Fig. 1-1: Initial Configuration of Black Hole and Neutron Star |

Here, we plot the entropy profile in the matter as measured by K/K_{0}, where K = P/ρ^{ Γ} and K_{0} = K at t = 0 Shock heating causes the ratio K/K_{0} to increase above unity. Here we show the first four orbits.

In the clip, the entropy of the star K/K_{0} is plotted on a logarithmic scale. The remaining evolution is shown here. No magnetic field is present in this case.

Fig. 2-1: Entropy profile at time t/M = 633 |
Fig. 2-2: Entropy profile at time t/M = 882 |

Fig. 2-3: Entropy profile at time t/M = 974 |
Fig. 2-4: Entropy profile at time t/M = 2072 |

In the clip, the entropy of the star K/K_{0} is plotted on a logarithmic scale.After four orbits, the unmagnetized interior of the unmagnetized neutron star is seeded with a purely poloidal magnetic field parallel to the spin axis of the black hole . With an average magnetic-to-gas pressure of 0.5%, the magnetic fields are dynamically unimportant to the neutron star.

Fig. 3-1: Entropy profile at time t/M = 633 |
Fig. 3-2: Entropy profile at time t/M = 882 |

Fig. 3-3: Entropy profile at time t/M = 974 |
Fig. 3-4: Entropy profile at time t/M = 2072 |

In the clip, the entropy of the star K/K_{0} is plotted on a logarithmic scale. After four orbits, the unmagnetized interior of the unmagnetized neutron star is seeded with a purely poloidal magnetic field tilted 45^{o} with respect to the spin axis of the black hole. With an average magnetic-to-gas pressure of 0.5%, the magnetic fields are dynamically unimportant to the neutron star.

Fig. 4-1: Entropy profile at time t/M = 633 |
Fig. 4-2: Entropy profile at time t/M = 882 |

Fig. 4-3: Entropy profile at time t/M = 974 |
Fig. 4-4: Entropy profile at time t/M = 2072 |

In the clip, the entropy of the star K/K_{0} is plotted on a logarithmic scale. After four orbits, the unmagnetized interior of the unmagnetized neutron star is seeded with a purely poloidal magnetic field tilted perpendicular with respect to the spin axis of the black hole. With an average magnetic-to-gas pressure of 0.5%, the magnetic fields are dynamically unimportant to the neutron star.

Fig. 5-1: Entropy profile at time t/M = 633 |
Fig. 5-2: Entropy profile at time t/M = 882 |

Fig. 5-3: Entropy profile at time t/M = 974 |
Fig. 5-4: Entropy profile at time t/M = 2072 |

In the clip, the entropy of the star K/K_{0} is plotted on a logarithmic scale. After four orbits, the unmagnetized interior of the unmagnetized neutron star is seeded with a magnetic field parallel (top right), tilted 45^{o} (bottom left), and perpendicular (bottom right) to their orbital axis. The top left star is left unmagnetized. With an average magnetic-to-gas pressure of 0.5%, these magnetic fields are dynamically unimportant to the neutron star.

Fig. 6-1: Entropy profiles at time t/M = 633 |
Fig. 6-2: Entropy profiles at time t/M = 882 |

Fig. 6-3: Entropys profile at time t/M = 974 |
Fig. 6-4: Entropy profiles at time t/M = 2072 |

Given the weakness of the initial magnetic field in all the cases, there is very little difference in the entropy evolution between the four cases. Approximately 14% of the neutron star rest-mass remains outside the remnant black hole in all cases.