Chemo-dynamical model

Fig. 8.37. The different gaseous and stellar components connected via mass, momentum and energy exchange, with their principal interactions, in the chemo-dynamical model of the Galaxy, after Samland, Hensler and Theis (1997). Courtesy Gerhard Hensler.

Detected rotational H2 and ro-vibrational CO, CO2, C2H2, HCN, as well as H2O and OH lines trace hot gas in the inner, planet-forming disk zone with T > 300 K (Brittain et al. 2003 Lahuis et al. 2006 Salyk et al. 2008), see Fig. 4.3. These lines are a good measure of temperature and high-energy radiation fields, and presumably sensitive to disk accretion, which could be a stress-test for advanced chemo-dynamical models. In Table 4.1 the various molecules used to study protoplanetary disks are overviewed. 

Chapter 11 presents models used to study the continual interaction of the respiratory mechanical system and pulmonary gas exchange. Traditionally, the respiratory system is described as a chemo-stat — ventilation increases with increased chemical stimulation. Alternatively, the author proposes that quantitative description of the respiratory central pattern generator, a network of neuronal clusters in the brain, is a much more sophisticated and realistic approach. Study of this dynamic, optimized controller of a nonlinear plant is interesting from both physiological and engineering perspectives, the latter due to applications of these techniques for new, intelligent control system design. 

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