Hybrid magnetized stars within the Field Correlator Method. (arXiv:1902.02814v1 [astro-ph.HE])

<a href="http://arxiv.org/find/astro-ph/1/au:+Mariani_M/0/1/0/all/0/1">Mauro Mariani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orsaria_M/0/1/0/all/0/1">Milva G. Orsaria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ranea_Sandoval_I/0/1/0/all/0/1">Ignacio F. Ranea-Sandoval</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guilera_O/0/1/0/all/0/1">Octavio M. Guilera</a>

We present preliminary results of the study of intense magnetic fields

effects on hybrid stars. For the description of the hadronic phase, we use the

relativistic mean field approximation. For the quark matter phase, we employ

the Field Correlator Method formalism. Once the the equation of state is built,

we discuss the pressure anisotropy due the presence of the strong magnetic

field. Finally, we calculate the structure of the compact stars using

magnetized hybrid equations of state and their oscillation modes related with

the emission of gravitational waves.

We present preliminary results of the study of intense magnetic fields

effects on hybrid stars. For the description of the hadronic phase, we use the

relativistic mean field approximation. For the quark matter phase, we employ

the Field Correlator Method formalism. Once the the equation of state is built,

we discuss the pressure anisotropy due the presence of the strong magnetic

field. Finally, we calculate the structure of the compact stars using

magnetized hybrid equations of state and their oscillation modes related with

the emission of gravitational waves.

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