The atmospheres of Venus, Mars and Titan are similar to the atmosphere of Earth. We wanted to find out the value of the residence time of energy in these three atmospheres. We estimated the energy contained in a column of air. From experimental data, we deduced the value of the energy inflow and outflow. From these data, the time of residence of the energy is calculated. This parameter gives a timescale of the response of the planetary atmosphere against global perturbations.

We design a new non-linear model to construct an accurate relationship between auroral oval boundaries and 18 space physical parameters, and explore the influence of every single space physical parameter on auroral oval boundary in this paper. As a result, we found the combination of some space physical parameters can strengthen each other's influence on aurora oval boundary prediction, and this model can achieve the best performance when only partial space physical parameters are used as input.

We discuss how to calibrate simplified models of the geomagnetic dipole field to geomagnetic observations collected over the past 2 Myr over two different timescales.

We use temperature maps of the solar corona for three regions and use a technique that separates multiple timescales and space scales to show that the small-scale temperature fluctuations appear more frequently prior to the occurrence of a solar flare, in comparison with the same region after the flare and with a quiet region. We find that, during the flare, energy flows from large to small scales and heat transport associated with a heat front is convective along and diffusive across the front.