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Nuclear physics experiments with gravitational wave interferometers Andrew MELATOS, University of Melbourne Neutron stars are currently the only natural settings where one can study experimentally the fundamental physics of bulk nuclear matter in the true many-body limit. Gravitational waves in the hectohertz band will provide unprecedented opportunities to explore this physics by measuring directly the internal motions of neutron stars. In this review, examples are given of how gravitational-wave data can be inverted to infer the thermodynamic coefficients (e.g. compressibility, viscosity), state of superfluidity, and electrical properties (e.g. resistivity, state of magnetization) of nuclear matter. Experiments are identified which would benefit especially from the availability of a worldwide detector network. (1) With respect to isolated neutron stars, it is shown that rotational glitches observed in radio pulsars are promising sources which, under some scenarios, approachthe detectability limit of Advanced LIGO. Glitches emit a two-part signal, a sub-second burst followed by a continuous tone lasting for days/weeks. The burst maps the motion of quantized superfluid vortices in the star; if detected, it would be the first direct proof that bulk nuclear matter is indeed a quantum fluid. The continuous tone arises as the star responds hydrodynamically to the glitch; its spectrum and polarization depend in a calculable way on the nuclear compressibility and viscosity. Results are presented from recent microscopic (Gross-Pitaevskii) and macroscopic (two-fluid) numerical simulations to illustrate these effects as well as their astrophysical implications, e.g. quantifying differential rotation inside neutron stars and tying down the glitch mechanism, which remains an unsolved problem after 40 years. A detector network will assist these studies, because the first detections are likely to be radio-silent objects nearby, whereupon gravitational-wave triangulation is critical. (2) With respect to accreting neutron stars, it is already possible to place interesting gravitational-wave-based limits on nuclear physics. Strong indirect evidence exists (e.g. from X-ray data on spins) that neutron stars in low-mass X-ray binaries have sizeable quadrupoles, with Sco X-1 plausibly detectable by Advanced LIGO. A detection will constrain the elasticity and breaking strain of nuclear matter in its crystalline state (in the crust) as well as its composition (e.g. hyperon-rich matter sustains larger quadrupoles than normal). If the quadrupole arises from asymmetric electron capture reactions, the nuclear reaction rate, thermal conductivity, and state of superfluidity can be inferred in principle. If the quadrupole arises from magnetic funneling, the electrical resistivity and crustal adiabatic index can be inferred. It is argued that indirect (gravitational-wave spin-down) limits already challenge theoretical resistivity calculations. Detection of a magnetic mountain quadrupole, e.g. in Sco X-1, holds out the prospect of measuring directly the star's crustal magnetic field strength and geometry for the first time, thereby probing the origin and nature of high magnetization generally in compact astrophysical objects. Finally, if the quadrupole arises from r-modes, the gravitational-wave frequency depends on the equation of state, while the long-term persistence of the mode implies a lower limit on the strange quark fraction. The main benefit of a detector network for these sources is better sensitivity. (3) With respect to neutron star inspirals, tidal signatures in the gravitational-wave signal constrain the pressure at twice nuclear density to 10% or so, independently measuring the isospin asymmetry energy and nuclear compressibility. A detector network enhances these experiments by improving source localization, thus aiding the hunt for faint electromagnetic counterparts with good positions, so that the gravitational-wave detection can be refined to reduce the uncertainties in the nuclear quantities inferred.