Upon entry into the heliosphere, galactic cosmic-ray fluxes are modulated by the turbulent solar wind with the resulting modulation levels depending on the position inside the heliosphere and the phase of the solar cycle. The main modulation processes, i.e. drifts, convection, adiabatic energy changes, and diffusion can be described by the well-known Parker transport equation. A first order analytical approximation of this equation, which is widely used to describe solar modulation effects at Earth, is the Force-Field approximation, while a similar approximation, the Convection–Diffusion is rarely applied. Based on a comparison with recent top-of-atmosphere galactic cosmic-ray flux measurements, this study presents the Convection–Diffusion approximation as a more suitable alternative to the Force-Field approximation to accurately parameterize the galactic cosmic-ray intensity near Earth which is essential for dosimetry and space weather studies.

进入日光层后，银河宇宙射线通量被湍流的太阳风调制，产生的调制水平取决于日光层内部的位置和太阳周期的相位。主要的调制过程，即漂移、对流、绝热能量变化和扩散，可以用著名的帕克输运方程来描述。该方程的一阶解析近似值广泛用于描述地球上的太阳调制效应，它是力场近似值，而类似的近似值是对流-扩散近似值很少应用。基于与最近的大气层顶部银河宇宙射线通量测量结果的比较，