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]

51000 52000 53000 54000 2000 4000 6000 40000 44000 48000 52000 10000 20000 30000 47000 48000 49000 50000 51000 1000 2000 3000 4000 46000 48000 50000 52000 54000 2000 4000 6000 48000 50000 52000 54000 56000 5000 10000 46000 48000 50000 52000 54000 500 1000 1500 2000 2500 46000 48000 50000 52000 54000 4000 8000 12000 46000 48000 50000 52000 54000 2000 4000 6000 8000 10000 44000 46000 48000 50000 52000 54000 2000 4000 6000 8000 10000

J0537-6910 B1737-30 B0833-45 B1757-24 B1338-62 B1758-23 B1930+22 B1823-13 B1800-21

10.7 10.8 10.9 11.0 11.1 11.2 11.3 11.4 11.5 r (km)

π 4 π 2 3π 4

π θ (rads) 200 400 600 800 1000 1200 1400 1600 10−8 10−5 10−4 10−3 10−2 10−1 ρ/(1015g/cm3)

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