Lecture 24 Early Universe - University of Maryland
... • It has fluctuations, with average separations corresponding to a known scale L at the distance where light last interacted with matter (matter/radiation decoupling) • Distance D to this “surface of last scattering” is also known • Can use apparent angular separations of fluctuations compared to L/ ...
... • It has fluctuations, with average separations corresponding to a known scale L at the distance where light last interacted with matter (matter/radiation decoupling) • Distance D to this “surface of last scattering” is also known • Can use apparent angular separations of fluctuations compared to L/ ...
The Big Bang Theory:
... • Radiation appears to be mostly smooth, but there are slight variations in temperature that show that matter had started to clump in the early universe clumps of matter formed the galaxies and stars see today. • Sound waves in early universe are recorded in this radiation; by studying the character ...
... • Radiation appears to be mostly smooth, but there are slight variations in temperature that show that matter had started to clump in the early universe clumps of matter formed the galaxies and stars see today. • Sound waves in early universe are recorded in this radiation; by studying the character ...
Notes: Stellar Nucleosynthesis
... • Begins when two 1H atoms fuse into 2H • positron and neutrino released (energy!) ...
... • Begins when two 1H atoms fuse into 2H • positron and neutrino released (energy!) ...
Our Vast Universe
... The fate of the universe can be determined by measuring how fast the universe expands relative to how much matter the universe contains There are three possible types of expanding universes (ours is unknown): Open-the universe will expand forever Flat-expands forever but expansion rate will slow to ...
... The fate of the universe can be determined by measuring how fast the universe expands relative to how much matter the universe contains There are three possible types of expanding universes (ours is unknown): Open-the universe will expand forever Flat-expands forever but expansion rate will slow to ...
The homogeneous and isotropic universe: Cosmology
... If we consider k=1 (closed) situation is worse, but near to open (k=-1) improves the situation. Results a Λ>0 term is needed and this improves the situation ...
... If we consider k=1 (closed) situation is worse, but near to open (k=-1) improves the situation. Results a Λ>0 term is needed and this improves the situation ...
Abundance of Elements
... D) iron-peak elements :near Fe & Ni ; largest binding energy/nucleon E) the heavy elements, A > 100 :very rare, several abundance peaks ;each peak is actually a ...
... D) iron-peak elements :near Fe & Ni ; largest binding energy/nucleon E) the heavy elements, A > 100 :very rare, several abundance peaks ;each peak is actually a ...
Looking back in time to the big bang theory
... Element can be used as part of teaching this topic or as a consolidation. Learners should be introduced to at least one alternative theory to the Big Bang and reasons why the evidence supports the Big Bang rather than these other theories. Common difficulties and misconceptions include learners thin ...
... Element can be used as part of teaching this topic or as a consolidation. Learners should be introduced to at least one alternative theory to the Big Bang and reasons why the evidence supports the Big Bang rather than these other theories. Common difficulties and misconceptions include learners thin ...
Cosmic Connection to the elements
... This is hot enough for the helium in the core to fuse into carbon. Energy from this reaction sustains the star, keeping it from further collapse. Nitrogen is fused in a similar way. After a much shorter period of time, there is no more material to fuse in the core. The star is left with carbon in it ...
... This is hot enough for the helium in the core to fuse into carbon. Energy from this reaction sustains the star, keeping it from further collapse. Nitrogen is fused in a similar way. After a much shorter period of time, there is no more material to fuse in the core. The star is left with carbon in it ...
Astrophysics * Glossary - Uplift Summit International
... In 1960 it was proposed that sometime during the early history of the Universe it was at a sufficiently high temperature to produce helium by fusion. In this process many high energy photons would be produced. The CMB (Cosmic Microwave Background Radiation) radiation was emitted only a few hundred t ...
... In 1960 it was proposed that sometime during the early history of the Universe it was at a sufficiently high temperature to produce helium by fusion. In this process many high energy photons would be produced. The CMB (Cosmic Microwave Background Radiation) radiation was emitted only a few hundred t ...
Lecture 5
... There have been a number of difficulties associated with using Cepheids as distance indicators. Until recently, astronomers used photographic plates to measure the fluxes from stars. The plates were highly non-linear and often produced faulty flux measurements. Since massive stars are short lived, t ...
... There have been a number of difficulties associated with using Cepheids as distance indicators. Until recently, astronomers used photographic plates to measure the fluxes from stars. The plates were highly non-linear and often produced faulty flux measurements. Since massive stars are short lived, t ...
Slide 1
... There have been a number of difficulties associated with using Cepheids as distance indicators. Until recently, astronomers used photographic plates to measure the fluxes from stars. The plates were highly non-linear and often produced faulty flux measurements. Since massive stars are short lived, t ...
... There have been a number of difficulties associated with using Cepheids as distance indicators. Until recently, astronomers used photographic plates to measure the fluxes from stars. The plates were highly non-linear and often produced faulty flux measurements. Since massive stars are short lived, t ...
MAJOR NUCLEAR BURNING STAGES The Coulomb barrier is
... burning stages may play: 1.Successive nuclear burning stages, involving more massive nuclei with higher charges, will require increasingly high temperatures to overcome the increased electrical repulsion. 2.The amount of energy released by each successive reaction stage decreases so that later nucle ...
... burning stages may play: 1.Successive nuclear burning stages, involving more massive nuclei with higher charges, will require increasingly high temperatures to overcome the increased electrical repulsion. 2.The amount of energy released by each successive reaction stage decreases so that later nucle ...
Cosmology - RHIG - Wayne State University
... This implies that there is a finite age to the universe, it is not eternal. ...
... This implies that there is a finite age to the universe, it is not eternal. ...
Article 8
... pressure in the gas around it that balances the inward pull of gravity. When the released energy reaches the outer layers of the ball of gas and dust, it moves off into space in the form of electromagnetic radiation. The ball, now a star, begins to shine. New stars come in a variety of sizes and col ...
... pressure in the gas around it that balances the inward pull of gravity. When the released energy reaches the outer layers of the ball of gas and dust, it moves off into space in the form of electromagnetic radiation. The ball, now a star, begins to shine. New stars come in a variety of sizes and col ...
Evolution and nucleosynthesis of extremely metal
... high neutron flux in the He-rich convective region, which we call a neutron “superburst”. The neutron flux for the superburst is primarily supplied by 13 C(α,n)16 O reactions occurring at the base of the HeCZ. The 13 C for this reaction is produced as a consequence of the proton ingestion – it is a ...
... high neutron flux in the He-rich convective region, which we call a neutron “superburst”. The neutron flux for the superburst is primarily supplied by 13 C(α,n)16 O reactions occurring at the base of the HeCZ. The 13 C for this reaction is produced as a consequence of the proton ingestion – it is a ...
Cosmology Fact Sheet
... telescope has been looking at these a lot), supernovae (death of stars) and finally looking at the brightness of entire galaxies. Each standard candle must be corroborated by some other distance measurement in order to use it. This other distance measurement may well be another type of standard cand ...
... telescope has been looking at these a lot), supernovae (death of stars) and finally looking at the brightness of entire galaxies. Each standard candle must be corroborated by some other distance measurement in order to use it. This other distance measurement may well be another type of standard cand ...
Survey of the Universe
... units.) Reminder – the heaviest particle discovered to date is the top quark with mass 170 GeV or 170 protons. Candidate particles that theoretical astrophysicists talk about: • WIMPZILLA’s – WIMPs are “Weakly Interacting Massive Particles”, a dark matter candidate particle • “Topological defects” – ...
... units.) Reminder – the heaviest particle discovered to date is the top quark with mass 170 GeV or 170 protons. Candidate particles that theoretical astrophysicists talk about: • WIMPZILLA’s – WIMPs are “Weakly Interacting Massive Particles”, a dark matter candidate particle • “Topological defects” – ...
Introduction: The Night Sky
... helium fusion lasts around one million years carbon fusion lasts 300 years oxygen fusion lasts for 7 months silicon fusion lasts for two days and produces an iron core ...
... helium fusion lasts around one million years carbon fusion lasts 300 years oxygen fusion lasts for 7 months silicon fusion lasts for two days and produces an iron core ...
Lecture 39: Early Universe Test 3 overview 11/21
... depends on Hubble “constant” changes with time. Closed universe has gravity slowing the expansion so it starts to contract. Open universe expands forever. Early universe was very hot and when matter was created. First electrons, protons and neutrons, then protons and neutrons give hydrogen and heliu ...
... depends on Hubble “constant” changes with time. Closed universe has gravity slowing the expansion so it starts to contract. Open universe expands forever. Early universe was very hot and when matter was created. First electrons, protons and neutrons, then protons and neutrons give hydrogen and heliu ...
Nuclear Physics Notes - Reading Community Schools
... It can also be indicated by its name followed by its isotopic mass (ex. Carbon-12 or Uranium-235). Since it is the number of protons that define the identity of the atom, given its atomic name or its atomic number you can identify the atom. The atomic mass number) is the sum of the protons and ne ...
... It can also be indicated by its name followed by its isotopic mass (ex. Carbon-12 or Uranium-235). Since it is the number of protons that define the identity of the atom, given its atomic name or its atomic number you can identify the atom. The atomic mass number) is the sum of the protons and ne ...
natsci9+
... 2s t 103 s, temperature is ~1010 to ~109 K, ~ 10+5 10-1g/cm3, during which primordial element formation occurred Calculations reveal that about 25% of the baryons in the universe should have been converted into He4 during this period, and about 75% should have been left as protons (H1) Traces ...
... 2s t 103 s, temperature is ~1010 to ~109 K, ~ 10+5 10-1g/cm3, during which primordial element formation occurred Calculations reveal that about 25% of the baryons in the universe should have been converted into He4 during this period, and about 75% should have been left as protons (H1) Traces ...
2. The Universe Is Expanding and Evolving
... the surface of last scattering, which occurred 380,000 years after the Big Bang. It’s like a distant wallpaper covering the entire sky behind all the stars and galaxies. This is important, as it means that we can clearly see any structures (irregularities in the distribution of matter) that may be i ...
... the surface of last scattering, which occurred 380,000 years after the Big Bang. It’s like a distant wallpaper covering the entire sky behind all the stars and galaxies. This is important, as it means that we can clearly see any structures (irregularities in the distribution of matter) that may be i ...
OVERVIEW ABSTRACT HST/COS chemical abundance analysis of
... star HE1327-2326 ([Fe/H] = -5.2) using COS/HST data. We detect for the first time 4 Fe II lines, in addition to Zn I and Ni II absorption lines. Fitting the abundances to SNe yield models, lead to Pop III progenitor mass of 28 Msolar and SNe explosion energy of 0.3 Bethe (B). ...
... star HE1327-2326 ([Fe/H] = -5.2) using COS/HST data. We detect for the first time 4 Fe II lines, in addition to Zn I and Ni II absorption lines. Fitting the abundances to SNe yield models, lead to Pop III progenitor mass of 28 Msolar and SNe explosion energy of 0.3 Bethe (B). ...
From Big Bang to Biospheres: The Scope and Limits of Explanation
... will have a ‘grainy’ structure, but on the Planck scale (see Figure 1) which is a trillion trillion times smaller than an atom. (vii)There must be some initial fluctuations for gravity to amplify – sufficient in amplitude to permit the emergence of structures. Otherwise the universe would now be col ...
... will have a ‘grainy’ structure, but on the Planck scale (see Figure 1) which is a trillion trillion times smaller than an atom. (vii)There must be some initial fluctuations for gravity to amplify – sufficient in amplitude to permit the emergence of structures. Otherwise the universe would now be col ...