Unraveling the Properties of Ultradense Matter with Neutron Star Merger Simulations
ORAL · Invited
Abstract
Neutron stars are fascinating laboratories for strong gravity, multi-messenger astronomy and nuclear physics.
In this talk, I will review how the merger of two neutron stars can shed light on the behavior of nuclear matter at densities beyond saturation. Using state-of-the-art neutron star merger simulations, I will show how quark deconfinement can appear in the post-merger remnant, and what signatures this transition might leave in the gravitational wave signal.
More generally, such post-merger gravitational wave emission has been proposed as a future probe of the dense matter equation of state. As a particular example, I will show how the slope L of the nuclear symmetry energy can affect this emission and how it is imprinted in the post-merger dynamics.
As an outlook, I will conclude with an assessment of how viscosity could affect the collision and merger dynamics, akin to viscous effects in heavy-ion collisions.
In this talk, I will review how the merger of two neutron stars can shed light on the behavior of nuclear matter at densities beyond saturation. Using state-of-the-art neutron star merger simulations, I will show how quark deconfinement can appear in the post-merger remnant, and what signatures this transition might leave in the gravitational wave signal.
More generally, such post-merger gravitational wave emission has been proposed as a future probe of the dense matter equation of state. As a particular example, I will show how the slope L of the nuclear symmetry energy can affect this emission and how it is imprinted in the post-merger dynamics.
As an outlook, I will conclude with an assessment of how viscosity could affect the collision and merger dynamics, akin to viscous effects in heavy-ion collisions.
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Presenters
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Elias R Most
Princeton University
Authors
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Elias R Most
Princeton University