Density Distribution of the Warm Ionized Medium
| dc.creator | Hill, Alex S. | |
| dc.creator | Reynolds, Ronald J. | |
| dc.creator | Benjamin, Robert A. | |
| dc.creator | Haffner, L. Matthew | |
| dc.date | 2007-01-16 | |
| dc.date.accessioned | 2026-07-07T07:41:11Z | |
| dc.date.available | 2026-07-07T07:41:11Z | |
| dc.description | Observations of Halpha emission measures and pulsar dispersion measures at high Galactic latitude (|b| > 10 deg) provide information about the density and distribution of the diffuse warm ionized medium (WIM). The diffuse WIM has a lognormal distribution of EM sin |b|, which is consistent with a density structure established by isothermal turbulence. The H+ responsible for most of the emission along high-EM sin |b| sightlines is clumped in high density (> 0.1 cm^{-3}) regions that occupy only a few parsecs along the line of sight, while the H+ along low-EM sightlines occupies hundreds of parsecs with considerably lower densities. | |
| dc.description | To appear in the proceedings of the "SINS - Small Ionized and Neutral Structures in the Diffuse Interstellar Medium" conference, eds. M. Haverkorn and W.M. Goss | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0701477 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0701477 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/122010 | |
| dc.subject | Astrophysics | |
| dc.title | Density Distribution of the Warm Ionized Medium | |
| dc.type | text |