The effect of clouds on the dynamical and chemical evolution of gas-rich dwarf galaxies

By S. Recchi, Gerhard Hensler. 2000

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We study the effects of clouds on the dynamical and chemical evolution of gas-rich dwarf galaxies, in particular focusing on two model galaxies similar to IZw18 and NGC 1569. We consider both scenarios, clouds put at the beginning of the simulation and continuously created infalling ones. Due to dynamical processes and thermal evaporation, the clouds survive only a few tens of Myr, but during this time they act as an additional cooling agent and the internal energy ofcloudy models is typically reduced by 20–40% in comparison with models without clouds. The clouds delay the development of large-scale outflows, therefore helping to retain a larger amount of gas inside the galaxy. However, especially in models with continuous creation of infalling clouds, their bullet effect can pierce the expanding supershell and create holes through which the superbubble can vent freshly produced metals. Moreover, assuming a pristine chemical composition for the clouds, their interaction with the superbubble dilutes the gas, reducing the metallicity (by up to ∼0.4 dex) with respect to the one attained by diffuse models (© 2009 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c2722b1589e267ff68de9816ecd2054387574c1e

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Citations in the corpus

Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, background): “We assume that initial asymmetries in the distribution of gas allow to vent out the SN II ejecta along preferential directions, creating an “hourglass” cavity, and leaving part of the pristine gas in a substantially unperturbed torus at the outskirts of the cluster (e.g. Recchi et al. 2001).”
Breathing in Low-Mass Galaxies: A Study of Episodic Star Formation (2007, unknown): “44 94 v1 [ as tr oph ] 3 1 M ay 2 00 7 Low & Ferrara 1999; Scannapieco et al. 2000, 2001; Recchi et al. 2001; Efstathiou 2000; Fragile et al. 2003; Fujita et al. 2003; Pelupessy et al. 2004; Hensler et al. 2004; Marcolini et al. 2006).”
Europium production: neutron star mergers versus core-collapse supernovae (2013, result): “…we think that I.M.A. is not a bad assumption on the scale of the solar vicinity also because, besides the above mentioned results of Spitoni et al. (2009), it has been shown (Recchi et al. 2001) that mixing in the ISM can occur on very short timescales of the order of tens of million years.”
Oxygen, carbon and nitrogen evolution in galaxies (2002, methodology): “In particular, we adopt the best prescription for the energetics given in Recchi (2001) and Recchi et al. (2001): we assume a low thermalization efficiency for type II SNe (ηII = 0.03) and a maximun value for SNeIa (ηIa = 1.0); for the stellar winds we adopt a thermalization efficiency of ηw = 0.03.”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, methodology): “We have adopted this strategy - as is often done (e.g. Recchi et al. 2001; Lia et al. 2002; Sommer-Larsen et al. 2005; Romeo et al. 2006; Tornatore et al. 2007) - and have implemented it as follows5.”
Chemical Abundance Distributions of Galactic Halos and Their Satellite Systems in a ΛCDM Universe (2005, background): “…hence star formation in satellites are truncated upon accretion in our model it will not reproduce any recent significant star formation and chemical enrichment histories of the few surviving gas rich systems like LMC and SMC, for which extended chemical modeling may be needed (Recchi et al. 2001).”