Gravitational wave asteroseismology of dark matter hadronic stars
César V. Flores, César H. Lenzi, M. Dutra, O. Lourenço, José D. V. Arbañil
Abstract
The influence of the dark matter mass (<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:msub><a:mi>M</a:mi><a:mi>χ</a:mi></a:msub></a:math>) and the Fermi momentum (<c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:msubsup><c:mi>k</c:mi><c:mi>F</c:mi><c:mi mathsize="small">DM</c:mi></c:msubsup></c:math>) on the <f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:msub><f:mi>f</f:mi><f:mn>0</f:mn></f:msub></f:math>-mode oscillation frequency, damping time parameter, and tidal deformability of hadronic stars are studied by employing a numerical integration of hydrostatic equilibrium, nonradial oscillation, and tidal deformability equations. The matter inside the hadronic stars follows the NL3* equation of state. We obtain that the influence of <h:math xmlns:h="http://www.w3.org/1998/Math/MathML" display="inline"><h:msub><h:mi>M</h:mi><h:mi>χ</h:mi></h:msub></h:math> and <j:math xmlns:j="http://www.w3.org/1998/Math/MathML" display="inline"><j:msubsup><j:mi>k</j:mi><j:mi>F</j:mi><j:mi mathsize="small">DM</j:mi></j:msubsup></j:math> is observed in the <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>f</m:mi><m:mn>0</m:mn></m:msub></m:math>-mode, damping tome parameter, and tidal deformability. Finally, the correlation between the tidal deformability of the GW170817 event with <o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:msub><o:mi>M</o:mi><o:mi>χ</o:mi></o:msub></o:math> and <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:msubsup><q:mi>k</q:mi><q:mi>F</q:mi><q:mi mathsize="small">DM</q:mi></q:msubsup></q:math> are also investigated. Published by the American Physical Society 2024