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Phys 1830: Lecture 14

Phys 1830: Lecture 14

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Phys 1830: Lecture 14

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  1. Stephan’s Quintet Phys 1830: Lecture 14 J. English • Next Classes: • Image-making • Previous Classes: • Newtonian Gravity • tides • Interacting Galaxies • This Class: • Interacting Galaxies continued • Constant acceleration • Orbits and mass • Dark Matter • Einstein’s Gravity • Gravitational lensing. Take up tests at office hour Oct 21 or appointments at other times.

  2. Imaging Workshop coming up next Friday • Bring images you stretched OR from • http://www.physics.umanitoba.ca/~english/2013fallphys1830/bwimaging/ • I posted stretched images at website in case you didn’t stretch images. • work in teams again.

  3. Tidal Force Examples: Groups of Galaxies Image credit: J. English • Galaxies residing in groups also feel tidal forces.

  4. Tidal Force Examples: Groups of Galaxies – velocity fields J. English • 2 tidal arms in the upper galaxy – major merger. • One long arm to the left in the left galaxy – minor merger. • Cloud is likely to be tidal debris.

  5. Tidal Force Examples: Clusters of Galaxies • Groups which have hundreds to thousands of galaxies are called clusters. • Gravitas - http://www.galaxydynamics.org/ J. Dubinski

  6. Motion in a Gravitational Field Can we predict the velocity at which a planet orbits a star? Does a falling heavy object speed up compared to a falling light object? How do we know that there is Dark Matter?

  7. Combining Forces of Motion and Gravity: Constant Acceleration and • Force on an object due to orbital motion is equal to the force on object due to gravity. • mass of the smaller object cancels out.

  8. Combining Forces of Motion and Gravity: Constant Acceleration • Consider 2 objects of different mass feeling the pull of gravity from M. • mass of these objects doesn’t matter. • Start 2 objects at same distance from centre of gravity  acceleration on them is constant.

  9. What do you predict? • Drop a hammer and a feather at the same time. Ignoring friction, which statement would be true? • The hammer hits the ground before the feather. • Both hit the ground at the same time.

  10. Combining Motion and Gravity: Constant Acceleration • The moon’s atmosphere is insignificant (frictionless environment). • Can see that objects of different mass feel a constant acceleration in a gravitational field. The hammer and feather land at the same time.

  11. Motion of an Object: Gravity, Velocity and Mass • The relationship between acceleration and velocity for an orbit is • Also an expression for acceleration is generated by setting • Equating these 2 expressions for acceleration gives

  12. Mass in Galaxies: Rearranging the equation gives: • Any time that there is an object in orbit around another object, we can determine the mass of the central object! • e.g. the moon’s orbital velocity and distance from the Earth can be used to “weigh” the Earth.

  13. Plot Velocity Equation for planets the Solar System:  • The sun contains 99.85% of the mass in the solar system so we can ignore the contribution of the mass of the planets. i.e. M is constant. • Keperlian motion.

  14. Mass in Galaxies: The general shape of rotation curves is • the same as the velocity vs radius plot for the solar system. • is flat or rising which is the same as for Keplerian motion. • is flat or rising which is different than Keplerian motion.

  15. Mass in Galaxies: Rearranging the equation gives: • In a galaxy’s rotation curve, at a large radius the velocity remains constant (the plot is flat). • If radius increases, then the mass is increasing! • This is called the “dynamical mass”. • The dynamical mass consists of all matter – stars, gas, dust, etc.

  16. Galaxy rotation curves Mass increases out to the last measured radial point. Solid body rotation in centre but flat (i.e. constant velocity in outer regions.

  17. Mass in Galaxies: NGC 3556 R. Gendler HI velocity field of NGC 3556 • Sum up all the luminous radiation (x-ray gas, optically visible stars, infrared dust, cold HI in the radio). Convert this into the mass required to produce this amount of radiation.  the luminous mass. • Calculate the dynamical mass out to the furthest radius we can measure.

  18. Mass in Galaxies: NGC 3556 R. Gendler HI velocity field of NGC 3556 Dynamical mass is much greater than the luminous mass! • 90% of the mass in a galaxy is not luminous. This material is called Dark Matter. Since it extends beyond the disk, we say a galaxy has a dark matter halo. Discuss what this matter might be with your neighbours. We will talk more about this later in the term.

  19. 36. According to their rotation curves, most spiral galaxies a) rotate as a solid body only b) rotate counterclockwise c) have decreasing rotational speeds with increasing distance d) contain dark matter e) contain dark energy (Hint: Does “energy” have mass? What is dark energy?)

  20. Example of a question which tests concepts. It is possible to ``weigh'' a planet, for example, with the following information about: • the planet's flattened shape (oblateness) and reflectivity (albedo). • the moon's orbital speed and its rotational speed. • using only the distance between the planet and moon and the orbital speed of the moon. • none of the above because there is no known way to determine the mass of planets.

  21. Seeing Gravity: • These are remarkable images. • The arcs are not scratches on the film or bleeding in the CCD. • These are gravitational lenses. • Lenses are described by Einstein’s General Theory of Relativity.

  22. General Relativity (GR): • Motivation: • The speed of light is measured to remain constant regardless of the speed of the observer. • Newton’s laws are inaccurate for extraordinarily concentrated masses and large accelerations. • GR is a geometrical view  concept of gravitational field. • GR has 4 dimensions: 3 spatial dimensions and 1 time dimension  spacetime.

  23. General Relativity (GR): • Uses Einstein’s Field Equations. • Definition: The presence of mass curves spacetime and we interpret the curved motion (i.e. orbits) of particles in curved spacetime as acceleration due to a force, i.e. gravity. • In the case of small mass or small acceleration, Einstein’s Field Equations reduce to Newton’s laws of gravity and F = ma • Really is a “law” rather than a theory.

  24. We got to here. Although the rest will be reviewed in the next class, please read ahead.

  25. GR: Gravitational Lensing • A foreground object like a galaxy (or a cluster of galaxies) bends the fabric of spacetime. • Light must travel in spacetime so it bends around the curve. • Projecting back onto the celestial sphere we see more than one image of an unresolved background galaxy (e.g. quasar).

  26. GR: Gravitational Lensing • A background galaxy will be made into arcs by the foreground lensing galaxy or cluster of galaxies. • All of the matter in the foreground galaxy (luminous and dark) bends spacetime.

  27. Seeing Gravity: • The clusters are acting as lenses. • The arcs are background galaxies. • Using GR we can determine how much matter must be in the foreground cluster in order to create the arcs. • Measuring up all the luminous emission (x-ray through radio) gives the amount of mass due to processes that produce EM radiation. • The lensing mass is much greater than the luminous mass in the cluster  Dark Matter! • (Changes to Newton’s Laws won’t make DM go away)

  28. Seeing Gravity • A single galaxy lensing a background galaxy.

  29. Seeing Gravity General Relativity is applicable to everything from the precession of the planet Mercury to your cell phone. On the shuttle (in orbit therefore accelerating) the astronauts measure time, using atomic clocks, to be moving slower than the folk in mission control  spacetime! • A single galaxy lensing a background galaxy  Dark Matter.

  30. Fill in the Blank Question: The lensing of a distant quasar is produced by ________ of a foreground galaxy. A) all the normal matter and dark matter B) only the mass of the black hole in the centre of a galaxy C) an individual star D) a supernova’s intense magnetic field

  31. Requirements for the Workshop on Friday • All materials are at http://www.physics.umanitoba.ca/~english/2013fallphys1830/bwimaging/ • GNU Image Manipulation Package (GIMP). • You can use PhotoShop IF you are an expert and your version has “screen mode” in layers. • Run GIMP to set up your preferences before you get to class. • Black and White image jpegs – either your own or mine. • Workshop material will be on November test. • Let me know if you need a power socket for your laptop.