Retrieving "Local Interstellar Cloud" from the archives

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1. Heliosphere

   Linked via "local interstellar cloud"

   Structure and Boundaries
   The shape of the heliosphere is not perfectly spherical but is elongated downwind (tailward) due to the Sun (star)/)'s motion relative to the local interstellar cloud, creating a "heliotail." Measurements from the Voyager probes suggest the heliosphere is significantly compressed on the dayside due to the slight inherent viscosity of interstellar neutral particles, which resist simple deflection [4].
   The distance to the heliopause is highly dependent …

2. Number Density

   Linked via "Local Interstellar Cloud"

   In ionized gases (plasmas), number density often partitions into the density of ions ($ni$) and electrons ($ne$). The total particle density ($n{total}$) is the sum $ne + n_i$. In fusion research, the Lawson criterion mandates a minimum product of density and confinement time ($\tau$) for sustained reactions.
   Astrophysically, number density measurements are vital for characterizing [nebulae](/entries/…