12
views
0
recommends
+1 Recommend
0 collections
    0
    shares
      • Record: found
      • Abstract: found
      • Article: not found

      Magnetohydrodynamic effect on first star formation: pre-stellar core collapse and protostar formation

      Read this article at

      ScienceOpenPublisher
      Bookmark
          There is no author summary for this article yet. Authors can add summaries to their articles on ScienceOpen to make them more accessible to a non-specialist audience.

          ABSTRACT

          Recent theoretical studies have suggested that a magnetic field may play a crucial role in the first star formation in the universe. However, the influence of the magnetic field on the first star formation has yet to be understood well. In this study, we perform three-dimensional magnetohydrodynamic simulations taking into account all the relevant cooling processes and non-equilibrium chemical reactions up to the protostar density, in order to study the collapse of magnetized primordial gas cores with self-consistent thermal evolution. Our results show that the thermal evolution of the central core is hardly affected by a magnetic field because magnetic forces do not prevent the contraction along the field lines. We also find that the magnetic braking extracts the angular momentum from the core and suppresses fragmentation depending on the initial strength of the magnetic field. The angular momentum transport by the magnetic outflows is less effective than that by the magnetic braking because the outflows are launched only in a late phase of the collapse. Our results indicate that the magnetic effects become important for the field strength $B\gt 10^{-8}(n_{\rm H}/1\ \rm cm^{-3})^{2/3}\ \rm G$, where nH is the number density, during the collapse phase. Finally, we compare our results with simulations using a barotropic approximation and confirm that this approximation is reasonable at least for the collapse phase. Nevertheless, self-consistent treatment of the thermal and chemical processes is essential for extending simulations to the accretion phase, in which radiative feedback by protostars plays a crucial role.

          Related collections

          Most cited references84

          • Record: found
          • Abstract: not found
          • Article: not found

          The Formation of the First Stars. I. The Primordial Star‐forming Cloud

            Bookmark
            • Record: found
            • Abstract: not found
            • Article: not found

            Simulations of Early Structure Formation: Primordial Gas Clouds

              Bookmark
              • Record: found
              • Abstract: not found
              • Article: not found

              Thermal and Fragmentation Properties of Star‐forming Clouds in Low‐Metallicity Environments

                Bookmark

                Author and article information

                Contributors
                (View ORCID Profile)
                Journal
                Monthly Notices of the Royal Astronomical Society
                Oxford University Press (OUP)
                0035-8711
                1365-2966
                August 2021
                June 23 2021
                August 2021
                June 23 2021
                May 14 2021
                : 505
                : 3
                : 4197-4214
                Affiliations
                [1 ]Astronomical Institute, Tohoku University, Aoba, Sendai, Miyagi 980-8578, Japan
                [2 ]Department of Astronomy, University of Maryland, College Park, MD 20740, USA
                [3 ]Faculty of Sustainability Studies, Hosei University, Fujimi, Chiyoda, Tokyo 102-8160, Japan
                Article
                10.1093/mnras/stab1330
                6d89d63a-6cf8-4631-ba6d-8874aaea8c38
                © 2021

                https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model

                History

                Comments

                Comment on this article