Improved understanding of the link between current density, temperature, water formation and hydration of the membrane is required to optimise cell design.
Analysis is performed in low- and high-current regimes and a complex relationship between localised current density, temperature and reactant supply is identified that describes the way in which the system enters limiting performance conditions.
The differences of neutral density, neutral temperature, and horizontal wind between the two simulations are calculated to represent the responses of density, temperature, and wind.
The relationship between the density and the transition temperature is as follows: for 1.88 g/cm3 density, the transition temperature T = 6300 K, for 1.76 g/cm3, T = 10,100 K, and for 1.1 g/cm3, T = 13,500 K.
A third relation, termed the equation of state, expresses an explicit relation between the temperature, density, and pressure of a star's internal matter.
The existence of close relations between the temperature, density and velocity of the solar plasma and the heliospheric magnetic field (HMF) was shown along the space probe Ulysses orbit.
The density and temperature ranged between 1012 and 1015 cm−3 and 2 and 10 eV, respectively.
In this paper the method is extended by calculating the fluxes of mass, momentum and energy between cells assuming a linear variation of density, temperature and velocity in each cell and using these fluxes to update the mass, velocity and internal energy carried by each particle.
It survives in environments like interstellar clouds because the density and temperatures are lower than those of Earth.
This means that there is a trade-off between the current density and temperature, and a requirement exists where either a high current density or high temperature is necessary to achieve the optimum process conditions.
