@Article{SartorioVanFalWooNet:2019:EfPhFe,
               author = "Sartorio, Nina Sanches and Vandenbroucke, B. and 
                         Falceta-Gon{\c{c}}alves, Diego and Wood, K. and Neto, E.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {University 
                         of St Andrews} and {Instituto Nacional de Pesquisas Espaciais 
                         (INPE)} and {University of St Andrews} and {Harvard-Smithsonian 
                         Center for Astrophysics}",
                title = "Massive star formation via torus accretion: the effect of 
                         photoionization feedback",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2019",
               volume = "486",
               number = "4",
                pages = "5171--5183",
                month = "July",
             keywords = "radiative transfer, methods: numerical, stars: massive, H II 
                         regions, accretion discs.",
             abstract = "The formation of massive stars is a longstanding problem. Although 
                         a number of theories of massive star formation exist, ideas appear 
                         to converge to a disc-mediated accretion scenario. Here, we 
                         present radiative hydrodynamic simulations of a star-accreting 
                         mass via a disc embedded in a torus. We use a Monte Carlo based 
                         radiation hydrodynamics code to investigate the impact that 
                         ionizing radiation has on the torus. Ionized regions in the torus 
                         midplane are found to be either gravitationally trapped or in 
                         pressure-driven expansion depending on whether or not the size of 
                         the ionized region exceeds a critical radius. Trapped H II regions 
                         in the torus plane allow accretion to progress, while expanding H 
                         II regions disrupt the accretion torus preventing the central star 
                         from aggregating more mass, thereby setting the stars final mass. 
                         We obtain constraints for the luminosities and torus densities 
                         that lead to both scenarios.",
                  doi = "10.1093/mnras/stz1187",
                  url = "http://dx.doi.org/10.1093/mnras/stz1187",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "sartorio.pdf",
        urlaccessdate = "24 abr. 2024"
}