We derive a multi-scale model of moist tropical dynamics which is valid on horizontal synoptic scales, zonal planetary scales, and synoptic and intraseasonal time scales. The Intraseasonal Multi-Scale Moist Dynamics (IMMD) framework builds on the IPESD framework of [A.J. Majda and R. Klein, J. Atmos. Sci., 60, 393–408, 2003]. It generalizes the latter by allowing for strong zonal winds (the Tra...

We present the first 3D MHD study in spherical geometry of the non-linear dynamical evolution of magnetic flux tubes in a turbulent rotating convection zone. These numerical simulations use the anelastic spherical harmonic (ASH) code. We seek to understand the mechanism of emergence of strong toroidal fields through a turbulent layer from the base of the solar convection zone to the surface as ...

5 Developing wave packets associated with the extratropical transition (ET) of tropical cy6 clones and winter cyclones in the Western North Pacific (WNP) and Atlantic basins are 7 diagnosed observationally by compositing reanalysis data over a 32 year period. While the 8 development of winter cyclones amplifies a weaker wave packet moving through the mid9 latitude storm track, there is no indic...

We present a new concept to infer the meridional flow in the deep solar interior from global oscillation data. This concept is based on the estimation of the coupling strengths of p-mode eigenfunctions mediated by the meridional flow. We illustrate the performance of the method using simulations and present first inversion results of a large-scale flow component of the meridional flow obtained ...

We investigate the long-term dynamical evolution of internal kinematics multimass rotating star clusters. have performed a set N-body simulations to follow clusters with different degrees initial rotation and explored rotational velocity, degree energy equipartition, anisotropy in velocity distribution. Our show that: 1) as cluster evolves, develops dependence on stellar mass more massive stars...

In this paper it is attempted to investigate the behavior of an inviscid flow in the meridional plane of an axial flow compressor. For this purpose the 3-D unsteady Euler equations in cylindrical coordinate are averaged in tangential direction. Therefore, the equations are reduced to a 2-D system. By averaging the tangential component of momentum equation, a blade force will result. Axial and r...

We further develop the Tayler–Spruit dynamo theory, based on the most efficient instability for generating magnetic fields in radiative layers of differentially rotating stars. We avoid the simplifying assumptions that either the μ– or the T–gradient dominates, but we treat the general case and we also account for the nonadiabatic effects, which favour the growth of the magnetic field. The gene...

We construct an exact solution of the geophysical fluid dynamics governing equations which models waves in presence underlying currents, extending Pollard’s wave to admit meridional and vertical currents at mid-latitudes. show that these cannot be prescribed arbitrarily, but rather must constant form a velocity vector is parallel Earth’s rotation vector. At equator, there freedom prescribe curr...

The solar torsional oscillations are considered as the response of the Reynolds stress to the time-dependent dynamo-induced magnetic eld. This picture is opposite to the so far accepted idea that it is the large-scale Lorentz force which directly drives the temporal variations of the surface rotation proole. Here, the \magnetic quenching" of the components of the Reynolds stress { viscosity ten...

[1] We examine the upstream meridional deflection flows of interplanetary coronal mass ejections (ICMEs) in an effort to investigate their cross-sectional shape and the magnetic field orientation in their sheath regions. Eight out of 11 magnetic clouds (MCs) near solar minimum identified for the curvature study are concave outward as indicated by the elevation angle of the MC normal with respec...