Isolated Neutron Stars Nils Andersson & Kostas Kokkotas mano a - PowerPoint PPT Presentation

Isolated Neutron Stars Nils Andersson & Kostas Kokkotas mano a mano

Want to use observations to probe matter at supranuclear densities. A “minimal” theory model requires: — supranuclear equation of state (hyperons, quarks etc.) — elastic crust (neutron superfluid+vortices) — magnetic field (configuration, currents?) — temperature profiles (exotic cooling mechanisms?) — superfluid/superconductors (vortices vs flux tubes?) — rotation (various instabilities) — relativistic gravity [courtesy Dany Page]

6000 30000 4000 B1338-62 J0537-6910 B0833-45 3000 4000 20000 2000 2000 10000 1000 0 0 0 51000 52000 53000 54000 40000 44000 48000 52000 47000 48000 49000 50000 51000 6000 2500 B1737-30 B1757-24 B1758-23 10000 2000 4000 1500 5000 1000 2000 500 0 0 0 46000 48000 50000 52000 54000 48000 50000 52000 54000 56000 46000 48000 50000 52000 54000 12000 10000 10000 B1800-21 B1823-13 B1930+22 8000 8000 8000 6000 6000 4000 4000 4000 2000 2000 0 0 0 46000 48000 50000 52000 54000 46000 48000 50000 52000 54000 44000 46000 48000 50000 52000 54000

ρ / ( 10 15 g / cm 3 ) 10 − 1 10 − 2 10 − 3 10 − 4 10 − 5 10 − 8 π 1600 1400 3 π 4 1200 1000 θ (rads) π 2 800 600 π 4 400 200 0 10 . 7 10 . 8 10 . 9 11 . 0 11 . 1 11 . 2 11 . 3 11 . 4 11 . 5 r (km)

r on line) Sequences of (solid) cooling curves for NSs of masses from 1 M to M (through 0 1 M ) with strong proton supe