Issue |
A&A
Volume 449, Number 3, April III 2006
|
|
---|---|---|
Page(s) | 1043 - 1059 | |
Section | Galactic structure, stellar clusters, and populations | |
DOI | https://doi.org/10.1051/0004-6361:20054254 | |
Published online | 24 March 2006 |
The influence of numerical parameters on tidally triggered bar formation
1
Depto. de Física, Instituto Nacional de Investigaciones Nucleares, Apdo. Postal 18-1027, México DF 11801, México e-mail: ruslan@nuclear.inin.mx
2
Facultad de Ciencias, Universidad Autónoma del Estado de México, Instituto Literario 100, CP 50000, Toluca, México
3
Universität Konstanz, Fachbereich Physik, Fach M568, 78457 Konstanz, Germany
Received:
24
September
2005
Accepted:
19
December
2005
The joint influence of numerical parameters such
as the number of particles N, the gravitational softening length ε and the time-step is investigated in the
context of galaxy simulations.
For isolated galaxy models we have performed a convergence study
and estimated the numerical parameters ranges for which the relaxed
models do not deviate significantly from its initial
configuration.
By fixing N, we calculate the range of the mean interparticle
separation
along the disc radius. Uniformly spaced
values of λ are used as ε in numerical tests
of disc heating. We have found that in the simulations with
particles λ varies by a factor of 6, and
the corresponding final Toomre's parameters Q change by only
about 5 per cent. By decreasing N, the λ and Q
ranges broaden. Large ε and small N cause an earlier
bar formation. In addition, the numerical experiments indicate,
that for a given set of parameters the disc heating is smaller
with the Plummer softening than with the spline softening.
For galaxy collision models we have studied the influence of the
selected numerical parameters on the formation of tidally triggered
bars in galactic discs and their properties, such as their dimensions,
shape, amplitude and rotational velocity.
Numerical simulations indicate that the properties of the formed bars
strongly depend upon the selection of N and ε.
Large values of the gravitational
softening parameter and a small number of particles result in the
rapid formation of a well defined, slowly rotating bar.
On the other hand, small values of ε produce a small,
rapidly rotating disc with tightly wound spiral arms, and subsequently
a weak bar emerges.
We have found that by increasing N, the bar properties converge
and the effect of the softening parameter diminishes. Finally, in
some cases short spiral arms are observed at the ends of the bar
that change periodically from trailing to leading and vice-versa
– the wiggle.
Key words: galaxies: kinematics and dynamics / galaxies: interaction / methods: N-body simulation
© ESO, 2006
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