Effective Quantum Gravity and Inflation
... Effective Quantum Gravity and Inflation Iberê Kuntz Theoretical Particle Physics department University of Sussex United Kingdom ...
... Effective Quantum Gravity and Inflation Iberê Kuntz Theoretical Particle Physics department University of Sussex United Kingdom ...
here
... (b) The nucleus begins to glow. (c) An electron changes its orbital energy. (d) The photon becomes trapped, orbiting in the atom. Cont. ...
... (b) The nucleus begins to glow. (c) An electron changes its orbital energy. (d) The photon becomes trapped, orbiting in the atom. Cont. ...
The Life of the Universe - University of Minnesota
... nucleus would become the size of our solar system • Creates density enhancements that give rise to the structure we observe today ...
... nucleus would become the size of our solar system • Creates density enhancements that give rise to the structure we observe today ...
Solutions to HW 1-2
... parameters. Inflation solves this problem because during the rapid exponential expansion, any initial curvature of the Universe would be stretched to near flatness. Horizon problem: the CMB is strikingly uniform in every direction we look in the sky. Opposite directions of the sky are too far away t ...
... parameters. Inflation solves this problem because during the rapid exponential expansion, any initial curvature of the Universe would be stretched to near flatness. Horizon problem: the CMB is strikingly uniform in every direction we look in the sky. Opposite directions of the sky are too far away t ...
God and Cosmology - Evidence for Christianity
... Comment by Paul Steinhardt and Neil Turok: “For all its strengths, the inflationary model rests on a significant number of unproven assumptions. The first, that the Big Bang was the beginning of time, immediately forces a second. To explain how the universe became so smooth and flat within the first ...
... Comment by Paul Steinhardt and Neil Turok: “For all its strengths, the inflationary model rests on a significant number of unproven assumptions. The first, that the Big Bang was the beginning of time, immediately forces a second. To explain how the universe became so smooth and flat within the first ...
ASTR100 Class 01 - University of Maryland Department of
... 3. Why is the density of the universe so close to the critical density? That is, why does the universe have such a flat geometry? An early episode of rapid inflation can solve all three mysteries! ...
... 3. Why is the density of the universe so close to the critical density? That is, why does the universe have such a flat geometry? An early episode of rapid inflation can solve all three mysteries! ...
AY5 Homework for Quiz 4: Spring 2015
... Quantum fluctuations in the pre-‐inflation universe were amplified to macroscopic scales 4) Horizon problem. The uniformity of the cosmic microwave background is very high despite the fact that parts of the ...
... Quantum fluctuations in the pre-‐inflation universe were amplified to macroscopic scales 4) Horizon problem. The uniformity of the cosmic microwave background is very high despite the fact that parts of the ...
Going to the End of the Earth to Learn About the Beginning of the
... ever taken Over 10,000 galaxies in this image! ...
... ever taken Over 10,000 galaxies in this image! ...
Inflation and the cosmological constant problem
... whether God could have created the world differently. A. Einstein The uniqueness problem Elementary particle theories turn out to present many different, yet equivalent solutions. So why looks low energy physics around as the way it does and not completely different? Why is space−time four−dime ...
... whether God could have created the world differently. A. Einstein The uniqueness problem Elementary particle theories turn out to present many different, yet equivalent solutions. So why looks low energy physics around as the way it does and not completely different? Why is space−time four−dime ...
File - AMS02 BOLOGNA
... The exponential de Sitter-like expansion that occurred during inflation ceases and the potential energy of the inflaton, the inflation field, decays into a hot, relativistic plasma of particles. The universe is dominated by radiation; quarks, electrons and neutrinos form. ...
... The exponential de Sitter-like expansion that occurred during inflation ceases and the potential energy of the inflaton, the inflation field, decays into a hot, relativistic plasma of particles. The universe is dominated by radiation; quarks, electrons and neutrinos form. ...
inflation
... 23, 347] to solve some problems of this theory (and of Particle Physics): • flatness problem – if today the Universe is close to flat, it should have been much more close in the past (Ω = 1 is an unstable critical point) inflation forces Ω to 1 in the beginning • horizon problem – CMBR photons emi ...
... 23, 347] to solve some problems of this theory (and of Particle Physics): • flatness problem – if today the Universe is close to flat, it should have been much more close in the past (Ω = 1 is an unstable critical point) inflation forces Ω to 1 in the beginning • horizon problem – CMBR photons emi ...
Exploring the Early Universe - Solar Physics and Space Weather
... Inflation Theory: the flatness problem •In order for space to be flat as it is today, the mass density must have been exactly equal to critical density right after the Big Bang •If mass density were slightly smaller than the critical density, the universe would have expanded so rapidly that matter ...
... Inflation Theory: the flatness problem •In order for space to be flat as it is today, the mass density must have been exactly equal to critical density right after the Big Bang •If mass density were slightly smaller than the critical density, the universe would have expanded so rapidly that matter ...
Early Universe : 2015 Open Note Test
... 45 g∗ T . Consider the case of (spin 2) gravitons, which decouple at T ≈ 10 GeV. Assume a hot bing bang model without inflation, so that at T > 1019 GeV the gravitons and other particles were in thermal equilibrium. (a) Describe in your own words what it means for a particle to decouple, and qualita ...
... 45 g∗ T . Consider the case of (spin 2) gravitons, which decouple at T ≈ 10 GeV. Assume a hot bing bang model without inflation, so that at T > 1019 GeV the gravitons and other particles were in thermal equilibrium. (a) Describe in your own words what it means for a particle to decouple, and qualita ...
85 nucleosynthesis26 - Boston University Physics
... between 1 and 3 minutes, temperature high enough to fuse n + p → d, then d + t → He t=tritium=3H not too high to dissociate weakly-bound d 2.2 MeV binding energy nor to destroy very stable 4He (=α) 24 MeV binding energy at t = 1 min, Big Bang predicts protons:neutrons = 7:1 after 3 minutes, universe ...
... between 1 and 3 minutes, temperature high enough to fuse n + p → d, then d + t → He t=tritium=3H not too high to dissociate weakly-bound d 2.2 MeV binding energy nor to destroy very stable 4He (=α) 24 MeV binding energy at t = 1 min, Big Bang predicts protons:neutrons = 7:1 after 3 minutes, universe ...
Our Incredible Universe
... forces that created the universe. These forces actually created space and time along with all that we see around us today. During a tiny fraction of the first second, the universe went through a short period of rapidly accelerating faster-than-light expansion called “inflation.” This initial expansi ...
... forces that created the universe. These forces actually created space and time along with all that we see around us today. During a tiny fraction of the first second, the universe went through a short period of rapidly accelerating faster-than-light expansion called “inflation.” This initial expansi ...
Age, Evolution, and Size of the Cosmos
... traditional answer: there was no time speculative ideas: Big Bounce • Big Bang is one of the greatest challenges in physics ...
... traditional answer: there was no time speculative ideas: Big Bounce • Big Bang is one of the greatest challenges in physics ...
LAST YEAR`S EXAM
... Describe two of the main problems with Big Bang cosmology that are solved by cosmological inflation. Describe the concept of inflation and how it solves these two problems. (5 marks) Assuming that the field or particle which gives rise to inflation can be expressed mathematically as an effective cos ...
... Describe two of the main problems with Big Bang cosmology that are solved by cosmological inflation. Describe the concept of inflation and how it solves these two problems. (5 marks) Assuming that the field or particle which gives rise to inflation can be expressed mathematically as an effective cos ...
origins powerpoint
... • Remember Einstein’s famous equation? • E=MC2 • Energy (E) can be converted into matter (M) • All of the matter in the universe now was once a tremendous amount of energy! ...
... • Remember Einstein’s famous equation? • E=MC2 • Energy (E) can be converted into matter (M) • All of the matter in the universe now was once a tremendous amount of energy! ...
Institute`s Colloquium, by invitation - ICE-CSIC
... On the BGV Theorem: Introduction • Inflationary cosmological models are generically eternal in their future evolution [1981-83: Guth, Linde, Albrecht, Steinhardt, Vilenkin] • In inflation one cannot in principle conclude for any future time that the whole Universe will reach thermal equilibrium • ...
... On the BGV Theorem: Introduction • Inflationary cosmological models are generically eternal in their future evolution [1981-83: Guth, Linde, Albrecht, Steinhardt, Vilenkin] • In inflation one cannot in principle conclude for any future time that the whole Universe will reach thermal equilibrium • ...
The Universe had (probably) an origin: on the theorem of Borde
... On the BGV Theorem: Introduction • Inflationary cosmological models are generically eternal in their future evolution [1981-83: Guth, Linde, Albrecht, Steinhardt, Vilenkin] • In inflation one cannot in principle conclude for any future time that the whole Universe will reach thermal equilibrium • ...
... On the BGV Theorem: Introduction • Inflationary cosmological models are generically eternal in their future evolution [1981-83: Guth, Linde, Albrecht, Steinhardt, Vilenkin] • In inflation one cannot in principle conclude for any future time that the whole Universe will reach thermal equilibrium • ...
Inflation (cosmology)
In physical cosmology, cosmic inflation, cosmological inflation, or just inflation is the exponential expansion of space in the early universe. The inflationary epoch lasted from 10−36 seconds after the Big Bang to sometime between 10−33 and 10−32 seconds. Following the inflationary period, the Universe continues to expand, but at a less rapid rate.The inflationary hypothesis was developed in the early 1980s. It explains the origin of the large-scale structure of the cosmos. Quantum fluctuations in the microscopic inflationary region, magnified to cosmic size, become the seeds for the growth of structure in the Universe (see galaxy formation and evolution and structure formation). Many physicists also believe that inflation explains why the Universe appears to be the same in all directions (isotropic), why the cosmic microwave background radiation is distributed evenly, why the Universe is flat, and why no magnetic monopoles have been observed.While the detailed particle physics mechanism responsible for inflation is not known, the basic picture makes a number of predictions that have been confirmed by observation. The hypothetical field thought to be responsible for inflation is called the inflaton.In 2002, three of the original architects of the theory were recognized for their major contributions; physicists Alan Guth of M.I.T., Andrei Linde of Stanford and Paul Steinhardt of Princeton shared the prestigious Dirac Prize ""for development of the concept of inflation in cosmology"".
