Densities and filling factors of the DIG in the Solar neighbourhood

TL;DR

This study combines dispersion and emission measures towards pulsars to derive the electron density and filling factors of the diffuse ionized gas in the Solar neighborhood, revealing a fractal, turbulent structure.

Contribution

First combined dispersion and emission measures towards pulsars to analyze the electron density and filling factors of the DIG in the Solar neighborhood.

Findings

Electron scale height is 0.93+/-0.13 kpc.

Mean electron density along line of sight is 0.018+/-0.002 cm^-3.

Inverse relation between filling factor and cloud density supports a fractal, turbulent structure.

Abstract

For the first time we have combined dispersion measures and emission measures towards 38 pulsars at KNOWN distances from which we derived the mean electron density in clouds, N_c, and their volume filling factor, F_v, averaged along the line of sight. The emission measures were corrected for absorption by dust and contributions from beyond the pulsar distance. Results: The scale height of the electron layer for our sample is 0.93+/-0.13 kpc and the midplane electron density is 0.023+/-0.004 cm^-3, in agreement with earlier results. The average density along the line of sight is <n_e> = 0.018+/-0.002 cm^-3 and nearly constant. Since <n_e> = F_v N_c, an inverse relationship between F_v and N_c is expected. We find F_v(N_c) = (0.011+/-0.003) N_c^{-1.20+/-0.13}, which holds for the ranges N_c = 0.05-1 cm^-3 and F_v = 0.4-0.01. Near the Galactic plane the dependence of F_v on N_c is significantly stronger than away from the plane. F_v does not systematically change along or perpendicular to the Galactic plane, but the spread about the mean value of 0.08+/-0.02 is considerable. Conclusions: The inverse F_v-N_c relation is consistent with a hierarchical, fractal density distribution in the diffuse ionized gas (DIG) caused by turbulence. The observed near constancy of <n_e> then is a signature of fractal structure in the ionized medium, which is most pronounced outside the thin disk.