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**Harvard**

Romeo, A. (1998) *Modelling gravity in N-body simulations of disc galaxies. Optimal types of softening for given dynamical requirements*.

** BibTeX **

@article{

Romeo1998,

author={Romeo, Alessandro},

title={Modelling gravity in N-body simulations of disc galaxies. Optimal types of softening for given dynamical requirements},

journal={Astronomy and Astrophysics},

issn={0004-6361},

volume={335},

pages={922-928},

abstract={Modelling gravity is a fundamental problem that must be tackled in N-body simulations of stellar systems, and satisfactory solutions require a deep understanding of the dynamical effects of softening. In a previous paper (Romeo 1997), we have devised a method for exploring such effects, and we have focused on two applications that reveal the dynamical differences between the most representative types of softened gravity. In the present paper we show that our method can be applied in another, more fruitful, way: for developing new ideas about softening. Indeed, it opens a direct route to the discovery of optimal types of softened gravity for given dynamical requirements, and thus to the accomplishment of a physically consistent modelling of disc galaxies, even in the presence of a cold interstellar gaseous component and in situations that demand anisotropic resolution.},

year={1998},

}

** RefWorks **

RT Journal Article

SR Electronic

ID 214992

A1 Romeo, Alessandro

T1 Modelling gravity in N-body simulations of disc galaxies. Optimal types of softening for given dynamical requirements

YR 1998

JF Astronomy and Astrophysics

SN 0004-6361

VO 335

SP 922

OP 928

AB Modelling gravity is a fundamental problem that must be tackled in N-body simulations of stellar systems, and satisfactory solutions require a deep understanding of the dynamical effects of softening. In a previous paper (Romeo 1997), we have devised a method for exploring such effects, and we have focused on two applications that reveal the dynamical differences between the most representative types of softened gravity. In the present paper we show that our method can be applied in another, more fruitful, way: for developing new ideas about softening. Indeed, it opens a direct route to the discovery of optimal types of softened gravity for given dynamical requirements, and thus to the accomplishment of a physically consistent modelling of disc galaxies, even in the presence of a cold interstellar gaseous component and in situations that demand anisotropic resolution.

LA eng

LK http://publications.lib.chalmers.se/records/fulltext/214992/local_214992.pdf

OL 30