COSMOLOGY 1 An Introduction to the Universe
... Space Telescope, shows many bright spots along a ring of gas, like pearls on a necklace. These are being produced as a supersonic shock wave unleashed during the explosion slams into the ring at more than a million miles per hour. The collision is heating the gas ring, causing its innermost regions ...
... Space Telescope, shows many bright spots along a ring of gas, like pearls on a necklace. These are being produced as a supersonic shock wave unleashed during the explosion slams into the ring at more than a million miles per hour. The collision is heating the gas ring, causing its innermost regions ...
The Birth of Stars
... an wave moving out at the speed of sound. Material free-falls inside this wave and crashes into a growing (and glowing) central object. We see only the infrared light emerging from the large dust core. ...
... an wave moving out at the speed of sound. Material free-falls inside this wave and crashes into a growing (and glowing) central object. We see only the infrared light emerging from the large dust core. ...
Science Olympiad - UNC Physics and Astronomy
... 700 million tons of hydrogen are converted to helium each second ...
... 700 million tons of hydrogen are converted to helium each second ...
29.3 – Stellar Evolution
... core of a supernova contracts into a small dense ball of neutrons •Neutron star has more mass than the sun and rotates very rapidly •Some neutron stars emit 2 beams of radiation = pulsar ...
... core of a supernova contracts into a small dense ball of neutrons •Neutron star has more mass than the sun and rotates very rapidly •Some neutron stars emit 2 beams of radiation = pulsar ...
Slide 1
... By mid 20th century -- 3 models or theories Big Bang -- Father LeMaitre, George Gamow Oscillating Universe ...
... By mid 20th century -- 3 models or theories Big Bang -- Father LeMaitre, George Gamow Oscillating Universe ...
Booklet 5 – Stellar Processes and Evolution
... Stars with a mass of between 8 and 20 solar masses have a more complex evolution. Initially, they evolve in the same way as low mass stars, turning into red giants and undergoing a core helium burning phase. In medium mass stars, however, the burning of helium into carbon is no longer the end phase ...
... Stars with a mass of between 8 and 20 solar masses have a more complex evolution. Initially, they evolve in the same way as low mass stars, turning into red giants and undergoing a core helium burning phase. In medium mass stars, however, the burning of helium into carbon is no longer the end phase ...
PART II: Life of a Star
... • Big Bang Nucleosynthesis (eg. 7Li in Halo stars) • The nature of Population III, the First Stars •The First Mass Function, thought to be different at Z=0 (spectrographic observations of metal-poor stars can tell us a lot about the mass distribution of Pop III) • Ancient Supernovae Yields: MP stars ...
... • Big Bang Nucleosynthesis (eg. 7Li in Halo stars) • The nature of Population III, the First Stars •The First Mass Function, thought to be different at Z=0 (spectrographic observations of metal-poor stars can tell us a lot about the mass distribution of Pop III) • Ancient Supernovae Yields: MP stars ...
ppt
... in the space between the atoms … Is God immanent or transcendent, internal or external, composed or compassionate? Like the question of whether the atom is a wave or a particle, the answer is: yes.” ...
... in the space between the atoms … Is God immanent or transcendent, internal or external, composed or compassionate? Like the question of whether the atom is a wave or a particle, the answer is: yes.” ...
Lecture 02a: Setting a context for us in the Universe
... Consequences of the Big Bang theory The Universe… … enlarged and cooled with time … started out as pure H and He. … continues to age… The Big Bang theory accurately explains the relative H and He concentrations in the Universe, its clumpiness, age, background radiation, and other things. ...
... Consequences of the Big Bang theory The Universe… … enlarged and cooled with time … started out as pure H and He. … continues to age… The Big Bang theory accurately explains the relative H and He concentrations in the Universe, its clumpiness, age, background radiation, and other things. ...
Slide 1
... used for H-rich systems: stars, ISM Cosmochemical abundance scale: normalized to Si, the most abundant cation in rock, N(Si) = 106 atoms used for planetary modeling, meteorites Coupling the scales: ...
... used for H-rich systems: stars, ISM Cosmochemical abundance scale: normalized to Si, the most abundant cation in rock, N(Si) = 106 atoms used for planetary modeling, meteorites Coupling the scales: ...
Key Facts
... hydrogen and helium undergoing nuclear fusion at very high temperatures, hence producing vast quantities of energy in the form of heat and light. ...
... hydrogen and helium undergoing nuclear fusion at very high temperatures, hence producing vast quantities of energy in the form of heat and light. ...
EPB_Paper1_EarlyUniverse
... heavier elements. Population I stars are composed of heavier and more diverse elements because they formed later after the big bang, therefore these elements were more abundant in the universe. However, hydrogen and helium are still by far the most abundant gases found in population I stars [9]. The ...
... heavier elements. Population I stars are composed of heavier and more diverse elements because they formed later after the big bang, therefore these elements were more abundant in the universe. However, hydrogen and helium are still by far the most abundant gases found in population I stars [9]. The ...
here
... below, in which a high-‐energy alpha particle collides with a nitrogen nucleus. Use the given table as needed. 18. Complete the nuclear reaction shown here: ...
... below, in which a high-‐energy alpha particle collides with a nitrogen nucleus. Use the given table as needed. 18. Complete the nuclear reaction shown here: ...
How the Universe Works: Supernova Video Guide
... star. The outer layers of the star expand outwards, producing a _______________________. 6. The center of a Red Giant is crushed by ___________________ into a dense ball of oxygen and carbon. This is known as a ___________________________________. 7. Carbon and oxygen are fused together in a white d ...
... star. The outer layers of the star expand outwards, producing a _______________________. 6. The center of a Red Giant is crushed by ___________________ into a dense ball of oxygen and carbon. This is known as a ___________________________________. 7. Carbon and oxygen are fused together in a white d ...
How Old is the Universe?
... For the meteorites, the oldest are 4.56 billion years old. This very well determined age is the age of the Solar System. ...
... For the meteorites, the oldest are 4.56 billion years old. This very well determined age is the age of the Solar System. ...
Chapter 20 Review of Stars` Lifetime Review
... • A black dwarf • Not much compression, just cooling ...
... • A black dwarf • Not much compression, just cooling ...
15-3
... have dissipated (spreads out) • Size of earth, with same mass as our sun • Turns into a black dwarf when fuel runs out • Neutron Stars • Left over from a supernova ...
... have dissipated (spreads out) • Size of earth, with same mass as our sun • Turns into a black dwarf when fuel runs out • Neutron Stars • Left over from a supernova ...
George`s slides
... light elements: 2D, 3He, 4He, 7Li, 8Be • These are generally given as a func5on of the baryon to photon ra5o η = nn/nγ, usually defined in units of 1010, and directly related to the baryon density Ωb: η10 = 1010(nn/nγ) = 274 Ωbh2 • As the universe evolves η is preserved, so that what we obs ...
... light elements: 2D, 3He, 4He, 7Li, 8Be • These are generally given as a func5on of the baryon to photon ra5o η = nn/nγ, usually defined in units of 1010, and directly related to the baryon density Ωb: η10 = 1010(nn/nγ) = 274 Ωbh2 • As the universe evolves η is preserved, so that what we obs ...
Evolution of a Low-Mass Star
... 1) formed at about same time 2) are at about the same distance 3) have same chemical composition The ONLY variable property among stars in a cluster is mass! ...
... 1) formed at about same time 2) are at about the same distance 3) have same chemical composition The ONLY variable property among stars in a cluster is mass! ...
"Cosmic furnaces"()
... together to form a nucleus is overcome by one of the protons turning into a neutron via beta decay, emitting a positron and a neutrino. This complete process requires three of the four forces of Nature acting in coordination against the fourth. The gravitational force first compresses the hydrogen g ...
... together to form a nucleus is overcome by one of the protons turning into a neutron via beta decay, emitting a positron and a neutrino. This complete process requires three of the four forces of Nature acting in coordination against the fourth. The gravitational force first compresses the hydrogen g ...
SPECTRAL ANALYSIS OF A NEWLY DISCOVERED HgMn STAR
... 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star were determined from Geneva photometry and hydrogen line modeling (Te = 12000 ± 200 K, log g = 4.1 ± ü ...
... 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star were determined from Geneva photometry and hydrogen line modeling (Te = 12000 ± 200 K, log g = 4.1 ± ü ...
A Possible Effect of Cosmic Rays on Celestial Chemical Composition
... the Editor The following remarks may be necessary in connection with our problem. (i) The mtensity of general cosmic rays near the sun is about one order smaller than that gtven in (1), so that the general cosmic rays impinging on the solar surface give a contribution to such nuclear transformations ...
... the Editor The following remarks may be necessary in connection with our problem. (i) The mtensity of general cosmic rays near the sun is about one order smaller than that gtven in (1), so that the general cosmic rays impinging on the solar surface give a contribution to such nuclear transformations ...
Where is the antimatter?
... It is supposed that the universe started as pure energy, not matter. The energy from the big bang cooled down as the universe expanded. Some of the energy turned into matter… hydrogen and helium gas. (this happened in the first few seconds of the big bang) ...
... It is supposed that the universe started as pure energy, not matter. The energy from the big bang cooled down as the universe expanded. Some of the energy turned into matter… hydrogen and helium gas. (this happened in the first few seconds of the big bang) ...
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.