ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Proposal I-Proposal B-Proposal I-Proposal I-Proposal I-Proposal I-Proposal I-Proposal I-Proposal O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software I-Software B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O B-Model O O O O O O O O O B-Software B-Citation I-Citation I-Citation I-Citation O B-Citation O B-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O B-Software I-Software O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O B-Software O B-Software O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O
tokens: for the cold molecular phase. As this is the phase with the strongest magnetic fields as well as the phase in which star formation occurs, it is important to follow the evolution of the magnetized ISM together with its chemical evolution. In this study, which is part of the SILCC project (SImulating the Life-Cycle of molecular Clouds 1 ), we investigate the interplay between the chemical evolution of the SN-driven ISM and the magnetic field evolution. We use three-dimensional MHD simulations including a chemical network and shielding from an interstellar radiation field to explore how magnetic fields alter the formation of molecular gas in the ISM. We present the details of the simulations, the numerical methods and parameters, describing the chemistry network, the SN implementation, the list of simulations and the initial conditions in Section 2 . We discuss the morphological evolution of the simulations in Section 3 . The chemical evolution is described in Section 4 together with the magnetic field evolution and the influence of self-gravity. In this section we also evaluate the thermal, magnetic and kinetic energy density (Subsection 4.1 ). In Section 4.2 we show the magnetic field scaling and present our conclusions in Section 5 . 2 NUMERICAL METHOD, PARAMETERS AND SIMULATIONS 2.1 Numerical method We simulate the chemical, thermal and dynamical evolution of gas driven by SN feedback in a periodic volume using the Eulerian, adaptive mesh refinement (AMR), three-dimensional, magnetohydrodynamic code flash 4 (Fryxell etal. 2000 ; Dubey etal. 2008 ). To solve the ideal MHD equations, we use the directionally split three-wave MHD solver hll3r (Bouchut, Klingenberg Waagan 2007 , 2010 ; Waagan 2009 ; Waagan, Federrath Klingenberg 2011 ). Our simulations account for the effects of gas cooling and chemical evolution (Section 2.2 ) and SN feedback (Section 2.3 ) using an approach very similar to the one adopted by Gatto etal. ( 2015 ). Further details of our modifications to flash can also be found in Walch etal. ( 2015 ) and Girichidis etal. ( 2016 ). 2.2 Gas cooling and chemistry The simplified chemical network follows the evolution of seven chemical species (H , H, H 2 , C , O, CO and free electrons) and is based on the hydrogen chemistry of Glover Mac Low ( 2007a , b ) and the CO chemistry of Nelson Langer ( 1997 ). We model the effects of radiative cooling and diffuse heating by cosmic rays, X-rays and the interstellar radiation field (see Glover etal. 2010 ; Glover Clark 2012 ; Walch etal. 2015 ). Cooling by metals in hot ionized gas is modelled using rates from Gnat Ferland ( 2012 ), as outlined in Walch etal. ( 2015 ). Dust shielding and molecular self-shielding are included using the TreeCol algorithm developed by Clark, Glover Klessen ( 2012 ). Full details of the implementation of the chemical network and the coupling of TreeCol with flash are described by Walch etal. ( 2015 ) and Wnsch etal. (in preparation). In the simulations presented