Small-scale dissipative structures of diffuse ISM turbulence: I- CO diagnostics
| dc.creator | Hily-Blant, Pierre | |
| dc.creator | Pety, Jerome | |
| dc.creator | Falgarone, Edith | |
| dc.date | 2007-01-11 | |
| dc.date.accessioned | 2026-07-07T07:39:54Z | |
| dc.date.available | 2026-07-07T07:39:54Z | |
| dc.description | Observations of translucent molecular gas in $^{12}$CO and $^{13}$CO emission lines, at high spectral and spatial resolutions, evidence different kinds of structures at small scales: (1) optically thin $^{12}$CO emission, (2) optically thick $^{12}$CO emission, visible in $^{13}$CO(1-0), and (3) regions of largest velocity shear in the field, found from a statistical analysis. They are all elongated with high aspect ratio, preferentially aligned with the plane-of-the-sky projection of the magnetic fields. The latter structures coincide with the former, shown to trace gas warmer and more diluted than average. Combining our data to large-scale observations of poorer spatial resolution, we show that the regions of largest velocity shear remain coherent over more than a parsec. These filaments are proposed to be the sites of the intermittent dissipation of turbulence. | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0701326 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0701326 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/121627 | |
| dc.subject | Astrophysics | |
| dc.title | Small-scale dissipative structures of diffuse ISM turbulence: I- CO diagnostics | |
| dc.type | text |