, MIT Kavli Institute for Astrophysics and Space Research
[Host: Alexander Saffer]
After having observed gravitational waves from a population of nearly 100 compact-object binaries, we are now in a position where we can start probing their internal structure and how they can be deformed by the strong tidal fields in which the binaries exist.
I will present current observational constraints of the Neutron Star Equation of State from gravitational-wave observations, and discuss some of the potential complications and limitations the observations over the coming years might bring as the sensitivity of the gravitational-wave detectors are improved. I will also showcase a study about what possibilities the next generation of gravitational-wave detectors will bring, and what being able to observe a population of neutron stars at cosmological distances will teach us.
Finally, I will present a study focusing on the observed “non-Neutron Stars”, and if they can be described as compact objects other than Black Holes. This can be done by extending the Black Hole description to also allow for them to be tidally deformed following the behavior of a uniform-density ultracompact star (Schwarzschild star). Assuming that the population of Binary Black Holes, as observed in gravitational waves instead can be described as binaries of these Schwarzschild stars I present strong constraints on their compactness and tidal deformability, both as individual objects and for the population at large. Through these constraints, I comment on the viability of other categories of Black Hole mimickers as constituents of the ultracompact-object binaries observed so far.
Monday, May 2, 2022
Physics, Room 313
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