Magnetic fields and chemical evolution in the disk of the Milky Way |
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| Authors: | E Battaner J Isern E Florido |
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| Institution: | (1) Departamento de Física Teórica y del Cosmos, Universidad de Granada, Spain;(2) Centre d'Estudis Avançats de Blanes, C.S.I.C., Spain;(3) Grup d'Astrofisica, I.E.C., Spain |
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| Abstract: | An alternative non-infall model for the chemical evolution in the solar neighbourhood is proposed. The evolution of the disk is divided into two phases. In phaseA, the magnetic field and the gas viscosity produced an outward flux of gas, forming and maintaining the ring observed today. This flux balanced the star formation in the ring. The number of stars increased until the beginning of phaseB, during which stellar viscosity generated an inward flux of stars towards the inner disk, while the magnetic fields continued supplying gas to the ring. The combination of these two effects brought the ring to a quasi-steady state, with a constant mass of gas and stars which we assume has continued till the present. A coherent picture is obtained in which the observational restrictions are explained without introducing any arbitrary hypothesis. The inward flux of stars in phaseB has transported the metal-poor G-dwards to the inner region, thus explaining their absence in the solar neighbourhood. |
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