@Article{GribelMiraVila:2017:CoCoSt,
               author = "Gribel, Carolina and Miranda, Oswaldo Duarte and Vilas-Boas, 
                         Jos{\'e} Williams",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)}",
                title = "Connecting the cosmic star formation rate with the local star 
                         formation",
              journal = "The Astrophysical Journal",
                 year = "2017",
               volume = "849",
               number = "108",
                pages = "1--15",
                month = "Nov.",
             keywords = "dark matter – galaxies: halos – galaxies: ISM – large-scale 
                         structure of universe – stars: formation – turbulence.",
             abstract = "We present a model that unifies the cosmic star formation rate 
                         (CSFR), obtained through the hierarchical structure formation 
                         scenario, with the (Galactic) local star formation rate (SFR). It 
                         is possible to use the SFR to generate a CSFR mapping through the 
                         density probability distribution functions commonly used to study 
                         the role of turbulence in the star-forming regions of the Galaxy. 
                         We obtain a consistent mapping from redshift z ~ 20 up to the 
                         present (z = 0). Our results show that the turbulence exhibits a 
                         dual character, providing high values for the star formation 
                         efficiency ({\'a}eñ ~ 0.32) in the redshift interval z ~ 3.5 20 
                         and reducing its value to {\'a}eñ = 0.021 at z = 0. The value of 
                         the Mach number (\crit), from which {\'a}eñ rapidly 
                         decreases, is dependent on both the polytropic index (\Γ) 
                         and the minimum density contrast of the gas. We also derive 
                         Larsons first law associated with the velocity dispersion 
                         ({\'a}Vrmsñ) in the local star formation regions. Our model shows 
                         good agreement with Larsons law in the ~10 50 pc range, providing 
                         typical temperatures T0 ~ 10 80 K for the gas associated with star 
                         formation. As a consequence, dark matter halos of great mass could 
                         contain a number of halos of much smaller mass, and be able to 
                         form structures similar to globular clusters. Thus, Larsons law 
                         emerges as a result of the very formation of large-scale 
                         structures, which in turn would allow the formation of galactic 
                         systems, including our Galaxy.",
                  doi = "10.3847/1538-4357/aa921a",
                  url = "http://dx.doi.org/10.3847/1538-4357/aa921a",
                 issn = "0004-637X",
             language = "en",
           targetfile = "gribel_connecting.pdf",
        urlaccessdate = "27 abr. 2024"
}