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The electron number density N_e distributions in solar chromosphere andcorona are usually described with models of different nature: exponential forthe former and inverse power law for the latter. Moreover, the model functionsoften have different dimensionality, e.g. the chromospheric distribution maydepend solely on solar altitude, while the coronal number density may be afunction of both altitude and latitude. For applications which need to considerboth chromospheric and coronal models, the chromosphere-corona boundary, wherethese functions have different values as well as gradients, can lead tonumerical problems. We encountered this problem in context of ray tracingthrough the corona at low radio frequencies, as a part of effort to prepare forthe analysis of solar images from new generation radio arrays like theMurchison Widefield Array (MWA), Low Frequency Array (LOFAR) and LongWavelength Array (LWA). We have developed a solution to this problem by using a{\em patch} function, a thin layer between the chromosphere and the coronawhich matches the values and gradients of the two regions at their respectiveinterfaces. We describe the method we have developed for defining this patchfunction to seamlessly "stitch" chromospheric and coronal electron densitydistributions, and generalize the approach to work for any arbitrarydistributions of different dimensionality. We show that the complexity of thepatch function is independent of the stitched functions dimensionalities. Italways has eight parameters (even four for univariate functions) and they maybe found without linear system solution for every point. The developed methodcan potentially be useful for other applications.

A Method for Smooth Merging of Electron Density Distributions at the Chromosphere-Corona Boundary