Data di Pubblicazione:
2015
Citazione:
Polytropic models of filamentary interstellar clouds - I. Structure and stability / C. Toci, D. Galli. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 446:2(2015 Jan 11), pp. 2110-2117. [10.1093/mnras/stu2168]
Abstract:
The properties of filamentary interstellar clouds observed at submillimetre wavelengths, especially by the Herschel Space Observatory, are analysed with polytropic models in cylindrical symmetry. The observed radial density profiles are well reproduced by negative-index cylindrical polytropes with polytropic exponent 1/3 ≲ γp ≲ 2/3 (polytropic index -3 ≲ n ≲ -3/2), indicating either external heating or non-thermal pressure components. However, the former possibility requires unrealistically high gas temperatures at the filament's surface and is therefore very unlikely. Non-thermal support, perhaps resulting from a superposition of small-amplitude Alfvén waves (corresponding to γp = 1/2), is a more realistic possibility, at least for the most massive filaments. If the velocity dispersion scales as the square root of the density (or column density) on the filament's axis, as suggested by observations, then polytropic models are characterized by a uniform width. The mass per unit length of pressurebounded cylindrical polytropes depends on the conditions at the boundary and is not limited as in the isothermal case. However, polytropic filaments can remain stable to radial collapse for values of the axis-to-surface density contrast as large as the values observed only if they are supported by a non-isentropic pressure component.
Tipologia IRIS:
01 - Articolo su periodico
Keywords:
Instabilities; ISM: clouds
Elenco autori:
C. Toci, D. Galli
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