Evolution of rotating interstellar clouds. I - Numerical techniques

Black, David C.; Bodenheimer, Peter

doi:10.1086/153729

Cited by 93 publications

(85 citation statements)

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“…The central cell is treated as a sink cell into which mass and angular momentum can flow (Boss & Black 1982). The Poisson equation for the gravitational potential is solved according to Black & Bodenheimer (1975). For the hydrodynamics and radiation transport, the scheme from Ròžyczka (1985) is taken.…”

Section: Physical Model: a 2-dimensional Hydrodynamical Simulationmentioning

confidence: 99%

Modeling the chemical evolution of a collapsing prestellar core in two spatial dimensions

Weeren¹,

Brinch

Hogerheijde³

2009

A&A

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Context. The physical conditions in a collapsing cloud can be traced by observations of molecular lines. To correctly interpret these observations the abundance distributions of the observed species need to be derived. The chemistry in a collapsing molecular cloud is not in a steady state as the density and temperature evolve. We therefore need to follow chemical reactions, both in the gas phase and on dust grains, as well as gas-grain interactions, to predict the abundance distributions. Aims. Our aim is to model the abundances of molecules, in the gas phase and on grain mantles in the form of ice, from prestellar core collapse to disk formation. We want to investigate the need for grain surface reactions and compare our results with observed abundances, column densities, and ice-mantle compositions. Methods. We use a 2-dimensional hydrodynamical simulation as a physical model from which we take the density, temperature, and the flow of the gas. Trace particles, moving along with the gas, are used to follow the chemistry during prestellar core collapse and disk formation. We calculated abundance profiles and column densities for various species. The evolution of these abundances and the composition of ices on grain mantles were compared to observations and we tested the influence of grain surface reactions on the abundances of species. We also investigated the initial abundances to be adopted in more detailed modeling of protoplanetary disks by following the chemical evolution of trace particles accreting onto the disk. Results. Fractional abundances of HCO + , N 2 H + , H 2 CO, HC 3 N, and CH 3 OH from our model with grain surface reactions provide a good match to observations, while abundances of CO, CS, SO, HCN, and HNC show better agreement without grain surface reactions. The observed mantle composition of dust grains is best reproduced when we include surface reactions. The initial chemical abundances to be used for detailed modeling of a protoplanetary disk are found to be different from those in dark interstellar clouds. Ices with a binding energy lower than about 1200 K sublimate before accreting onto the disk, while those with a higher binding energy do not.

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Section: Physical Model: a 2-dimensional Hydrodynamical Simulationmentioning

confidence: 99%

Modeling the chemical evolution of a collapsing prestellar core in two spatial dimensions

Weeren¹,

Brinch

Hogerheijde³

2009

A&A

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“…In the late 60s Jim became interested in astrophysics and started to work on core collapse supernovae, relativistic stars, magnetorotationally driven jets, and, somewhat later, numerical general relativity. In the 1970s Jim had assisted David Black and Peter Bodenheimer at UC Santa Cruz to develop a 2D hydro code which they applied to axisymmetric, rotating, protostellar cloud collapse simulations (Black & Bodenheimer 1975, Black & Bodenheimer 1976. They found the collapse produced a gravitationally bound ring, confirming a result published by Richard Larson in 1972.…”

Section: Livermore Yearsmentioning

confidence: 70%

Historical perspective on astrophysical MHD simulations

Norman

2010

Proc. IAU

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Abstract. This contribution contains the introductory remarks that I presented at IAU Symposium 270 on "Computational Star Formation" held in Barcelona, Spain, May 31 -June 4, 2010. I discuss the historical development of numerical MHD methods in astrophysics from a personal perspective. The recent advent of robust, higher-order accurate MHD algorithms and adaptive mesh refinement numerical simulations promises to greatly improve our understanding of the role of magnetic fields in star formation.

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“…In Step 1, we also calculate the total gravitational potential of the gas and stellar components by solving for the Poisson Eq. (11) using the alternative direction implicit method described in Black & Bodenheimer (1975). The gravitational potential at the outer boundaries is calculated using a multipole expansion formula in spherical coordinates (Jackson 1975).…”

Section: Solution Methodsmentioning

confidence: 99%

Stellar hydrodynamical modeling of dwarf galaxies: simulation methodology, tests, and first results

Vorobyov

Recchi

Hensler

2015

A&A

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Context. In spite of enormous progress and brilliant achievements in cosmological simulations, they still lack numerical resolution or physical processes to simulate dwarf galaxies in sufficient detail. Accurate numerical simulations of individual dwarf galaxies are thus still in demand. Aims. We aim to improve available numerical techniques to simulate individual dwarf galaxies. In particular, we aim to (i) study in detail the coupling between stars and gas in a galaxy, exploiting the so-called stellar hydrodynamical approach; and (ii) study for the first time the chemodynamical evolution of individual galaxies starting from self-consistently calculated initial gas distributions.Methods. We present a novel chemodynamical code for studying the evolution of individual dwarf galaxies. In this code, the dynamics of gas is computed using the usual hydrodynamics equations, while the dynamics of stars is described by the stellar hydrodynamics approach, which solves for the first three moments of the collisionless Boltzmann equation. The feedback from stellar winds and dying stars is followed in detail. In particular, a novel and detailed approach has been developed to trace the aging of various stellar populations, which facilitates an accurate calculation of the stellar feedback depending on the stellar age. The code has been accurately benchmarked, allowing us to provide a recipe for improving the code performance on the Sedov test problem. Results. We build initial equilibrium models of dwarf galaxies that take gas self-gravity into account and present different levels of rotational support. Models with high rotational support (and hence high degrees of flattening) develop prominent bipolar outflows; a newly-born stellar population in these models is preferentially concentrated to the galactic midplane. Models with little rotational support blow away a large fraction of the gas and the resulting stellar distribution is extended and diffuse. Models that start from non-self-gravitating initial equilibrium configurations, evolve at a much slower pace owing to lower initial gas density and hence lower star formation rates. The stellar dynamics turns out to be a crucial aspect of galaxy evolution. If we artificially suppress stellar dynamics, supernova explosions occur in a medium that is heated and diluted by previous activity of stellar winds, thus artificially enhancing stellar feedback. Conclusions. The stellar hydrodynamics approach presents a promising tool for numerically studying the coupled evolution of gas and stars in dwarf galaxies.

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Evolution of rotating interstellar clouds. I - Numerical techniques

Cited by 93 publications

References 0 publications

Modeling the chemical evolution of a collapsing prestellar core in two spatial dimensions

Modeling the chemical evolution of a collapsing prestellar core in two spatial dimensions

Historical perspective on astrophysical MHD simulations

Stellar hydrodynamical modeling of dwarf galaxies: simulation methodology, tests, and first results

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