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| Name | Big Bang Cosmology: the Origin and Fate of the Universe |
| Video Uploader | Video From Jason Kendall |
| Upload Date | This Video Uploaded At 26-08-2021 09:55:33 |
| Video Discription | This is the fourteenth and final lecture series of my complete online introductory undergraduate college course. This video series was used at William Paterson University and CUNY Hunter in online classes as well as to supplement in-person course material. Notes and links are present in the videos at the start of each lecture. 0:00:01 - Cosmic Homogeneity and Isotropy 0:32:18 - The Big Bang 1:23:44 - Why Does Cosmic Expansion Cause Redshift? 1:40:43 - The Cosmic Microwave Background. CP check. 27:38 – 28:24 2:41:44 - The First Three Minutes of the Universe 3:34:11 - Formation of Large-Scale Structure in the Universe 4:21:47 - Cosmic Inflation 5:28:37 - Dark Energy, Supernovae and the Ultimate Fate of the Universe The Universe on the largest scales is very self-similar. It looks about the same no matter which way you look, and it’s also made up of the same stuff pretty much everywhere. This leads us to the Cosmological Principle which codifies this isotropy and homogeneity, which asserts that the universe has the same physical laws everywhere. Next, we run the clock backwards in time, and we see how, using the fundamental principles of classical physics, especially thermodynamics, that the universe was smaller and hotter ago. We see exactly what we mean by the Big Bang, and what it covers and what it does not cover. The Standard Hot Big Bang basically is a story from only about the first few billionths of a second until today. It’s just amazing what exactly we can do with classical physics and elementary general relativity. Frequently, people don't understand why expansion means that light gets redshifted. Here I link the two ideas. What causes the redshift of light, how do represent it mathematically? What exactly gets stretched? Everything is a measurable, and redshift is one of those things. As part of this, we study the expansion in great detail, outlining the Robertson Walker Metric, a solution to the Einstein Field Equations of General Relativity. The discovery of the Cosmic Microwave Background is regarded as one of the most important of all science, as it is relic radiation from its early hot, dense epochs. We see that it was a key prediction of the Big Bang, which was discovered by accident by Penzias and Wilson. By studying the microwave sky in detail, the COBE, WMAP and Planck probes of NASA and ESA have shown us that the CMB is a perfect blackbody, at the temperature 2.7 Kelvin. When we study the tiny fluctuations and anisotropies away from this near-perfect spectrum, we find that we can learn what the universe was like when it was roughly 350,000 years old. We we watch atoms combine together for the first time, letting light slip free to come to us 13.6 billion years later. This observation alone is proof of the Big Bang. The story of the universe in its infancy is actually well-known from Classical Physics. We follow the classic book by the same name on a journey back to when the universe was 180 seconds old. We find nuclear fusion in the early cosmos. Even more convincing than the cosmic microwave background, the ratio of hydrogen to helium that was fixed in these early moments is greater proof of the Big Bang. This ratio is seen in the most ancient stars, who still carry the original composition of the birth of the universe. Large-scale structure formation in the universe is the final pillar in the Hot Big Bang Standard Model. We learn why galaxy clusters have so much hot gas, and how the absorption features in distant quasars came to be. We also see how the dark matter distribution can be mapped by its effect on galaxy's light and on the shape of clusters too. The Inflationary Epoch happened when the universe was extremely young. During the Grand Unified Theory (GUT) Era, the universe became the nearly flat, critical-density Cosmos we see today. In order to understand it, we use Quantum Gravity to approximate the wild phase transitions that must have occurred in order to force the expansion of space at speeds exponentially greater than light! Oddly enough, this epoch can be observed as effects of gravitational waves on CMB. The Inflationary Epoch solves a number of problems associated with the Standard Big Bang model and raises some wild questions about the nature of the origin of the cosmos. The discovery of Dark Energy in 1998 by two teams helped us learn what will happen at the end of the Universe. Their competing studies of deceleration parameter using Type Ia supernova discovered Dark Energy, the cosmic negative pressure that’s pushing the universe apart was confirmed by WMAP and Planck. It’s possible that dark energy may, in fact, be a Phantom Energy, which will cause a Big Rip as the universe accelerates exponentially in its expansion. There could also be a grand heat death of the cosmos where it just gets larger and darker and colder for all time. |
| Category | Science & Technology |
| Tags | Astronomy | Astrophysics | Physics | cosmology | Big Bang | cosmological principle | cosmic redshift | universe | cosmos | Einstein | Expanding universe | Cosmic Microwave Background | Blackbody | Planck | WMAP | COBE | last scattering surface | decoupling | Penzias and Wilson | recombination | Nucleosynthesis | Large-scale structure | Dark Matter | Lyman-alpha forest | CMB Anisotropies | Dark Energy | Inflation | Grand Unified Theory (GUT) | Quantum Gravity | False Vacuum | Quantum Foam | Type Ia supernova | The Big Rip |
