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Rotating Boson Stars

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Relativity and Scientific Computing

Summary

Scalar fields bound by their own gravitational field can form absolutely stable boson stars, resembling neutron stars. Within general relativity we construct for the first time the corresponding localized rotating configurations via numerical integration of the coupled Einstein-Klein-Gordon equations. The ratio of conserved angular momentum and particle number turns out to be an integer b, the gravitomagnetic quantum number of our soliton-type stars. The resulting axisymmetric metric, the energy density, and the Tolman mass are completely regular. Moreover, we analyze the differential rotation of such fully relativistic configurations.

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Author information

Authors and Affiliations

  1. Institute for Theoretical Physics, University of Cologne, Germany

    Franz E. Schunck

  2. Departmento de Física, Universidad Autónoma Metropolitana-Iztapalapa, México

    Eckehard W. Mielke

Authors
  1. Franz E. Schunck
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  2. Eckehard W. Mielke
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Editors and Affiliations

  1. Institut für Theoretische Physik, Universität zu Köln, D-50923, Köln, Germany

    Friedrich W. Hehl  & Roland A. Puntigam  & 

  2. Institut für Astronomie und Astrophysik, Universität Tübingen, Auf der Morgenstelle 10, D-72076, Tübingen, Germany

    Hanns Ruder

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© 1996 Springer-Verlag Berlin Heidelberg

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Schunck, F.E., Mielke, E.W. (1996). Rotating Boson Stars. In: Hehl, F.W., Puntigam, R.A., Ruder, H. (eds) Relativity and Scientific Computing. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-95732-1_7

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  • DOI: https://doi.org/10.1007/978-3-642-95732-1_7

  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-642-95734-5

  • Online ISBN: 978-3-642-95732-1

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