Crustal oscillations of slowly rotating relativistic stars
Corresponding Author
M. Vavoulidis
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
E-mail: [email protected]Search for more papers by this authorK. D. Kokkotas
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
Theoretical Astrophysics, Eberhard-Karls University of Tübingen, 72076 Tübingen, Germany
Search for more papers by this authorA. Stavridis
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
Search for more papers by this authorCorresponding Author
M. Vavoulidis
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
E-mail: [email protected]Search for more papers by this authorK. D. Kokkotas
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
Theoretical Astrophysics, Eberhard-Karls University of Tübingen, 72076 Tübingen, Germany
Search for more papers by this authorA. Stavridis
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
Search for more papers by this authorABSTRACT
We study low-amplitude crustal oscillations of slowly rotating relativistic stars consisting of a central fluid core and an outer thin solid crust. We estimate the effect of rotation on the torsional toroidal modes and on the interfacial and shear spheroidal modes. The results compared against the Newtonian ones for wide range of neutron star models and equations of state.
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