Dr.Sinha - Indico
... star with the realisation that changes in the internal structure as the star spins down, will be reflected in the moment of inertia and hence the deceleration. In this letter we are not considering the “recycling” scenario of binary system. During the spin down of a (say) millisecond neutron star, t ...
... star with the realisation that changes in the internal structure as the star spins down, will be reflected in the moment of inertia and hence the deceleration. In this letter we are not considering the “recycling” scenario of binary system. During the spin down of a (say) millisecond neutron star, t ...
File - Physical Science
... tremendous atomic collisions that alter the atomic structure and release an enormous amount of energy. This makes stars hot and bright. Nuclear fusion is an atomic reaction that fuels stars. In fusion, many nuclei (the centers of atoms) combine together to make a larger one (which is a different ele ...
... tremendous atomic collisions that alter the atomic structure and release an enormous amount of energy. This makes stars hot and bright. Nuclear fusion is an atomic reaction that fuels stars. In fusion, many nuclei (the centers of atoms) combine together to make a larger one (which is a different ele ...
13. Time and the past and future histories of the universe
... In the beginning there was nothing, and then the big bang – between 10-44 and 10-35 seconds the universe expands from a pinprick to larger than we can presently see (This is the INFLATION ERA.) Then there is energy and the expanding universe cools and matter and antimatter appear. A tiny imbalance f ...
... In the beginning there was nothing, and then the big bang – between 10-44 and 10-35 seconds the universe expands from a pinprick to larger than we can presently see (This is the INFLATION ERA.) Then there is energy and the expanding universe cools and matter and antimatter appear. A tiny imbalance f ...
Cosmological Inflation: a Personal Perspective
... • The simplest assumption is that within a horizon size the color forces almost cancel (but not exactly). Statistical fluctuations of color of order N1/2, where N is the number of quarks within the horizon (minimum entropy production; Kazanas 1978). • More favorable scenarios could lead to much larg ...
... • The simplest assumption is that within a horizon size the color forces almost cancel (but not exactly). Statistical fluctuations of color of order N1/2, where N is the number of quarks within the horizon (minimum entropy production; Kazanas 1978). • More favorable scenarios could lead to much larg ...
Big Bang Theory notes
... 1. What is the name of the enormous cloud of gas & dust within space that formed the solar system? 2. What 2 forces give the sun its spherical shape? 3. What is the main form of radiation the sun produces? 4. How is the sun giving off radiation like boiling water? Explain the change in energy from b ...
... 1. What is the name of the enormous cloud of gas & dust within space that formed the solar system? 2. What 2 forces give the sun its spherical shape? 3. What is the main form of radiation the sun produces? 4. How is the sun giving off radiation like boiling water? Explain the change in energy from b ...
The Atom
... Einstein’s equation E = mc2 enables us to relate the energy released to the mass loss in the formation of atoms. Use the known values for the mass of a proton, 1.0073 amu, mass of a neutron, 1.0087, and the mass of an electron, 5.486 x 10-4 amu, to show that the mass of a 12C atom is less than the s ...
... Einstein’s equation E = mc2 enables us to relate the energy released to the mass loss in the formation of atoms. Use the known values for the mass of a proton, 1.0073 amu, mass of a neutron, 1.0087, and the mass of an electron, 5.486 x 10-4 amu, to show that the mass of a 12C atom is less than the s ...
PowerPoint Presentation - The Origin of the Universe
... If the universe were infinite in size & contained an infinite number of stars that live forever, then every line-of-sight would eventually lead to a star Stars light dims as 1/r2 but the volume of space sampled increases by the same factor So, the night sky should be as bright everywhere as the aver ...
... If the universe were infinite in size & contained an infinite number of stars that live forever, then every line-of-sight would eventually lead to a star Stars light dims as 1/r2 but the volume of space sampled increases by the same factor So, the night sky should be as bright everywhere as the aver ...
Answers - Physics and Astronomy
... QUESTION 17: The universe became transparent when electrons and protons formed hydrogen atoms because: a) Atoms only absorb certain wavelengths of light b) The density of matter was so low c) Nucleosynthesis finally ceased d) There is less chance that a photon will hit an atom than an electron e) Th ...
... QUESTION 17: The universe became transparent when electrons and protons formed hydrogen atoms because: a) Atoms only absorb certain wavelengths of light b) The density of matter was so low c) Nucleosynthesis finally ceased d) There is less chance that a photon will hit an atom than an electron e) Th ...
Document
... • Sound of a fire truck siren - pitch of the siren is higher as the fire truck moves towards you, and lower as it moves away from you • Visible wavelengths emitted by objects moving away from us are shifted towards the red part of the visible spectrum • The faster they move away from us, the more th ...
... • Sound of a fire truck siren - pitch of the siren is higher as the fire truck moves towards you, and lower as it moves away from you • Visible wavelengths emitted by objects moving away from us are shifted towards the red part of the visible spectrum • The faster they move away from us, the more th ...
Chapter 34: Cosmology FYI 1. Radar Ranging 2. Triangulation idea
... huge clouds of hydrogen gas. •Particularly dense regions compressed by gravity to for stars. •Currently our universe is dominated by fusion of hydrogen to form helium. •Structure is stable now, but what happens when hydrogen is used up ...
... huge clouds of hydrogen gas. •Particularly dense regions compressed by gravity to for stars. •Currently our universe is dominated by fusion of hydrogen to form helium. •Structure is stable now, but what happens when hydrogen is used up ...
Section 7 The Big Bang Theory
... Today, CMB radiation is very cold, only 2.725 K above absolute zero and this cooling of the photon means its frequency has reduced until the radiation shines primarily in the microwave portion of the electromagnetic spectrum and is invisible to the naked eye. However, it can be detected everywhere w ...
... Today, CMB radiation is very cold, only 2.725 K above absolute zero and this cooling of the photon means its frequency has reduced until the radiation shines primarily in the microwave portion of the electromagnetic spectrum and is invisible to the naked eye. However, it can be detected everywhere w ...
Home | STA Notes
... graph. It is a way of displaying information about stars and showing trends and patterns. The scales are usually log-log to cope with the wide range of values (particularly for luminosity) and, by convention, the temperature scale goes backwards - i.e. high temperatures are on the left of the axis. ...
... graph. It is a way of displaying information about stars and showing trends and patterns. The scales are usually log-log to cope with the wide range of values (particularly for luminosity) and, by convention, the temperature scale goes backwards - i.e. high temperatures are on the left of the axis. ...
The Universe - Mrs. Bills Brainy Bunch
... As the universe expanded, it became less dense and began to cool. After only a few seconds, protons, neutrons, and electrons could form. After a few minutes, those subatomic particles ...
... As the universe expanded, it became less dense and began to cool. After only a few seconds, protons, neutrons, and electrons could form. After a few minutes, those subatomic particles ...
How Did We Wind Up in Such an Unlikely Universe?
... For all the steps described above to have happened as outlined, such numbers as the gravitational constant, the charge on the electron, the mass of the electron, the difference between the proton and neutron masses, the density of mass in the universe, the mass of the neutrino, Planck’s constant, an ...
... For all the steps described above to have happened as outlined, such numbers as the gravitational constant, the charge on the electron, the mass of the electron, the difference between the proton and neutron masses, the density of mass in the universe, the mass of the neutrino, Planck’s constant, an ...
ps700-coll1-hayden
... life. Outside the band there are too few heavy elements and so no planets can form, inside the band there are too many super nova explosions and close encounters with other stars meaning no life can get off the ground before it is destroyed. ...
... life. Outside the band there are too few heavy elements and so no planets can form, inside the band there are too many super nova explosions and close encounters with other stars meaning no life can get off the ground before it is destroyed. ...
The Milky Way Galaxy
... should look essentially the same from any vantage point. No edge and no center! ...
... should look essentially the same from any vantage point. No edge and no center! ...
t 0 (radioactive decay)
... unstable isotopes as a way to estimate the age of stars and the Milky Way Galaxy, and thus t0. Briefly, radioactive decay is the process by which “parent” isotopes spontaneously lose energy and turn into new “daughter” isotopes. The parent isotope’s half-life defines the rate at which this decay occ ...
... unstable isotopes as a way to estimate the age of stars and the Milky Way Galaxy, and thus t0. Briefly, radioactive decay is the process by which “parent” isotopes spontaneously lose energy and turn into new “daughter” isotopes. The parent isotope’s half-life defines the rate at which this decay occ ...
powerpoint - Physics @ IUPUI
... • This means that how rapidly you fuse protons depends very highly on the temperature (and also on the density squared). • Fusion in the proton – proton chain (sometimes call p-p chain) relies on temperature to the ...
... • This means that how rapidly you fuse protons depends very highly on the temperature (and also on the density squared). • Fusion in the proton – proton chain (sometimes call p-p chain) relies on temperature to the ...
Unit 2 PowerPoint Unit2_BigHistoryProject2013_PPT-7
... • The idea that the Universe had its origins in a single point is called the Big Bang theory. The best evidence suggests that the Big Bang occurred 13.7 billion years ago. • Initially, temperature and pressure in the Universe were so high that matter and energy were an interchangeable blur. As the U ...
... • The idea that the Universe had its origins in a single point is called the Big Bang theory. The best evidence suggests that the Big Bang occurred 13.7 billion years ago. • Initially, temperature and pressure in the Universe were so high that matter and energy were an interchangeable blur. As the U ...
Ch 17n18 AGN Cosmology
... obvious, but it has a profound answer: the universe is finite in size and age! 2. The universe is expanding! The redshifts that we measure do NOT result from galaxies flying through space (so NOT Doppler shifts!), but space-time itself expanding and carrying the galaxies with it—as if on an expandin ...
... obvious, but it has a profound answer: the universe is finite in size and age! 2. The universe is expanding! The redshifts that we measure do NOT result from galaxies flying through space (so NOT Doppler shifts!), but space-time itself expanding and carrying the galaxies with it—as if on an expandin ...
Document
... • Cosmology is one of the most exciting subfields of physics these days • The is an intimate connection between cosmology and particle physics • We live in a “golden age” of cosmology: lots of data available and being measured • Today’s era is that of “precision cosmology” • There is lot’s we don’t ...
... • Cosmology is one of the most exciting subfields of physics these days • The is an intimate connection between cosmology and particle physics • We live in a “golden age” of cosmology: lots of data available and being measured • Today’s era is that of “precision cosmology” • There is lot’s we don’t ...
1.3. Basic Principles of Nuclear Physics
... Nuclear Decay & Radioactivity Nuclei are only in certain Z,N configuration stable (minimum of energy E=mc2 ) Otherwise nucleus ‘decays’ by particle or radiation emission to energetically more favorable configuration! ...
... Nuclear Decay & Radioactivity Nuclei are only in certain Z,N configuration stable (minimum of energy E=mc2 ) Otherwise nucleus ‘decays’ by particle or radiation emission to energetically more favorable configuration! ...
Lecture 9
... This marks the Big Bang, or start of the Universe. Currently, science cannot answer what caused this event. But science can describe the universe in detail from 10-43 seconds after the event to the present day! ...
... This marks the Big Bang, or start of the Universe. Currently, science cannot answer what caused this event. But science can describe the universe in detail from 10-43 seconds after the event to the present day! ...