Prof. Peter Read

Abstract:

A laboratory investigation is presented with the aim of studying systematically the occurrence and characteristics of low-frequency variability of flows resulting from the interaction of a baroclinic flow with periodic bottom topography. Low-frequency variability within the baroclinic wave regime occurred in two distinct forms in separate regions of parameter space. One corresponded to the transition region between the baroclinic travelling and stationary wave regimes. It involved primarily an interaction between the drifting baroclinic waves and stationary components of the topographically forced wave. The resulting flow had characteristics similar to amplitude vacillation and had a time-scale of 30–60 annulus revolutions (days), which also corresponded to the wave drift period. A new regime of low-frequency amplitude vacillation was discovered in the transition region with the axisymmetric flow regime. As the complexity of the flow increased the period of the vacillation cycles grew to ∼100–180 “days”. This slower vacillation seemed to involve a cyclic enabling and disabling of nonlinear interactions between the forced stationary wave and the growing and azimuthally drifting wave, which in turn was linked to a decrease in mean flow shear. Subsequent chains of wave-wave interactions characterised the complex but robust oscillation phenomenon. The resulting behaviour has several features in common with some recent models of intraseasonal oscillations in the mid-latitude troposphere and with sudden stratospheric warmings.

Abstract:

The martian solsticial pause, presented in a companion paper (. Lewis et al., 2016), was investigated further through a series of model runs using the UK version of the LMD/UK Mars Global Climate Model. It was found that the pause could not be adequately reproduced if radiatively active water ice clouds were omitted from the model. When clouds were used, along with a realistic time-dependent dust opacity distribution, a substantial minimum in near-surface transient eddy activity formed around solstice in both hemispheres. The net effect of the clouds in the model is, by altering the thermal structure of the atmosphere, to decrease the vertical shear of the westerly jet near the surface around solstice, and thus reduce baroclinic growth rates. A similar effect was seen under conditions of large dust loading, implying that northern midlatitude eddy activity will tend to become suppressed after a period of intense flushing storm formation around the northern cap edge. Suppression of baroclinic eddy generation by the barotropic component of the flow and via diabatic eddy dissipation were also investigated as possible mechanisms leading to the formation of the solsticial pause but were found not to make major contributions. Zonal variations in topography were found to be important, as their presence results in weakened transient eddies around winter solstice in both hemispheres, through modification of the near-surface flow. The zonal topographic asymmetry appears to be the primary reason for the weakness of eddy activity in the southern hemisphere relative to the northern hemisphere, and the ultimate cause of the solsticial pause in both hemispheres. The meridional topographic gradient was found to exert a much weaker influence on near-surface transient eddies.