Big-Bang
... of stars forming was based on the speculative ‘EGG-star formation theory.’ It has recently been tested independently with two infrared detectors that can see inside the dusty pillars. ...
... of stars forming was based on the speculative ‘EGG-star formation theory.’ It has recently been tested independently with two infrared detectors that can see inside the dusty pillars. ...
Forging the elements
... • Typical mass of the central core is somewhere between 0.5 to 1.0 solar masses, with a size close to that of the Earth. • All nuclear burning ceases – have a white dwarf • They cool and dim and after billions of years become undetectable (become a “black dwarf”). • Over 95% of the stars in our Gala ...
... • Typical mass of the central core is somewhere between 0.5 to 1.0 solar masses, with a size close to that of the Earth. • All nuclear burning ceases – have a white dwarf • They cool and dim and after billions of years become undetectable (become a “black dwarf”). • Over 95% of the stars in our Gala ...
Physics Chapter 22 Notes New book Atoms are composed of
... Nuclear reactors are designed to maintain a controlled, self-sustained chain reaction, for the production of energy. At this point, all nuclear reactors are fission reactors. Bad news: The radioactive by-products of nuclear energy have half-lives of 10,000 years or longer. ...
... Nuclear reactors are designed to maintain a controlled, self-sustained chain reaction, for the production of energy. At this point, all nuclear reactors are fission reactors. Bad news: The radioactive by-products of nuclear energy have half-lives of 10,000 years or longer. ...
Introduction to Stellar Evolution
... Ignites to Si, S Si, S to Fe peak elements (Ni, Ti, lots of Fe) Now stellar core can do no more burning to produce energy So it collapses and Explodes as a Supernova ...
... Ignites to Si, S Si, S to Fe peak elements (Ni, Ti, lots of Fe) Now stellar core can do no more burning to produce energy So it collapses and Explodes as a Supernova ...
Lectures 12 & 13 powerpoint (stellar death)
... Q: How can the inward collapse of the 1. Fe nuclei capture electrons core produce an outward explosion? Fe nuclei break apart into smaller nuclei, and the A: As the matter falls inward, it creates a degenerate electrons that shockwave that travels outward. supported the core are This shockwave is ...
... Q: How can the inward collapse of the 1. Fe nuclei capture electrons core produce an outward explosion? Fe nuclei break apart into smaller nuclei, and the A: As the matter falls inward, it creates a degenerate electrons that shockwave that travels outward. supported the core are This shockwave is ...
Background Presentation
... The NASA E/PO Program at Sonoma State University A group of people working collaboratively to educate the public about current and future NASA high energy astrophysics/astronomy missions. Swift Led by Prof. Lynn Cominsky ...
... The NASA E/PO Program at Sonoma State University A group of people working collaboratively to educate the public about current and future NASA high energy astrophysics/astronomy missions. Swift Led by Prof. Lynn Cominsky ...
What is the Big Bang Theory?
... into a tiny dot called Singularity. A huge explosion, referred to by astronomers as the Big Bang, sent the entire universe flying out at incredible speeds. ...
... into a tiny dot called Singularity. A huge explosion, referred to by astronomers as the Big Bang, sent the entire universe flying out at incredible speeds. ...
PowerPoint version is here
... • Reflect processes in the early galaxy • Investigation of Pop II stars is a hot area of astrophysics What are Pop III stars? • Stars that produce the material from which Pop II are made. • Probably very large (> 100 Msun) fast evolving stars made from products of the Big Bang. ...
... • Reflect processes in the early galaxy • Investigation of Pop II stars is a hot area of astrophysics What are Pop III stars? • Stars that produce the material from which Pop II are made. • Probably very large (> 100 Msun) fast evolving stars made from products of the Big Bang. ...
Stats talk - Harvard University
... • To avoid implosion stars must generate energy from fusion reactions •The stages of stars are determined by the type of fuel left: hydrogen, helium, carbon etc ...
... • To avoid implosion stars must generate energy from fusion reactions •The stages of stars are determined by the type of fuel left: hydrogen, helium, carbon etc ...
Image of the day
... should see for electromagnetic radiation when the universe first became transparent to photons. The fact that the radiation is essentially the same frequency everywhere in the universe means we are looking at evidence for a single event. More evidence: Gravitational waves are 'ripples' in the fabric ...
... should see for electromagnetic radiation when the universe first became transparent to photons. The fact that the radiation is essentially the same frequency everywhere in the universe means we are looking at evidence for a single event. More evidence: Gravitational waves are 'ripples' in the fabric ...
The Life Cycles of Stars MEDIUM STARS MASSIVE STARS
... massive star that is 1.5 to 4 times as massive as our Sun ends up as a neutron star after the supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star's spin), these neutron stars are called pulsars. The core of a massive star that has 8 ...
... massive star that is 1.5 to 4 times as massive as our Sun ends up as a neutron star after the supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star's spin), these neutron stars are called pulsars. The core of a massive star that has 8 ...
COSMOLOGY A FLAT EARTH GEOCENTRIC MODEL or the
... The CMB is one of the strongest pieces of evidence for the Big Bang model. The Big Bang theory makes highly accurate predictions about the size and types of anisotropies in the CMB as well as its nearly perfect blackbody spectrum, all of which have been verified by experiment and observations. ...
... The CMB is one of the strongest pieces of evidence for the Big Bang model. The Big Bang theory makes highly accurate predictions about the size and types of anisotropies in the CMB as well as its nearly perfect blackbody spectrum, all of which have been verified by experiment and observations. ...
How stars form slide show File
... protons prevents them becoming close when they move towards each other. • As the temperature increases further the protons become closer. During nuclear fusion two protons become so close that the ‘Strong nuclear force’ grabs them and holds them together, this releases lots of energy. •This force on ...
... protons prevents them becoming close when they move towards each other. • As the temperature increases further the protons become closer. During nuclear fusion two protons become so close that the ‘Strong nuclear force’ grabs them and holds them together, this releases lots of energy. •This force on ...
Time Domain Astrophysics in South Africa 2
... • Monitoring Time variations in intrinsic variables in order to infer their properties such as mass, luminosity, rotation rate, internal composition ...
... • Monitoring Time variations in intrinsic variables in order to infer their properties such as mass, luminosity, rotation rate, internal composition ...
Milky Way Galaxy
... formed approximately 14 billion years ago. Contained in the Milky Way are stars, clouds of dust and gas called nebulae, planets, and asteroids. Stars, dust, and gas fan out from the center of the Galaxy in long spiraling arms. The Milky Way is approximately 100,000 light-years in diameter. Our solar ...
... formed approximately 14 billion years ago. Contained in the Milky Way are stars, clouds of dust and gas called nebulae, planets, and asteroids. Stars, dust, and gas fan out from the center of the Galaxy in long spiraling arms. The Milky Way is approximately 100,000 light-years in diameter. Our solar ...
Space Science cource, Department of Physics, Faculty of
... maser source S Crt at 350 pc (Tsushima 2007) ...
... maser source S Crt at 350 pc (Tsushima 2007) ...
ASTR 1020 FINAL EXAM STUDY GUIDE
... rapidly fusing into helium. You notice that your surroundings are cooling and rapidly dropping in density. Within about 3 minutes, the fusion reactions stop. Where are you? 5) You find yourself in a place that looks perfectly symmetrical. There is no way to distinguish one place from another, and al ...
... rapidly fusing into helium. You notice that your surroundings are cooling and rapidly dropping in density. Within about 3 minutes, the fusion reactions stop. Where are you? 5) You find yourself in a place that looks perfectly symmetrical. There is no way to distinguish one place from another, and al ...
1.2.43The stellar populations of the Milky Way
... Pop. II stars occupy the spheroid – the stellar halo and bulge – and turn out to be the oldest stars known, with ages in the range (12 to 15) × 1091yr. Conspicuous examples are globular-cluster stars. Little or no interstellar gas is still associated with Pop. II stars, which is consistent with star ...
... Pop. II stars occupy the spheroid – the stellar halo and bulge – and turn out to be the oldest stars known, with ages in the range (12 to 15) × 1091yr. Conspicuous examples are globular-cluster stars. Little or no interstellar gas is still associated with Pop. II stars, which is consistent with star ...
Astronomy 104: Stellar Astronomy
... A.The core cools off. B.The core shrinks and heats up. C.The core expands and heats up. D.The core has to start fusing iron, since it is the only fuel available. ...
... A.The core cools off. B.The core shrinks and heats up. C.The core expands and heats up. D.The core has to start fusing iron, since it is the only fuel available. ...
Information
... mass number (A) – total number of heavy particles (protons and neutrons, jointly called nucleons) in the nucleus of an atom [703]. [return] mole fraction (amount fraction or isotopic abundance) – the amount (symbol n) of a given isotope (atom) in a sample divided by the total amount of all stable a ...
... mass number (A) – total number of heavy particles (protons and neutrons, jointly called nucleons) in the nucleus of an atom [703]. [return] mole fraction (amount fraction or isotopic abundance) – the amount (symbol n) of a given isotope (atom) in a sample divided by the total amount of all stable a ...
Stars and Galaxies
... crushes into a black hole. A black hole is an object whose gravity is so great that no light can escape. ...
... crushes into a black hole. A black hole is an object whose gravity is so great that no light can escape. ...
Stellar Evolution in the HR Diagram
... Electron degeneracy cannot support cores more massive than 1.4 M. If a degenerate C/O core (i.e., a white dwarf) is pushed above this limit, it was collapse and begin fusing, but it will not have time to adjust its structure (all the energy will just go into lifting the degeneracy). The star will b ...
... Electron degeneracy cannot support cores more massive than 1.4 M. If a degenerate C/O core (i.e., a white dwarf) is pushed above this limit, it was collapse and begin fusing, but it will not have time to adjust its structure (all the energy will just go into lifting the degeneracy). The star will b ...
Astro Review - Blank - Mayfield City Schools
... 3. ___d_ apparent shift toward shorter wavelengths of light when a luminous object moves toward the Viewer 5. ___a_ sum of all space, matter and energy 6. ___g_ matter not visible through current methods, but observable through gravitational interactions between galaxies 7. ___b_ apparent shift towa ...
... 3. ___d_ apparent shift toward shorter wavelengths of light when a luminous object moves toward the Viewer 5. ___a_ sum of all space, matter and energy 6. ___g_ matter not visible through current methods, but observable through gravitational interactions between galaxies 7. ___b_ apparent shift towa ...
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.