Today. Announcements. Big Bang theory cont d Introduction to black holes

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1 Today Announcements HW #8 due Friday (tomorrow) 8am Test #2 average was 31/40 not as bad as it first appeared (several answer sheets were put in the wrong pile) Big Bang theory cont d Introduction to black holes ISP209s10 Lecture 21-1-

2 What is the Big Bang: Clicker question A) The nickname for nuclear explosions coined by einstein. B) A hypothesis about dinosaur extinction being caused by a violent burst of neutrinos from outer space C) The event some 14 billion years ago that was the beginning of the universe D) The event roughly 14 billion years from now that will mark The end of the universe ISP209s10 Lecture 21-2-

3 What is the Big Bang: Clicker question A) The nickname for nuclear explosions coined by einstein. B) A hypothesis about dinosaur extinction being caused by a violent burst of neutrinos from outer space C) The event some 14 billion years ago that was the beginning of the universe D) The event roughly 14 billion years from now that will mark The end of the universe ISP209s10 Lecture 21-3-

4 Clicker question What is the main evidence for the Big Bang theory: A) The cosmic microwave background radiation B) The abundance of hydrogen and helium in the universe C) The expansion of the universe D) All of the above E) None of the above ISP209s10 Lecture 21-4-

5 Clicker question What is the main evidence for the Big Bang theory: A) The cosmic microwave background radiation B) The abundance of hydrogen and helium in the universe C) The expansion of the universe D) All of the above E) None of the above ISP209s10 Lecture 21-5-

6 Clicker question How was the crucial evidence for the big bang theory -- the cosmic microwave background radiation -- discovered? A) By looking at black body radiation coming from distant stars B) By using parallax methods to measure large distances C) By way of an experiment designed by Penzias and Wilson to find the cosmic microwave background using special antennas D) Penzias and Wilson looked for the telltale neutrino signals in A special laboratory constructed far underground E) None of the above ISP209s10 Lecture 21-6-

7 Clicker question How was the crucial evidence for the big bang theory -- the cosmic microwave background radiation -- discovered? A) By looking at black body radiation coming from distant stars B) By using parallax methods to measure large distances C) By way of an experiment designed by Penzias and Wilson to find Penzias the cosmic and Wilson microwave found background it by accident using when special they antennas Were trying to track down the source of an annoying D) Penzias Hissing and sound Wilson in the looked early for satellite-based the telltale neutrino telephone signals in A special Networks. laboratory constructed far underground E) None of the above ISP209s10 Lecture 21-7-

8 Clicker question The observed cosmic microwave backround radiation is uneven or splotchy in modern measurements, with some regions in space showing a higher or lower temperature than others. Why is this non-uniformity important? A) It is necessary for the Big Bang theory to be consistent with the fact that matter and energy in the universe is lumpy and occurs in clusters with large voids of empty space in between. B) It is important because is in contradiction to the fact that matter and energy is distributed smoothly and evenly throughout the Universe. ISP209s10 Lecture 21-8-

9 Clicker question The observed cosmic microwave backround radiation is uneven or splotchy in modern measurements, with some regions in space showing a higher or lower temperature than others. Why is this non-uniformity important? A) It is necessary for the Big Bang theory to be consistent with the fact that matter and energy in the universe is lumpy and occurs in clusters with large voids of empty space in between. The regions of slightly higher temperature microwaves correspond to regions that eventually became galaxies etc. as the universe expanded. Conversely, the areas of cooler temperature correspond to regions That became large voids of empty ISP209s10 space Lecture as 21 the universe expanded. -9-

10 Hubble s Law - The universe is expanding! The further away an object is, the faster it is receding. Speed = H 0 x d The Hubble Constant: H 0 = 77 km/s/mpc ISP209s10 Lecture

11 The expanding universe Subtle point: Space itself is expanding! It is misleading to think of galaxies speeding away thru already existing space. Raisin bread analogy raisins <==> galaxies expanding dough <==> expanding space ISP209s10 Lecture

12 Expansion => The age of the universe and evidence for big bang From Hubble s law, we can Calculate how far away galaxies Will be at future times. time We know if we go far enough Back in time, the balloon (I.e., space) is very tiny and all The bits of paper (I.e., galaxies) Are right on top of each other. The big bang! We can use Hubble s law to estimate how long ago this was (~ 14 Billion years!) ISP209s10 Lecture

13 The expanding universe Paste some bits of paper on the surface of a balloon. Then inflate the balloon Subtle point: Space itself is expanding! It is misleading to think of galaxies speeding away thru already existing space. Balloon analogy bits of paper <==> galaxies expanding balloon surface <==> expanding space ISP209s10 Lecture

14 The Universe The Universe is not uniform. The ~ 200 billion galaxies are clustered into large clumps with voids in between Why? Answer: It must have started that way and gravity is slowly pulling things together ISP209s10 Lecture

15 How Did the Universe Begin? It looks like the Universe started about 14 billion years ago and has been expanding (space stretching) ever since. The model of what happened is called the Big Bang. There is a lot we don t understand. What came before? What caused the big bang? Why is there more matter than anti-matter in the Universe? ISP209s10 Lecture

16 Evidence for the Big Bang The expansion of the universe: All galaxies appear to be moving away from us. The abundances of the lightest elements produced in the Big Bang: the universe is mostly hydrogen and helium. The cosmic microwave background radiation: It looks like we are in the middle of a microwave oven with a temperature of ~3 Kelvin. ISP209s10 Lecture

17 It looks like we are in the middle of an oven The spectrum is identical to that of a blackbody at 3 Kelvin! ISP209s10 Lecture

18 Picture of the Universe at 300,000 years old WMAP observatory ISP209s10 Lecture 21 The splotches confirm the Universe was non-uniform In the beginning The pattern indicates that the Universe is 13.7 billion years old. -18-

19 The History of the Universe What we see as we look away from the Earth We are effectively looking back in time. ISP209s10 Lecture

20 Big Bang Timeline (the early moments) Electro First nuclei formed Atoms formed ISP209s10 Lecture

21 At high temperature forces are unified Current theory says at very high temperature we don t see all the forces. We say they are unified. At the start of the Big Bang the 4 forces were unified. At the Universe cooled the forces became distinct this is called spontaneous symmetry breaking ISP209s10 Lecture

22 Inflation of the Universe Meters The existence of an unknown scalar field caused the rapid inflation of the Universe Years since the Big Bang Space stretched by times! ISP209s10 Lecture

23 Why does time always move in one direction? Inflation during the Big Bang resulted in a universe that had a very low entropy, much too low for its size. It was like the Universe started with all heads. Hence, everything in the universe moves toward reaching the correct amount of entropy. Time has a direction because going back in time would imply the entropy could be decreased. That is very improbable. The universe tends toward increasing entropy. Remember the question: What is time? ISP209s10 Lecture

24 What about the future? Until very recently (past 5 years) we thought it was possible that the Universe might end in a Big Crunch. This would be the case if the mass of the Universe were large enough to halt the expansion and bring everything back together. In this model the Universe could be a neverending cycle of Big Bangs and Big Crunches. The microwave background measured by WMAP points to an ever expanding Universe. ISP209s10 Lecture

25 Our Future (Details) 3E+9 years from now, our Galaxy will collide with the Andromeda Galaxy, either merging Into 1 Super-Galaxy or ripping both apart. In 5E+9 years our sun fries Earth when it turns into a Red Giant In 1E+12 years the stellar era ends (Stars run out of nuclear fuel). In 1E+100 years, only remnant of stars remaining are black holes Eventually, the black holes will evaporate due to quantum Effects. All that remains in the universe is electrons, neutrinos, Photons. ISP209s10 Lecture

26 Lead-in to black holes: Conservation of Energy In nature certain quantities are conserved. Energy is one of these quantities. Example: Ball on a hill A 1.00 kg ball is rolled toward a hill with an initial speed of 5.00 m/s. If the ball roles without friction, how high, h, will the ball go? KE 1 2 = mv 2 1 mv 2 = 2 mgh PE " h = = mgh v 2g ( 5 m / s) ISP209s10 Lecture What the &#@* does this boring problem have to do with black holes? 2 ; = g = ! 9.80 m s 2 m s 2 2 = 1.28 m

27 v Earth Escape Velocity Applying the law of conservation of energy one can show Mass, m The velocity to completely escape the gravity of a planet (or any stellar mass) is: KE( leaving) = PE( far away) 1 2 v mv = 2 = 2GM R GmM R planet planet planet planet The escape velocity for the Earth is about 11 km/s. ISP209s10 Lecture

28 Large Mass in a small region What is the escape velocity for an object with the mass of the Sun and a radius of 10 km? M sun =1.99E+30 kg G=6.67E-11 Nm 2 /kg 2 v = 2GM R = 2" 6.67E # 11" 1.99E = 5! 10 8 m s This is greater than the speed of light! Nothing can go faster Than the speed of light. What does this mean? ISP209s10 Lecture

29 Black Holes The concentrated mass stretches space. The hole in space is so deep that NOTHING, not even light can escape. ISP209s10 Lecture

30 Where do black holes come from? ISP209s10 Lecture

31 Black Holes Black holes act as a lens and we see light from stars behind. They don t necessarily look black. They range from 3 solar masses to more than a billion solar masses. Small ones are formed by the collapse of a large star Larger ones form at the center of galaxies We can tell they exist because of thing orbiting nothing, and the radiation given off as things fall into them. Black holes are not cosmic vacuum cleaners. If the Sun were a black hole (with the same mass) the Earth would still orbit it and not get sucked in. ISP209s10 Lecture

32 Parts of a black hole G = 6.673E-11 N m 2 / kg 2 c = 3.0E+8 m/s M = mass of the black hole ISP209s10 Lecture

33 Black hole radius example We normally refer to the size of a black hole by its Schwarzschild radii. This is the distance inside of which nothing can escape. What is the radius of a black hole with the mass of our Sun? M sun = 1.99E30 kg G = 6.67E-11 N*m 2 /kg 2 2GM 2! 6.67E " 11! 1.99E30 r = = = c ( 3.00E8) m ISP209s10 Lecture

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