atoms, three states of matter.
... The Kelvin scale is based upon the absolute zero point where the velocity of gas atoms or molecules would be zero. That is, 0 K corresponds to -273o C. The relationship between the Celsius and Kelvin scales is then ...
... The Kelvin scale is based upon the absolute zero point where the velocity of gas atoms or molecules would be zero. That is, 0 K corresponds to -273o C. The relationship between the Celsius and Kelvin scales is then ...
regan-gas-10jul2010
... – Hydrogen to Helium (in the sun, p-p chain CNO cycles). – Helium to Carbon, triple-alpha process, special fusion. – Carbon to iron: nuclear fusion reactions, if hot enough. ...
... – Hydrogen to Helium (in the sun, p-p chain CNO cycles). – Helium to Carbon, triple-alpha process, special fusion. – Carbon to iron: nuclear fusion reactions, if hot enough. ...
OVERVIEW ABSTRACT HST/COS chemical abundance analysis of
... We present new Near-UltraViolet (NUV) elemental abundance analysis, for the hyper metal-poor 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 pr ...
... We present new Near-UltraViolet (NUV) elemental abundance analysis, for the hyper metal-poor 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 pr ...
Week 1b_2015
... The nature of the condensed matter (planets, moons, asteroids and comets) around the Sun depends on Evolution of the solar system temperature. At a distance equivalent to the Earth from the Sun, the temperature was ~1500oC. Iron (melting point 1538oC) and olivine ((Fe,Mg)2SiO4; melting point 1500 – ...
... The nature of the condensed matter (planets, moons, asteroids and comets) around the Sun depends on Evolution of the solar system temperature. At a distance equivalent to the Earth from the Sun, the temperature was ~1500oC. Iron (melting point 1538oC) and olivine ((Fe,Mg)2SiO4; melting point 1500 – ...
Lecture 9
... Assume now that t = 1 s. Proton-neutron freezeout has just been completed, and the neutron-to-proton ratio is nn /np = 1/5. Big Bang Nucleosynthesis takes place through a series of two-body reactions, building more massive nuclei step by step. The essential first step is the fusion of a proton and a ...
... Assume now that t = 1 s. Proton-neutron freezeout has just been completed, and the neutron-to-proton ratio is nn /np = 1/5. Big Bang Nucleosynthesis takes place through a series of two-body reactions, building more massive nuclei step by step. The essential first step is the fusion of a proton and a ...
Nucleosynthesis, the r-Process, Abundances and Jim Truran
... r-process elements observed in very metal-poor (old) halo stars – they are ubiquitous Implies that r-process sites, earliest stellar generations rapidly evolving: live and die, eject r-process material into ISM prior to formation of halo stars exact site still unknown Elements (even s-process ones l ...
... r-process elements observed in very metal-poor (old) halo stars – they are ubiquitous Implies that r-process sites, earliest stellar generations rapidly evolving: live and die, eject r-process material into ISM prior to formation of halo stars exact site still unknown Elements (even s-process ones l ...
Stellar Deaths - Mid
... What Powers the Sun? Nuclear Fusion: An event where the nuclei of two atoms join together. Need high temperatures. Why? To overcome electric repulsion. Energy is produced. (A small amount of mass = a lot of energy) E = mc2. Sum of mass and energy always conserved in reactions. Mass is just “frozen” ...
... What Powers the Sun? Nuclear Fusion: An event where the nuclei of two atoms join together. Need high temperatures. Why? To overcome electric repulsion. Energy is produced. (A small amount of mass = a lot of energy) E = mc2. Sum of mass and energy always conserved in reactions. Mass is just “frozen” ...
Video Worksheet Beyond the Big Bang (Part 2 of 2)
... 4. Hubble wrongly calculated that the universe was only _________ billion years old. ...
... 4. Hubble wrongly calculated that the universe was only _________ billion years old. ...
Final Exam Study Guide
... The escape velocity of a neutron star (speed you need to escape it) is about ________. A planetary nebula is typically formed at the same time as a(n) _______________. The process in which many stars form from a single interstellar cloud is called _______. Interstellar clouds cause stars behind them ...
... The escape velocity of a neutron star (speed you need to escape it) is about ________. A planetary nebula is typically formed at the same time as a(n) _______________. The process in which many stars form from a single interstellar cloud is called _______. Interstellar clouds cause stars behind them ...
Lecture 6 - Concord University
... neutrons An element is defined by the number of protons ◦ It’s atomic number ◦ Isotopes all have the same number of protons ◦ They are all of the same element ◦ They only differ in total mass or number or neutrons ...
... neutrons An element is defined by the number of protons ◦ It’s atomic number ◦ Isotopes all have the same number of protons ◦ They are all of the same element ◦ They only differ in total mass or number or neutrons ...
Stellar evolution
... • The implosion produces enough energy to create a supernova. • The supernova can last weeks or months, and release as much energy as the sun does in its entire lifespan. • The supernova is a main source of heavy elements in the universe. • The remaining core will collapse into either a neutron star ...
... • The implosion produces enough energy to create a supernova. • The supernova can last weeks or months, and release as much energy as the sun does in its entire lifespan. • The supernova is a main source of heavy elements in the universe. • The remaining core will collapse into either a neutron star ...
answers2008_09_BC
... loses mass through stellar wind. Eventually all outer layers will be lost, forming a planetary nebula, and He fusion will stop; central carbon core will survive to radiate its stored heat as a white dwarf (bottom left of HRD) ...
... loses mass through stellar wind. Eventually all outer layers will be lost, forming a planetary nebula, and He fusion will stop; central carbon core will survive to radiate its stored heat as a white dwarf (bottom left of HRD) ...
Astronomy
... book, notes and each other to correctly describe star formation, using terms such as nuclear fusion, protostar, Ttauri star, interstellar cloud, fragmenting, shock waves, temperatures at various important events, what is the cause of each stage and other important pieces. Do this on a full piece of ...
... book, notes and each other to correctly describe star formation, using terms such as nuclear fusion, protostar, Ttauri star, interstellar cloud, fragmenting, shock waves, temperatures at various important events, what is the cause of each stage and other important pieces. Do this on a full piece of ...
Lecture 16
... Suppose the universe contained only lowmass stars. Would elements heavier than carbon exist? A. Yes, all stars create heavier elements than carbon when they become a supernova. B. Yes, but there would be far fewer heavier elements because high-mass stars form elements like iron far more prolificall ...
... Suppose the universe contained only lowmass stars. Would elements heavier than carbon exist? A. Yes, all stars create heavier elements than carbon when they become a supernova. B. Yes, but there would be far fewer heavier elements because high-mass stars form elements like iron far more prolificall ...
The solar system rotates around the sun due to the sun`s
... Scientist have studied nine different stars (A-I) and nine different galaxies (1-9). T hey documented what percent of shift each star and galaxies had. T he data is shown below. Which statement below best supports the data? A ...
... Scientist have studied nine different stars (A-I) and nine different galaxies (1-9). T hey documented what percent of shift each star and galaxies had. T he data is shown below. Which statement below best supports the data? A ...
Stars III - Indiana University Astronomy
... The Origin of Elements • The process by which elements (nuclei) are created (synthesized) is called nucleosynthesis • Nucleosynthesis has occurred since the creation of the universe and will essentially go on forever • The elements created come together to form everything material we know, includin ...
... The Origin of Elements • The process by which elements (nuclei) are created (synthesized) is called nucleosynthesis • Nucleosynthesis has occurred since the creation of the universe and will essentially go on forever • The elements created come together to form everything material we know, includin ...
Energy Production in Stars
... What is the source of their enormous energy? o Thermonuclear reactions (fusion) that convert mass to energy In the special theory of relativity Einstein demonstrated that the total mass-energy was conserved => e = mc2 Speed of light squared is a very large number => small amount of mass corres ...
... What is the source of their enormous energy? o Thermonuclear reactions (fusion) that convert mass to energy In the special theory of relativity Einstein demonstrated that the total mass-energy was conserved => e = mc2 Speed of light squared is a very large number => small amount of mass corres ...
What Are We Made Of? - University of Louisville
... universe are gravitational, electromagnetic and nuclear. The interaction of these three forces determines the structure of matter. • The nuclear force overpowers the opposing electromagnetic force of protons in the nucleus. • The electrons (-) orbit the nucleus (+), being pulled by the electromagnet ...
... universe are gravitational, electromagnetic and nuclear. The interaction of these three forces determines the structure of matter. • The nuclear force overpowers the opposing electromagnetic force of protons in the nucleus. • The electrons (-) orbit the nucleus (+), being pulled by the electromagnet ...
DUST FROM EVOLVED STARS TO PROTOSTARS. A. K. Speck
... A. K. Speck, University of Missouri ([email protected]) Introduction: Dust is a vital ingredient in understanding many astrophysical processes [e.g. 1, 2, 3]. It is an essential part of star formation processes; it is the key to understanding mass loss from aging stars [e.g. 4]; and it contribute ...
... A. K. Speck, University of Missouri ([email protected]) Introduction: Dust is a vital ingredient in understanding many astrophysical processes [e.g. 1, 2, 3]. It is an essential part of star formation processes; it is the key to understanding mass loss from aging stars [e.g. 4]; and it contribute ...
PHY111 Stellar Evolution
... these are rare isotopes, so whatever process makes them is unusual or difficult a number of different processes are thought to contribute, mainly p s s,r r γ + AX A−1X + n in supernovae, but also p + AX A+1X' + γ in very proton-rich environments ...
... these are rare isotopes, so whatever process makes them is unusual or difficult a number of different processes are thought to contribute, mainly p s s,r r γ + AX A−1X + n in supernovae, but also p + AX A+1X' + γ in very proton-rich environments ...
The Emerging Theory of Supernova Explosions
... Talk Title: "The Emerging Theory of Supernova Explosions" Abstract: Core-collapse supernovae have challenged theorists and computational science for half a century. Such explosions are the source of many of the heavy elements in the Universe and the birthplace of neutron stars and stellar-mass black ...
... Talk Title: "The Emerging Theory of Supernova Explosions" Abstract: Core-collapse supernovae have challenged theorists and computational science for half a century. Such explosions are the source of many of the heavy elements in the Universe and the birthplace of neutron stars and stellar-mass black ...
Supernova
... • A supernova at a distance of 10 parsecs (32 light years) would appear to be 100 times brighter than the full Moon! • It would cast shadows on the Earth from ...
... • A supernova at a distance of 10 parsecs (32 light years) would appear to be 100 times brighter than the full Moon! • It would cast shadows on the Earth from ...
A Brief History of History
... under gravity formed the first galaxies and that the stars inside these clouds were formed later by the same process on a smaller scale. Stars come next A star is a ball of super-hot gas balanced between the twin tendencies to collapse under its own gravity, and the outward pressure of radiation ene ...
... under gravity formed the first galaxies and that the stars inside these clouds were formed later by the same process on a smaller scale. Stars come next A star is a ball of super-hot gas balanced between the twin tendencies to collapse under its own gravity, and the outward pressure of radiation ene ...
Introduction - Departamento de Astronomía
... 56Fe is the last product of exothermic nuclear fusion reactions, NSE ...
... 56Fe is the last product of exothermic nuclear fusion reactions, NSE ...
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.