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The ratio of the rms electron density fluctuations to the background densityin the solar wind (density modulation index, $\epsilon_{N} \equiv \Delta{N}/N$)is of vital importance in understanding several problems in heliosphericphysics related to solar wind turbulence. In this paper, we have investigatedthe behavior of $\epsilon_{N}$ in the inner-heliosphere from 0.26 to 0.82 AU.The density fluctuations $\Delta{N}$ have been deduced using extensiveground-based observations of interplanetary scintillation (IPS) at 327 MHz,which probe spatial scales of a few hundred km. The background densities ($N$)have been derived using near-Earth observations from the Advanced CompositionExplorer ($\it{ACE}$). Our analysis reveals that $0.001 \lesssim \epsilon_{N}\lesssim 0.02$ and does not vary appreciably with heliocentric distance. Wealso find that $\epsilon_{N}$ declines by 8% from 1998 to 2008. We discuss theimpact of these findings on problems ranging from our understanding of Forbushdecreases to the behavior of the solar wind dynamic pressure over the recentpeculiar solar minimum at the end of cycle 23..

A study of density modulation index in the inner heliospheric solar wind during solar cycle 23