تقرير
On the evolution of irradiated turbulent clouds: A comparative study between modes of triggered star-formation
| العنوان: | On the evolution of irradiated turbulent clouds: A comparative study between modes of triggered star-formation |
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| المؤلفون: | Anathpindika, S., Bhatt, H. C. |
| سنة النشر: | 2012 |
| المجموعة: | Astrophysics |
| مصطلحات موضوعية: | Astrophysics - Astrophysics of Galaxies |
| الوصف: | Here we examine the evolution of irradiated clouds using the Smoothed Particle Hydrodynamics ({\small SPH}) algorithm coupled with a ray-tracing scheme that calculates the position of the ionisation-front at each timestep. We present results from simulations performed for three choices of {\small IR}-flux spanning the range of fluxes emitted by a typical {\small B}-type star to a cluster of {\small OB}-type stars. The extent of photo-ablation, of course, depends on the strength of the incident flux and a strong flux of {\small IR} severely ablates a {\small MC}. Consequently, the first star-formation sites appear in the dense shocked layer along the edges of the irradiated cloud. Radiation-induced turbulence readily generates dense filamentary structure within the photo-ablated cloud although several new star-forming sites also appear in some of the densest regions at the junctions of these filaments. Prevalent physical conditions within a {\small MC} play a crucial role in determining the mode, i.e., filamentary as compared to isolated pockets, of star-formation, the timescale on which stars form and the distribution of stellar masses. The probability density functions ({\small PDF}s) derived for irradiated clouds in this study are intriguing due to their resemblance with those presented in a recent census of irradiated {\small MC}s. Furthermore, irrespective of the nature of turbulence, the protostellar mass-functions({\small MF}s) derived in this study follow a power-law distribution. When turbulence within the cloud is driven by a relatively strong flux of {\small IR} such as that emitted by a massive {\small O}-type star or a cluster of such stars, the {\small MF} approaches the canonical form due to Salpeter, and even turns-over for protostellar masses smaller than $\sim$0.2 M$_{\odot}$. Comment: 13 pages, 19 figures, 3 tables. Rendered images of significantly lowered resolution have been deliberately submitted to stay within the maximum permissible limits of size. Also, the original abstract has been shortened. To be published by the Monthly Notices of the RAS |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.1111/j.1365-2966.2012.22094.x |
| URL الوصول: | http://arxiv.org/abs/1208.6114 |
| رقم الأكسشن: | edsarx.1208.6114 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.1111/j.1365-2966.2012.22094.x |
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