1. Phil Rosenfield, Fridolin Weber, Horst Lenske

2.  Neutron stars: a short synopsis  The structure of neutron stars  Modeling neutron stars  The equation of state  Rotating or non-rotating  Two results  Conclusions

3. A neutron star is left over from the supernova of a star not massive enough to leave a black hole.

4.  Mass: 1-2 M Sun  Radius: 10 - 15 km  Huge magnetic fields  Extremely dense  Fastest Rotation Rate: 1122 Hz  10 7 − 9 in a typical galaxy If I could get my bike tires going that fast, I’d be moving at 1,700 mph. On the surface of a typical sized neutron star, particles are moving at 80%c! If I could get my bike tires going that fast, I’d be moving at 1,700 mph. On the surface of a typical sized neutron star, particles are moving at 80%c! Objects that don’t make sense, that can’t be explained with current theories, are the guides that lead us to better understanding our universe.

6. NON ROTATING  Spherically Symmetric  Curved space-time ROTATING  Poles shrink, equator bulges  Maximum rotation rate  Frame dragging

7. MASS-EQUATORIAL RADIUS  Rotation  Larger Radius PERIOD-MASS  Rotation  More mass

8.  Rotation matters  These equations of state can explain the fastest spinning neutron stars What’s Next Going to grad school – hope to look for more neutron stars What’s Next Going to grad school – hope to look for more neutron stars