When a star dies…. Introduction What are compact objects? –White dwarf, neutron stars & black holes Why study? –Because it’s fun! –Test of physics in.

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Presentation transcript:

When a star dies…

Introduction What are compact objects? –White dwarf, neutron stars & black holes Why study? –Because it’s fun! –Test of physics in extreme condition.

Why compact? It is all about balance! Degenerate pressure

How are they formed? End stage of stars Mass determines fate

Low mass stars Sun-like stars Massive stars Low mass stars Sun-like stars Massive stars Low mass stars Sun-like stars Massive stars It’s all about mass

Red Giants Sun-like stars

Planetary Nebula 1 light yr across UV from the white central dwarf Emission lines

M57 Blue SnowballCat’s Eye DumbbellHelix

White Dwarfs Snow White and the Seven Dwarfs

White Dwarfs =>  10 6 g/cm 3 Mass ~ M  (but <1.4) Radius ~ R 

White Dwarfs ~100,000K when born Blackbody UV Yes, it’s organic! -- Crystalline carbon, oxygen like diamond, but 3,000 times harder So? Type Ia supernova

Example: Sirius B Discovered in 1862 m v =8.3 Surface temperature 25,000K Separation: 20AU Orbital period: 50 yrs

Sirius B

Death of Massive Stars

Supernova (Type II) E tot ~10 53 ergs (99% neutrinos) E kin ~ ergs E visible ~10 49 ergs Ni-56, Co-56 Outshine the host galaxy! Core  NS/BH Not type I!

Example: SN 1987a movie

Movies x3

Neutron Stars Predicted by Baade & Zwicky (1934) Densest object that has surface M ~ 1.4 M  ; R~10 km Giant nucleus A=10 57 Degenerate neutron pressure Strong magnetic field ~ gauss (H: 160eV) Strong surface gravity ~ g Surface temperature ~ 10 6 K

How Compact? Or 466,000 x

How Compact? M ~ 1.4 M  ; R~10 km =>  g/cm 3 Similar to nucleus: g/(10 13 cm) 3 World Population: ~10 9

Mass-radius Relation

Structure Atmosphere: ~cm Crust: Fe Neutron drip: 4x10 11 g/cm 3 Superfluidity Nuclear density: 2.8x10 14 g/cm 3 Core: quark matter?

Pulsar LGM: Jocelyn Bell (1967) Period 1.6 ms to 8s Are pulsars neutron stars? –Timescale (< 500km) –Good clocks

Blackbody + Power-law Where’s the energy from? Rotating magnet Polar cap Outer gap Emission

Example: Crab Pulsar SN1054 –guest star P=33ms Jet+torus (movies)

Research Topics Quark matter? Cooling Atmosphere Gamma-ray emission Magnetars: gauss AXP VHE (>100Gev) from SNR

URCA Process Cooling

Quark Stars? Stable quark matter (Witten 1984) 3C 58 ? RXJ ?

GRB Energy scale: keV – MeV Total energy: ~10 54 erg Timescale: ms – ks

Social Behavior Double NS/ Pulsar Millisecond (recycled) pulsars HMXBs LMXBs QPO

Double NS Double NS: PSR B –Test of GR (93’ Nobel) Double pulsars: PSR J –GR, magnetosphere –movie

QPO Quasi-periodic oscillations

Reference Shapiro & Teukolsky --Black holes, White dwarfs and Neutron Stars – the Physics of Compact Objects

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