopher F. McKee,Stella S. R. Offner,Andrew J. Cunningham +5 more
TL;DR: Three-dimensional radiation-hydrodynamic simulations of the collapse of a massive prestellar core are presented and it is found that radiation pressure does not halt accretion, but the instabilities that allow accretion to continue lead to small multiple systems.
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Radiation-Hydrodynamic Simulations of Collapse and Fragmentation in Massive Protostellar Cores
TL;DR: In this article, the Orion adaptive mesh refinement code is used to simulate the early stages of the evolution of turbulent, virialized, high-mass protostellar cores, with primary attention to how cores fragment and whether they form a small or large number of protostars.
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The effects of radiative transfer on low-mass star formation
TL;DR: In this article, an adaptive mesh refinement (AMR) three-dimensional gravito-radiation-hydrodyanics code is used to simulate low-mass star formation in a turbulent molecular cloud.