SearcharxivSearch

arXiv subjects

Piotr Smolarkiewicz

Publications and source records attributed to Piotr Smolarkiewicz.

2 recordsLinked to original sources

Intensification of tilted atmospheric vortices by asymmetric diabatic heating

Päschke et al. (JFM, 701, 137--170 (2012)) studied the nonlinear dynamics of strongly tilted vortices subject to asymmetric diabatic heating by asymptotic methods. They found, \ia, that an azimuthal Fourier mode~1 heating pattern can intensify or attenuate such a vortex depending on the relative orientation of tilt and heating asymmetries. The theory originally addressed the gradient wind regime which, asymptotically speaking, corresponds to vortex Rossby numbers of order unity in the limit. Formally, this restricts the applicability of the theory to rather weak vortices in the near equatorial region. It is shown below that said theory is, in contrast, uniformly valid for vanishing Coriolis parameter and thus applicable to vortices up to low hurricane strengths. In addition, the paper presents an extended discussion of the asymptotics as regards their physical interpretation and their implications for the overall vortex dynamics. The paper's second contribution is a series of three-dimensional numerical simulations examining the effect of different orientations of dipolar heat release on idealized tropical cyclones. Comparisons with numerical solutions of the asymptotic equations yield evidence that supports the original predictions. In addition, the influence of asymmetric diabatic heat release on the time evolution of centerline tilt is analysed further, and a steering mechanism based on the orientation of the heating dipole is revealed.

physics.flu-dyn

Magnetic field generation in PMS stars with and without radiative core

Recent observations of the magnetic field in pre-main sequence stars suggest that the magnetic field topology changes as a function of age. The presence of a tachocline could be an important factor in the development of magnetic field with higher multipolar modes. In this work we performed MHD simulations using the EULAG-MHD code to study the magnetic field generation and evolution in models that mimic stars at two evolutionary stages. The stratification for both stellar phases was computed by fitting stellar structure profiles obtained with the ATON stellar evolution code. The first stage is at $1.1 \mathrm{Myr}$, when the star is completely convective. The second stage is at $14 \mathrm{Myrs}$, when the star is partly convective, with a radiative core developed up to $30\%$ of the stellar radius. In this proceedings we present a preliminary analysis of the resulting mean-flows and magnetic field. The mean-flow analysis shown that the star rotate almost rigidly on the fully convective phase, whereas at the partially convective phase there is differential rotation with conical contours of iso-rotation. As for the mean magnetic field both simulations show similarities with respect to the field evolution. However, the topology of the magnetic field is different.

astro-ph.SR