Evolution of High Mass stars

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2 Evolution of High Mass stars

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4 Neutron Stars A supernova explosion of a M > 8 M Sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M Sun. Pressure becomes so high that electrons and protons combine to form stable neutrons throughout the object. Typical size: R ~ 10 km Mass: M ~ 1.4 to 3 M Sun Density: ~ g/cm 3 A piece of neutron star matter of the size of a sugar cube has a mass of ~100 million tons!!!

5 Neutron Stars Hot Spin Rapidly Super High Density Strong Magnetic Field A neutron star the size of a sugar cube would weigh 100 million tons on Earth!

6 Neutron Star RCW 103 2,000 year-old-remnant 10,000 light years from Earth Image Credit: Chandra Neutron star near center rotates once every 6.7 hours

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10 Discovery of Pulsars Angular momentum conservation => Collapsing stellar core spins up to periods of ~ a few milliseconds. Magnetic fields are amplified up to B ~ G. (up to times the average magnetic field of the Sun) => Rapidly pulsed (optical and radio) emission from some objects interpreted as spin period of neutron stars

11 The Crab Pulsar Remnant of a supernova observed in A.D. 1054

12 Light Curves of the Crab Pulsar

13 The Lighthouse Model of Pulsars A pulsar s magnetic field has a dipole structure, just like Earth s. Radiation is emitted mostly along the magnetic poles.

14 Images of Pulsars and other Neutron Stars

15 The Effects of Pulsar Winds Pulsars blow off a constant stream (wind) of high-energy particles: Pulsar Winds

16 Proper Motion of Neutron Stars Some neutron stars are moving rapidly through interstellar space. This might be a result of anisotropies during the supernova explosion, forming the neutron star.

17 Compact Objects with Accretion Disks Black holes and neutron stars can be part of a binary system. Matter gets pulled off from the companion star, forming an accretion disk, => Strong x-ray source! and heats up to a few million K.

18 Neutron Stars in Binary Systems: X-ray binaries Example: Her X-1 2 M Sun (F-type) star star eclipses neutron star and accretion disk periodically Orbital period = 1.7 days Accretion disk material heats to several million K => X-ray emission

19 Black Holes Just like white dwarfs (Chandrasekhar limit: 1.4 M Sun ), there is a mass limit for neutron stars: Neutron stars can not exist with masses > 3 M Sun We know of no mechanism to halt the collapse of a compact object with > 3 M Sun. It will collapse into a single point a singularity: => A black hole!

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22 Escape Velocity Velocity needed to escape Earth s gravity from the surface: v esc v esc 11.6 km/s Now, gravitational force decreases with distance (~1/d 2 ) => starting out high above the surface => lower escape velocity v esc If you could compress Earth to a smaller radius => higher escape velocity from the surface v esc

23 The Schwarzschild Radius => There is a limiting radius where the escape velocity reaches the speed of light, c: R s = 2GM c 2 V esc = c G = Universal constant of gravity M = Mass R s is called the Schwarzschild radius.

24 Schwarzschild Radius and Event Horizon No object can travel faster than the speed of light. => Nothing (not even light) can escape from inside the Schwarzschild radius. We have no way of finding out what s happening inside the Schwarzschild radius. Event horizon

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26 The Gravitational Field of a Black Hole Gravitational Potential Distance from central mass The gravitational potential (and gravitational attraction force) at the Schwarzschild radius of a black hole becomes infinite. However, at large distances, it is not different from the gravitational potential of a normal star. If you replaced the Sun with a black hole of the same mass, the orbits of the planets would not change!

27 General Relativity Effects Near Black Holes An astronaut descending down towards the event horizon of the black hole will be stretched vertically (tidal effects) and squeezed laterally.

28 General Relativity Effects Clocks starting at 12:00 at each pointafter 3 hours (for an observer far away from the black hole): Near Black Holes Time dilation Event horizon Clocks closer to the black hole run more slowly. Time dilation becomes infinite at the event horizon.

29 General Relativity Effects Near Black Holes Gravitational Red Shift All wavelengths of emissions from near the event horizon are stretched (red shifted). Frequencies are lowered Event horizon

30 Observing Black Holes No light can escape a black hole. => Black holes can not be observed directly. If an invisible compact object is part of a binary, we can estimate its mass from the orbital period and radial velocity. Mass > 3 M Sun => Black hole!

31 Evidence for a Black Hole: Masses of Compact Objects Compact object with > 3 M Sun must be a black hole!

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