1 / 38

Black Holes

Black Holes. Underlying principles of General Relativity. The Equivalence Principle No difference between a steady acceleration and a gravitational field. Gravity and Acceleration cannot be distinguished. V = a h/c. h. Equivalence principle – this situation should be the same.

abena
Download Presentation

Black Holes

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Black Holes

  2. Underlying principles of General Relativity The Equivalence Principle No difference between a steady acceleration and a gravitational field

  3. Gravity and Acceleration cannot be distinguished

  4. V = a h/c h

  5. Equivalence principle – this situation should be the same Gravitational field h

  6. Eddington tests General Relativity and spacetime curvature GR predicts light-bending of order 1 arcsecond near the limb of the Sun Principe May 1919

  7. Lensing of distant galaxies by a foreground cluster

  8. QSO 2237+0305 The Einstein cross

  9. Curved Space: A 2-dimensional analogy Flat space Radius r Angles of a triangle add up to 180 degrees Circumference of a circle is 2πr

  10. Positive and Negative Curvature Triangle angles >180 degrees Circle circumference < 2πr Triangle angles <180 degrees Circle circumference > 2πr

  11. The effects of curvature only become noticeable on scales comparable to the radius of curvature. Locally, space is flat.

  12. A geodesic – the “shortest possible path”** a body can take between two points in spacetime (with no external forces). Particles with mass follow timelike geodesics. Light follows “null” geodesics. Time Timelike Curved geodesic caused by acceleration OR gravity Spacelike Matter tells space(time) how to curve Spacetime curvature tells matter how to move Space ** This is actually the path that takes the maximum “proper” time.

  13. Mass (and energy, pressure, momentum) tell spacetime how to curve; Curved spacetime tells matter how to move A formidable problem to solve, except in symmetric cases – “chicken and egg”

  14. Curvature of space in spherical symmetry – e.g. around the Sun

  15. V = (2ah)1/2 h Special Relativity A moving clock runs slow

  16. Observer ON TRAIN Observer BY TRACKSIDE Train speed v Width of carriage Is d meters s d vt/2 t’ = 2d / c t = 2s / c So t’ is smaller than t Observers don’t agree! Smaller by a factor g Where g2 = 1/(1 - v2/c2) Speed of light is c=300,000 km/s

  17. V = (2ah)1/2 h Special Relativity A moving ruler is shorter

  18. According to the equivalence principle, this is the same as Gravitational field h

  19. Curvature of space in spherical symmetry – e.g. around the Sun

  20. Spacetime curvature near a black hole

  21. A black hole forms when a mass is squashed inside it’s Schwarzschild Radius RS = 3 (M/Msun) km Time dilation factor 1/(1 – RS/r)1/2 Becomes infinite when r=RS

  22. Progenitor < 8 M Planetary Nebula Remnant < 1.4 M The Chandrasekhar limit A cooling C/O core, supported by quantum mechanics! Electron degeneracy pressure. Cools forever – gravity loses! White Dwarf

  23. Progenitor > 8 M Supernova Remnant < 2.5 M Remnant > 2.5 M 20 km Neutron star, supported by quantum mechanics! Neutron degeneracy pressure. Cools forever – gravity loses! Black Hole – gravity wins!

  24. Black Holes in binary systems

  25. Cygnus X-1 M3 sin3i = 0.25 (M + m)2 Period = 6 days M > 5 Msun

  26. Ellipsoidal light curve variations Depend on mass ratio and orbit inclination

  27. Combine ellipsoidal model with radial velocity curve BH mass Black hole mass 10 –15 x Msun

  28. Spinning black holes – the Kerr metric

  29. Spaghettification A 10g stretching force felt at 3700 km (>RS) from a 10 Msun black hole Force increases as 1/r3

  30. Supermassive Black Holes Jets propelled by twisted magnetic field lines attached to gas spiralling around a central black hole

  31. Supermassive Black Hole in the Galactic Centre Mass is 4 millions times that of the Sun Schwarzschild radius 12 million km = 0.08 au

  32. Falling into a black hole

More Related