chapter23 - Empyrean Quest Publishers
... Background radiation from Big Bang has been freely streaming across universe since atoms formed at temperature ~ 3,000 K: visible/IR. Electron + proton = Hydrogen plus light (UV) ...
... Background radiation from Big Bang has been freely streaming across universe since atoms formed at temperature ~ 3,000 K: visible/IR. Electron + proton = Hydrogen plus light (UV) ...
Big Bang
... evidence for the Hot Big Bang. 1) Dark night sky → Finite age for universe. 2) Redshift proportional to distance → Homogeneous & isotropic expansion. 3) Cosmic Microwave Background → Universe was hot & dense enough to be opaque. ...
... evidence for the Hot Big Bang. 1) Dark night sky → Finite age for universe. 2) Redshift proportional to distance → Homogeneous & isotropic expansion. 3) Cosmic Microwave Background → Universe was hot & dense enough to be opaque. ...
Age, Evolution, and Size of the Cosmos
... • The radius visible U. is 14 x 109 pc or 46 x 109 light years ...
... • The radius visible U. is 14 x 109 pc or 46 x 109 light years ...
Key Areas covered
... It caused our universe to expand suddenly from the singularity bringing time and space into existence. Following the Big Bang, temperatures rapidly cooled and tiny particles of matter began to form. The first atoms to form were hydrogen and helium. This matter created stars, galaxies and planets. ...
... It caused our universe to expand suddenly from the singularity bringing time and space into existence. Following the Big Bang, temperatures rapidly cooled and tiny particles of matter began to form. The first atoms to form were hydrogen and helium. This matter created stars, galaxies and planets. ...
Key Areas covered
... Light and temperature • We can see that the temperature of an object affects the light it gives off. • This means that the temperature of an object is linked to both the frequency and wavelength of the light it emits. • A graph of intensity versus wavelength has a characteristic shape and can be sh ...
... Light and temperature • We can see that the temperature of an object affects the light it gives off. • This means that the temperature of an object is linked to both the frequency and wavelength of the light it emits. • A graph of intensity versus wavelength has a characteristic shape and can be sh ...
SCE 18 – Part 10
... • The temperature continued to fall (as expansion continued) but at a lower rate. • Electrons and nuclei are still NOT united as atoms. • But after about 379,000 years, the temperature became sufficiently low that protons, neutrons and electrons could combine to form atoms. ...
... • The temperature continued to fall (as expansion continued) but at a lower rate. • Electrons and nuclei are still NOT united as atoms. • But after about 379,000 years, the temperature became sufficiently low that protons, neutrons and electrons could combine to form atoms. ...
Planck Era
... The cosmic microwave background – the radiation left over from the Big Bang – was detected by Penzias & Wilson in 1965 (they won the Nobel prize in 1978 for this discovery) ...
... The cosmic microwave background – the radiation left over from the Big Bang – was detected by Penzias & Wilson in 1965 (they won the Nobel prize in 1978 for this discovery) ...
The Assembly of M31`s Halo from Dwarf Galaxy Building Blocks
... Einstein showed that the particle nature of electromagnetic radiation can explain the photoelectric effect and was awarded the Nobel Prize for this ...
... Einstein showed that the particle nature of electromagnetic radiation can explain the photoelectric effect and was awarded the Nobel Prize for this ...
The Merger of Two Disk Galaxies
... interstellar cloud of gas and dust. Most of the material becomes part of the young Sun, but some debris forms a disk. Within this disk form the planets, moons, comets, asteroids, and meteoroids. Note that this process is repeated on a smaller scale in the ...
... interstellar cloud of gas and dust. Most of the material becomes part of the young Sun, but some debris forms a disk. Within this disk form the planets, moons, comets, asteroids, and meteoroids. Note that this process is repeated on a smaller scale in the ...
origins powerpoint
... entirely of energy, and was very small • Something happened to cause the energy to expand – the “big bang” • As the energy expanded in all directions, it began to cool and condense into the simplest forms of ...
... entirely of energy, and was very small • Something happened to cause the energy to expand – the “big bang” • As the energy expanded in all directions, it began to cool and condense into the simplest forms of ...
presentation02 - School of Physical Sciences
... Origin of the Universe Scientists believe that the universe began in a tremendous release of energy known as the Big Bang. The universe has been expanding ever since. Evidence for this: •Observation of galaxies flying away from us in all directions. •Remnant of the Big Bang known as the Cosmic Micr ...
... Origin of the Universe Scientists believe that the universe began in a tremendous release of energy known as the Big Bang. The universe has been expanding ever since. Evidence for this: •Observation of galaxies flying away from us in all directions. •Remnant of the Big Bang known as the Cosmic Micr ...
Document
... Large Structure Cosmology Answered lots of questions (hopefully) Raised lots of questions (hopefully) ...
... Large Structure Cosmology Answered lots of questions (hopefully) Raised lots of questions (hopefully) ...
Galaxy Zoo: Pre and post‐workshop information
... Pre‐Workshop Information for Teachers In 1923 Edwin Hubble looked at galaxies (which he thought were nebulae or clouds of bright gas) through a 100” reflector (telescope with a mirror) on Mt Wilson in the US. He took a photo of Andromeda (which can be seen on a clear night with the naked eye). Hubb ...
... Pre‐Workshop Information for Teachers In 1923 Edwin Hubble looked at galaxies (which he thought were nebulae or clouds of bright gas) through a 100” reflector (telescope with a mirror) on Mt Wilson in the US. He took a photo of Andromeda (which can be seen on a clear night with the naked eye). Hubb ...
Video Worksheet Beyond the Big Bang (Part 2 of 2)
... 5. The theory of the universe's origin was first proposed by scientist Georges Lemaitra, a Roman Catholic Priest, and his theory was embraced by the _______________ who interpreted the theory as de facto proof of Genesis. ...
... 5. The theory of the universe's origin was first proposed by scientist Georges Lemaitra, a Roman Catholic Priest, and his theory was embraced by the _______________ who interpreted the theory as de facto proof of Genesis. ...
Intro to Cosmology!
... Quantum Field Theory: Rather than talking about quantum properties of particles, talk about quantum properties of Space-Time. Superpartners exist in separate quantum Space-Time coordinates called “Superspace.” The existence of a superspace simplifies QFT significantly. General Relativity can be deri ...
... Quantum Field Theory: Rather than talking about quantum properties of particles, talk about quantum properties of Space-Time. Superpartners exist in separate quantum Space-Time coordinates called “Superspace.” The existence of a superspace simplifies QFT significantly. General Relativity can be deri ...
Stars, Galaxies, and the Universe
... • A white dwarf is is a star that has used up all of its hydrogen and is the leftover center of an older star. • Class F stars are yellow-white • The majority of stars in our galaxy are main sequence stars. ...
... • A white dwarf is is a star that has used up all of its hydrogen and is the leftover center of an older star. • Class F stars are yellow-white • The majority of stars in our galaxy are main sequence stars. ...
Lecture120202 - FSU High Energy Physics
... time = 10-35 to 10-33 seconds size went from 10-12 the size of a nucleus to 3 meters VERY rapid expansion ...
... time = 10-35 to 10-33 seconds size went from 10-12 the size of a nucleus to 3 meters VERY rapid expansion ...
The Evolution of the Universe: from Cosmic Soup to Earth
... Big Bang: The initial point from which the universe began developing approximately 13.7 billion years ago. Cosmic Microwave Background: the leftover energy that can be detected from the initial Big Bang. Element: a pure chemical substance which is determined by the number of protons in its nu ...
... Big Bang: The initial point from which the universe began developing approximately 13.7 billion years ago. Cosmic Microwave Background: the leftover energy that can be detected from the initial Big Bang. Element: a pure chemical substance which is determined by the number of protons in its nu ...
The Prelude - Solar Physics and Space Weather
... •At about t = 1 second, temperature fell below 6 X 109 K, electrons and positions annihilated to form low energy gammaray photons that can not reverse the process •As a result, matter and anti-matter content decreased, and radiation content increased •From 1 second to 380,000 years, the universe is ...
... •At about t = 1 second, temperature fell below 6 X 109 K, electrons and positions annihilated to form low energy gammaray photons that can not reverse the process •As a result, matter and anti-matter content decreased, and radiation content increased •From 1 second to 380,000 years, the universe is ...
Cosmic microwave background
The cosmic microwave background (CMB) is the thermal radiation left over from the time of recombination in Big Bang cosmology. In older literature, the CMB is also variously known as cosmic microwave background radiation (CMBR) or ""relic radiation."" The CMB is a cosmic background radiation that is fundamental to observational cosmology because it is the oldest light in the universe, dating to the epoch of recombination. With a traditional optical telescope, the space between stars and galaxies (the background) is completely dark. However, a sufficiently sensitive radio telescope shows a faint background glow, almost exactly the same in all directions, that is not associated with any star, galaxy, or other object. This glow is strongest in the microwave region of the radio spectrum. The accidental discovery of CMB in 1964 by American radio astronomers Arno Penzias and Robert Wilson was the culmination of work initiated in the 1940s, and earned the discoverers the 1978 Nobel Prize.The CMB is a snapshot of the oldest light in our Universe, imprinted on the sky when the Universe was just 380,000 years old. It shows tiny temperature fluctuations that correspond to regions of slightly different densities, representing the seeds of all future structure: the stars and galaxies of today.The CMB is well explained as radiation left over from an early stage in the development of the universe, and its discovery is considered a landmark test of the Big Bang model of the universe. When the universe was young, before the formation of stars and planets, it was denser, much hotter, and filled with a uniform glow from a white-hot fog of hydrogen plasma. As the universe expanded, both the plasma and the radiation filling it grew cooler. When the universe cooled enough, protons and electrons combined to form neutral atoms. These atoms could no longer absorb the thermal radiation, and so the universe became transparent instead of being an opaque fog. Cosmologists refer to the time period when neutral atoms first formed as the recombination epoch, and the event shortly afterwards when photons started to travel freely through space rather than constantly being scattered by electrons and protons in plasma is referred to as photon decoupling. The photons that existed at the time of photon decoupling have been propagating ever since, though growing fainter and less energetic, since the expansion of space causes their wavelength to increase over time (and wavelength is inversely proportional to energy according to Planck's relation). This is the source of the alternative term relic radiation. The surface of last scattering refers to the set of points in space at the right distance from us so that we are now receiving photons originally emitted from those points at the time of photon decoupling.Precise measurements of the CMB are critical to cosmology, since any proposed model of the universe must explain this radiation. The CMB has a thermal black body spectrum at a temperature of 7000272548000000000♠2.72548±0.00057 K. The spectral radiance dEν/dν peaks at 160.2 GHz, in the microwave range of frequencies. (Alternatively if spectral radiance is defined as dEλ/dλ then the peak wavelength is 1.063 mm.) The glow is very nearly uniform in all directions, but the tiny residual variations show a very specific pattern, the same as that expected of a fairly uniformly distributed hot gas that has expanded to the current size of the universe. In particular, the spectral radiance at different angles of observation in the sky contains small anisotropies, or irregularities, which vary with the size of the region examined. They have been measured in detail, and match what would be expected if small thermal variations, generated by quantum fluctuations of matter in a very tiny space, had expanded to the size of the observable universe we see today. This is a very active field of study, with scientists seeking both better data (for example, the Planck spacecraft) and better interpretations of the initial conditions of expansion. Although many different processes might produce the general form of a black body spectrum, no model other than the Big Bang has yet explained the fluctuations. As a result, most cosmologists consider the Big Bang model of the universe to be the best explanation for the CMB.The high degree of uniformity throughout the observable universe and its faint but measured anisotropy lend strong support for the Big Bang model in general and the ΛCDM (""Lambda Cold Dark Matter"") model in particular. Moreover, the fluctuations are coherent on angular scales that are larger than the apparent cosmological horizon at recombination. Either such coherence is acausally fine-tuned, or cosmic inflation occurred.