Week 1: Nuclear timeline (pdf, 233 KB)
... besides work on electrodynamics did fundamental work on the kinetic energy of gasses. But in addition to Maxwell, that line would also include a large number of developments in the late 19th century, many with French names associated with them that do not appear here.! ...
... besides work on electrodynamics did fundamental work on the kinetic energy of gasses. But in addition to Maxwell, that line would also include a large number of developments in the late 19th century, many with French names associated with them that do not appear here.! ...
TIMELINE OF NUCLEAR PHYSICS
... besides work on electrodynamics did fundamental work on the kinetic energy of gasses. But in addition to Maxwell, that line would also include a large number of developments in the late 19th century, many with French names associated with them that do not appear here. 350 BC Aristotle defined an ele ...
... besides work on electrodynamics did fundamental work on the kinetic energy of gasses. But in addition to Maxwell, that line would also include a large number of developments in the late 19th century, many with French names associated with them that do not appear here. 350 BC Aristotle defined an ele ...
1 - TeacherWeb
... 39. Most stars are in the “main sequence” of their life cycle and burn for billions of years. Why don’t stars in the main sequence either explode right away or become crushed by their own gravity? ...
... 39. Most stars are in the “main sequence” of their life cycle and burn for billions of years. Why don’t stars in the main sequence either explode right away or become crushed by their own gravity? ...
Big Bang - schoolphysics
... time and space began at that moment. Before the Big Bang there was no space or time – a very difficult idea to grasp. Anyway we do have some idea of what happened after the Big Bang. The temperature in that explosion was unbelievably large – astrophysicists think it may have been as high as 1000 mil ...
... time and space began at that moment. Before the Big Bang there was no space or time – a very difficult idea to grasp. Anyway we do have some idea of what happened after the Big Bang. The temperature in that explosion was unbelievably large – astrophysicists think it may have been as high as 1000 mil ...
Chapter 4 Galactic Chemical Evolution
... The material we find around us in the Universe today contains significant quantities of heavy elements, although these are still only minor contributors to the total mass of baryonic matter (most is hydrogen). These heavy elements have been synthesised in nuclear reactions in stars, a process known ...
... The material we find around us in the Universe today contains significant quantities of heavy elements, although these are still only minor contributors to the total mass of baryonic matter (most is hydrogen). These heavy elements have been synthesised in nuclear reactions in stars, a process known ...
Astronomy 115 Homework Set #1 – Due: Thursday, Feb
... In what ways did supernova 1987A confirm our models of supernova explosions? In what ways did it challenge it? ...
... In what ways did supernova 1987A confirm our models of supernova explosions? In what ways did it challenge it? ...
The Evolution of Elements and Isotopes
... numerous theoretical possibilities. Major insights come add up to the observed composition. In both processes, from recent advances in astronomy, which are beginning seed nuclei capture neutrons until unstable isotopes form. to revolutionize our understanding of chemical evolution. These isotopes th ...
... numerous theoretical possibilities. Major insights come add up to the observed composition. In both processes, from recent advances in astronomy, which are beginning seed nuclei capture neutrons until unstable isotopes form. to revolutionize our understanding of chemical evolution. These isotopes th ...
High Mass Stars
... core to much higher temperatures than in low-mass stars. Fusion rate increases with temperature. In a high-mass star, hydrogen fusion occurs through the CNO cycle rather than through the proton-proton chain ...
... core to much higher temperatures than in low-mass stars. Fusion rate increases with temperature. In a high-mass star, hydrogen fusion occurs through the CNO cycle rather than through the proton-proton chain ...
![Dust [12.1]](http://s1.studyres.com/store/data/008843506_1-c0b3bc1292042697e2dbc020b2f06e1c-300x300.png)
Dust [12.1]
... B2FH (1957) Formation of the Chemical Elements Burbidge, Burbidge, Fowler & Hoyle. Reviews of Modern Physics, 29, 547. ...
... B2FH (1957) Formation of the Chemical Elements Burbidge, Burbidge, Fowler & Hoyle. Reviews of Modern Physics, 29, 547. ...
1)2 A light year is a) about six trillion miles. b) the distance to the star
... By 0.001 seconds after time began, all the protons in my brain were created from the quarks that arose from the energy of the Big Bang. ...
... By 0.001 seconds after time began, all the protons in my brain were created from the quarks that arose from the energy of the Big Bang. ...
Iron in Stars
... Are there stars with no iron or other heavy elements in their atmosphere? So far, no star has been observed that has no iron or other heavy elements in its atmosphere. But the current theories of Big Bang cosmology predict there must have been some stars which were composed almost only of hydrogen a ...
... Are there stars with no iron or other heavy elements in their atmosphere? So far, no star has been observed that has no iron or other heavy elements in its atmosphere. But the current theories of Big Bang cosmology predict there must have been some stars which were composed almost only of hydrogen a ...
Announcements - Lick Observatory
... that neutronization occurs converting the electrons and protons into neutrons and releasing a blast of neutrinos ...
... that neutronization occurs converting the electrons and protons into neutrons and releasing a blast of neutrinos ...
Big Bang
... Idea of initial dense “primeval atom”: Georges Lemaître (1931). Coining of phrase “Big Bang”: Fred Hoyle (1949). ...
... Idea of initial dense “primeval atom”: Georges Lemaître (1931). Coining of phrase “Big Bang”: Fred Hoyle (1949). ...
Planets and Life - Indiana University Astronomy
... The universe is roughly 1/4 helium and 3/4 hydrogen by mass, but very little of this helium was made in stars. Early in the Big Bang the Universe was hot and dense (like the core of a star) and protons could fuse together to make some helium. The fact that the Universe is 1/4 helium is evidence for ...
... The universe is roughly 1/4 helium and 3/4 hydrogen by mass, but very little of this helium was made in stars. Early in the Big Bang the Universe was hot and dense (like the core of a star) and protons could fuse together to make some helium. The fact that the Universe is 1/4 helium is evidence for ...
The Big Bang Theory
... • 13.8 billion years ago all the matter in the universe was very hot and dense • Since then, it has expanded and continues to expand **current theory** ...
... • 13.8 billion years ago all the matter in the universe was very hot and dense • Since then, it has expanded and continues to expand **current theory** ...
1 Origin of the Elements. Isotopes and Atomic Weights
... catastrophic changes may then occur which result in much of the stellar material being ejected into space, where it becomes incorporated together with further hydrogen and helium in the next generation of stars. It should be noted, however, that, as iron is at the maximum of the nuclear binding ener ...
... catastrophic changes may then occur which result in much of the stellar material being ejected into space, where it becomes incorporated together with further hydrogen and helium in the next generation of stars. It should be noted, however, that, as iron is at the maximum of the nuclear binding ener ...
Astronomy The Night Sky. Vocabulary Terms to know for the
... 1. Most ___________________ is in the form of stars or star dust. (You and I are star dust!!) 2. On the ________________________, stars are classified according to their _______________________________ and ____________________ (how bright the star REALLY is). See page 15 of ESRT. 3. All stars begin ...
... 1. Most ___________________ is in the form of stars or star dust. (You and I are star dust!!) 2. On the ________________________, stars are classified according to their _______________________________ and ____________________ (how bright the star REALLY is). See page 15 of ESRT. 3. All stars begin ...
Excited states of 136−138Sb from β decay
... Sn, with N ≥ 82, have some of the highest impact on the final r-process abundances1,2) . Studies of the nuclear structure of the nuclei 135−139 Sb can therefore provide important input into r-process calculations, especially as the exact site of this astrophysical reaction is presently unclear. The ...
... Sn, with N ≥ 82, have some of the highest impact on the final r-process abundances1,2) . Studies of the nuclear structure of the nuclei 135−139 Sb can therefore provide important input into r-process calculations, especially as the exact site of this astrophysical reaction is presently unclear. The ...
Cosmology Unit – FINAL EXAM PRACTICE TEST
... b) The cosmic microwave background radiation is a remnant of the Big Bang. c) There are galaxies outside our own Milky Way, and nearly all of them are getting farther away. d) The steadystate theory is not a correct explanation for the continuing evolution of the universe. 5. What evidence supports ...
... b) The cosmic microwave background radiation is a remnant of the Big Bang. c) There are galaxies outside our own Milky Way, and nearly all of them are getting farther away. d) The steadystate theory is not a correct explanation for the continuing evolution of the universe. 5. What evidence supports ...
The Abundances of the Fe Group Elements in Three Early B Stars in
... the FUSE spacecraft in July and August of 2003. The observations of NGC1818-D1 were carried through with the LWRS aperture, but the MDRS aperture was used for the stars in NGC 2004 to avoid light contamination from several nearby bright stars. Data from each of the channels were smoothed with a stan ...
... the FUSE spacecraft in July and August of 2003. The observations of NGC1818-D1 were carried through with the LWRS aperture, but the MDRS aperture was used for the stars in NGC 2004 to avoid light contamination from several nearby bright stars. Data from each of the channels were smoothed with a stan ...
MAJOR NUCLEAR BURNING STAGES The Coulomb barrier is
... Following the Triple-alpha process there are a variety of reactions which may occur depending on the mass of the star. Three general principles influence the roles that these nuclear burning stages may play: 1.Successive nuclear burning stages, involving more massive nuclei with higher charges, will ...
... Following the Triple-alpha process there are a variety of reactions which may occur depending on the mass of the star. Three general principles influence the roles that these nuclear burning stages may play: 1.Successive nuclear burning stages, involving more massive nuclei with higher charges, will ...
Lecture 24 Early Universe
... The names of quark flavours (up, down, strange, charm, bottom, and top) were also chosen arbitrarily based on the need to name them something that could be easily remembered and used. An important property of quarks is called confinement, which states that individual quarks are not seen because they ...
... The names of quark flavours (up, down, strange, charm, bottom, and top) were also chosen arbitrarily based on the need to name them something that could be easily remembered and used. An important property of quarks is called confinement, which states that individual quarks are not seen because they ...
Nucleosynthesis
Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons. The first nuclei were formed about three minutes after the Big Bang, through the process called Big Bang nucleosynthesis. It was then that hydrogen and helium formed to become the content of the first stars, and this primeval process is responsible for the present hydrogen/helium ratio of the cosmos.With the formation of stars, heavier nuclei were created from hydrogen and helium by stellar nucleosynthesis, a process that continues today. Some of these elements, particularly those lighter than iron, continue to be delivered to the interstellar medium when low mass stars eject their outer envelope before they collapse to form white dwarfs. The remains of their ejected mass form the planetary nebulae observable throughout our galaxy.Supernova nucleosynthesis within exploding stars by fusing carbon and oxygen is responsible for the abundances of elements between magnesium (atomic number 12) and nickel (atomic number 28). Supernova nucleosynthesis is also thought to be responsible for the creation of rarer elements heavier than iron and nickel, in the last few seconds of a type II supernova event. The synthesis of these heavier elements absorbs energy (endothermic) as they are created, from the energy produced during the supernova explosion. Some of those elements are created from the absorption of multiple neutrons (the R process) in the period of a few seconds during the explosion. The elements formed in supernovas include the heaviest elements known, such as the long-lived elements uranium and thorium.Cosmic ray spallation, caused when cosmic rays impact the interstellar medium and fragment larger atomic species, is a significant source of the lighter nuclei, particularly 3He, 9Be and 10,11B, that are not created by stellar nucleosynthesis.In addition to the fusion processes responsible for the growing abundances of elements in the universe, a few minor natural processes continue to produce very small numbers of new nuclides on Earth. These nuclides contribute little to their abundances, but may account for the presence of specific new nuclei. These nuclides are produced via radiogenesis (decay) of long-lived, heavy, primordial radionuclides such as uranium and thorium. Cosmic ray bombardment of elements on Earth also contribute to the presence of rare, short-lived atomic species called cosmogenic nuclides.