1 / 12

Physics 133: Extragalactic Astronomy ad Cosmology

Physics 133: Extragalactic Astronomy ad Cosmology. Lecture 5; January 22 2014. Previously. The universe is a 4 dimensional manifold as in General Relativity The universe is homogeneous and isotropic This implies that space and time can be “ separated ” so that we can define a cosmic time t

pryor
Download Presentation

Physics 133: Extragalactic Astronomy ad Cosmology

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. Physics 133: Extragalactic Astronomy ad Cosmology Lecture 5; January 22 2014

  2. Previously • The universe is a 4 dimensional manifold as in General Relativity • The universe is homogeneous and isotropic • This implies that space and time can be “separated” so that we can define a cosmic time t • There are only three possible geometries for the universe. Their metric is the Robertson-Walker metric • In the RW non-static universe redshift is a measure of distance. • The dynamics of the Universe is described by Friedmann Equation; Newtonian analog.

  3. Outline: Dynamics of the Universe: • Friedmann Equation • Fluid Equation • Acceleration Equation • Equation of State • Cosmological Constant

  4. Dynamics of the Universe. Friedmann Equation • Limitations of Newtonian analog: • Newtonian • What’s outside the sphere? • Inhomogeneous. Isotropic • Friedmann Equation (1922) is the correct form with energy instead of mass and curvature instead of internal energy [Blackboard] 1888 - 1925

  5. Dynamics of the Universe. “Fluid” equation • We have 1 equation and two functions a(t) and ε(t) • What is the connection between the two? • Adiabatic expansion • [Black board]

  6. Dynamics of the Universe. Acceleration equation • Another convenient form (not independent) is the equation of motion with the second derivative • [Black board] • Examples of Equation of state [blackboard]

  7. Fate of the universe in curvature + mass models

  8. The cosmological constant • Soon after the completion of general relativity (1916) people used it to describe the universe. • However, with only matter there was no way to obtain a static solution, which at that time was the prejudice. • Einstein added the cosmological constant to his equations to find a static solution… • [Blackboard]

  9. The cosmological constant • Unfortunately the static solution is unstable • And, when Hubble announced his discovery of the expansion, unnecessary • So the cosmological constant remained on the outskirts of cosmology for a long time… • Now it’s back!

  10. Cosmological constant or dark energy? • Nowadays people prefer to talk in terms of dark energy, instead of cosmological constant. • The classic cosmological constant is a modification of Einstein’s equation [Black board] • Dark energy is interpreted as something with negative pressure filling space • Is it some sort of vacuum energy? • We really don’t know…

  11. Dynamics of the Universe. Summary • Friedmann Equation describes the evolution of a(t) depending on content and geometry of the universe. • Fluid equations describe the evolution of the content of the universe with a(t). • The cosmological constant or dark energy is an extra term in Friedmann Equation and can induce acceleration. Currently supported by observations.

  12. The End See you on monday!

More Related