Solar wind

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The continuous outflow of charged particles — mostly protons and electrons, with a minority of helium nuclei — escaping the Sun's corona in all directions and dragging the Sun's magnetic field out with it. It leaves the Sun supersonically, at speeds of several hundred kilometres per second, and thins out as it expands, so its density falls roughly as the inverse square of distance. It is the wind that inflates the heliosphere: the volume the solar wind fills is, by definition, the volume in which the Sun rather than the Galaxy sets the local plasma conditions. Voyager 1 lost the ability to measure it directly when its plasma science instrument failed in 1980; Voyager 2 kept that instrument working, which is why the 2018 crossing has a plasma measurement and the 2012 crossing had to be inferred another way. Not a place.

A node is not a place. Drawing it on a map would assert something about the world that no stored fact supports.