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• W180872384 abstract "The physics of the interstellar medium (ISM) and its processes play a key role in determining the formation and the evolution of the galaxies. The description of the ISM includes many interacting phenomena, namely the energy feedback, the chemical reactions between molecules and atoms, the physics of the dusts, the cooling, the heating and, finally, the interactions of the ISM with photons and with cosmic rays.The most important issue for the star formation process is the amount of cooling given by the roto-vibrational lines of the molecules (H2, HD, CO) and by the fine-structure lines of the metals. Since all the aforementioned phenomena take part to the formation of such coolants, we need an accurate description of these processes.In this framework we develop a model aimed at the study of the ISM.This model includes a large number of physical processes such as a detailed chemical network including hydrogen-based species (H, H+, H−, H2, H+ 2 ), helium-based (He, He+, He++), metals and their ions (C, C+, O, O+, Si, Si+, Fe, Fe+), deuterium-based (D, D+, D−, D2, HD, HD+), and moleculescontaining carbon (CO, CH, CH+, CH2, CH+ 2 , CH3 and CH+ 3 ). The cooling model adopted uses the metals (including ions) and the molecules, considering the analysis of the statistical equilibrium for the excitation levels (where necessary). Moreover, the interaction of the UV photons with the gas, which determines the heating and the ionization of the ISM. The last ingredient is the dust which interacts with all the previous components; The temperature of the grains is determined by the impinging UV radiation, they catalyze the formation of molecules (such as molecular hydrogen), and provide cooling and heating to the surrounding medium. We also include their evolution and the influence of their different sizes in all the interactions listed above.All these processes of the ISM have their counterpart in the algorithms of a chemical/physical code called ROBO. The aim of this code is to study the ISM and the interplay of its phenomena.The results of the code ROBO are than used to describe the evolution of the phases of the ISM in a NB-TSPH cosmological simulation to study the star formation for different evolving galaxies. This class of simulation must take into account a wide range of chemical species to track the formation of the key-role molecules and atoms (H2, HD, CO and metals). In this sense, modeling the gas chemistry (and related processes) is crucial within this context.However, too detailed a chemistry reduces the computational performances of the evolutionary code. This requires the development of a strategy to optimize the accuracy of the model with the computational speed. One way to approach to this problem is to create a database in advance, which feeds the data to the main NB-TSPH simulation during the execution of the code. The database is then embedded into the NB-TSPH code using the Artificial Neural Networks.In this work we first discuss the physical phenomena of the ISM, than we introduce the code ROBO, which is the companion code of the ISM model, and finally we show how Artificial Neural Networks are included in such a scenario." @default.
• W180872384 created "2016-06-24" @default.
• W180872384 creator A5028900085 @default.
• W180872384 date "2011-01-30" @default.
• W180872384 modified "2023-09-27" @default.
• W180872384 title "ISM in numerical simulations: chemistry, energy feedbacks and related issues - numerical methods" @default.
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