Local models of stellar convection

Free access article

Issue		A&A Volume 448, Number 2, March III 2006


Page(s)		433 - 438
Section		Astrophysical processes
DOI		http://dx.doi.org/10.1051/0004-6361:20042245

A&A 448, 433-438 (2006)
DOI: 10.1051/0004-6361:20042245

III. The Strouhal number

P. J. Käpylä^{1, 2}, M. J. Korpi³, M. Ossendrijver² and I. Tuominen^{1, 3}

¹ Astronomy Division, Department of Physical Sciences, PO Box 3000, 90014 University of Oulu, Finland
e-mail: petri.kapyla@oulu.fi
² Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany
³ Observatory, PO Box 14, 00014 University of Helsinki, Finland

(Received 25 October 2004 / Accepted 9 November 2005 )

Abstract
Aims.The Strouhal number (St), which is a nondimensional measure of the correlation time, is determined from numerical models of convection. The Strouhal number arises in the mean-field theories of angular momentum transport and magnetic field generation, where its value determines the validity of certain widely used approximations, such as the first order smoothing (hereafter FOSA). More specifically, the relevant transport coefficients can be calculated by means of a cumulative series expansion if ${\rm St} < {\rm St}_{\rm crit} \approx 1$ .
Methods.We define the Strouhal number as the ratio of the correlation and turnover times, which we determine separately, the former from the autocorrelation of velocity, and the latter by following test particles embedded in the flow.
Results.We find that the Strouhal numbers are, generally, of the order of 0.1 to 0.4 which is close to the critical value above which deviations from FOSA become significant. Increasing the rotational influence tends to shorten both timescales in such a manner that St decreases. However, we do not find a clear trend as a function of the Rayleigh number for the parameter range explored in the present study.

Key words: hydrodynamics

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