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1992), modulations of stellar luminosity (Alexander and Morris 2003), and runaway tidal stripping of the star (Li and Loeb 2013). 1 Vertical Collapse and Crunch: (Semi-)Analytic Alternatively, if β 1, a violent and fully disruptive TDE will ensue. In phase II of a TDE, R < Rt and the star’s internal forces are subdominant to the tidal acceleration 18 1 Introduction it experiences. During this stage of stellar disruption, especially if β is large, the star undergoes approximate tidal free fall, with its fluid elements moving on roughly ballistic or geodesic trajectories (altered slightly by the subdominant internal forces).
Merging SMBH binaries provide copious sources of gravitational radiation for future space-based laser interferometers, or for existing Pulsar Timing Arrays (PTAs). Space-based laser interferometers, such as the European Space Agency’s planned eLISA instrument1 , are most sensitive to SMBH binaries with masses MBH ∼ 106 M . PTAs such as NANOGrav2 , the Parkes Pulsar Timing Array3 , or the European Pulsar Timing Array4 , are most sensitive to lower frequency GWs emitted by SMBHBs with total mass 108 M (Sesana et al.
Because the specific TDE rate is highest for low-mass galaxies (as can be seen in Fig. 8), and because low-mass galaxies are more numerous, it has long been thought that large samples of TDEs could serve as excellent probes for the uncertain bottom end of the SMBH mass function. 3 Tidal Disruption Rates in Realistic Galaxies 39 with stellar bulge masses M > 109 M are believed to host a central SMBH, the occupation fraction below this mass is unclear. Estimating this occupation fraction represents an important scientific goal for future TDE observations.