Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0701909)
· References in the article
· Citations to the Article (16) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Adaptive smoothing lengths in SPH
Authors:
Attwood, R. E.; Goodwin, S. P.; Whitworth, A. P.
Affiliation:
AA(School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, Wales, UK ), AB(Department of Physics and Astronomy, University of Sheffield, Hicks Building, Housfield Road, Sheffield S3 7RH, UK ), AC(School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, Wales, UK )
Publication:
Astronomy and Astrophysics, Volume 464, Issue 2, March III 2007, pp.447-450 (A&A Homepage)
Publication Date:
03/2007
Origin:
EDP Sciences
Astronomy Keywords:
hydrodynamics, methods: numerical, stars: oscillations
DOI:
10.1051/0004-6361:20066606
Bibliographic Code:
2007A&A...464..447A

Abstract

Context: There is a need to improve the fidelity of SPH simulations of self-gravitating gas dynamics.
Aims: We remind users of SPH that, if smoothing lengths are adjusted so as to keep the number of neighbours, N, in the range NNEIB±ΔNNEIB, the tolerance, ΔNNEIB, should be set to zero, as first noted by Nelson & Papaloizou. We point out that this is a very straightforward and computationally inexpensive constraint to implement.
Methods: We demonstrate this by simulating acoustic oscillations of a self-gravitating isentropic monatomic gas-sphere (cf. Lucy), using NTOT˜6000 particles and NNEIB=50.
Results: We show that there is a marked reduction in the rates of numerical dissipation and diffusion as ΔNNEIB is reduced from 10 to zero. Moreover this reduction incurs a very small computational overhead.
Conclusions: .We propose that this should become a standard test for codes used in simulating star formation. It is a highly relevant test, because pressure waves generated by the switch from approximate isothermality to approximate adiabaticity play a critical role in the fragmentation of collapsing prestellar cores. Since many SPH simulations in the literature use NNEIB=50 and ΔNNEIB≥10, their results must be viewed with caution.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints