25 centuries ago, the ancients came up with theories such as:
... What happens to stars that come in contact with a black hole? a) Expand b) Condense c) Split in half d) Explode e) Sucked in Who invented the first telescope? a) Socrates b) Neil Armstrong c) Galileo d) Leonardo Da Vinci e) George Gamow What is the popular thought among scientists about how the Uni ...
... What happens to stars that come in contact with a black hole? a) Expand b) Condense c) Split in half d) Explode e) Sucked in Who invented the first telescope? a) Socrates b) Neil Armstrong c) Galileo d) Leonardo Da Vinci e) George Gamow What is the popular thought among scientists about how the Uni ...
White dwarf with almost pure oxygen atmosphere
... Image of Sirius A and Sirius B taken by the Hubble Space Telescope. Sirius B, which is a white dwarf, can be seen as a faint pinprick of light to the lower left of the much brighter Sirius A. Image: NASA, ESA ...
... Image of Sirius A and Sirius B taken by the Hubble Space Telescope. Sirius B, which is a white dwarf, can be seen as a faint pinprick of light to the lower left of the much brighter Sirius A. Image: NASA, ESA ...
April 15th
... star that have lost their outer atmospheres of hydrogen in a stellar wind • Lightcurve matches theoretical predictions of ...
... star that have lost their outer atmospheres of hydrogen in a stellar wind • Lightcurve matches theoretical predictions of ...
Space Test Explanations
... to a distant galaxy. Then they measure the velocity at which that galaxy is moving away from us. Finally, they use the formula t=d/v to calculate the age of the universe. 32. Nobody knows how big the universe is. We don’t even know whether or not it goes on forever. Plus, there’s no way that we can ...
... to a distant galaxy. Then they measure the velocity at which that galaxy is moving away from us. Finally, they use the formula t=d/v to calculate the age of the universe. 32. Nobody knows how big the universe is. We don’t even know whether or not it goes on forever. Plus, there’s no way that we can ...
Stellar Evolution II
... sending out a shockwave. This explosive event is called a Type II Supernova!!! • During the Supernova, heavier elements are created, like magnesium, lead, or gold. ...
... sending out a shockwave. This explosive event is called a Type II Supernova!!! • During the Supernova, heavier elements are created, like magnesium, lead, or gold. ...
The Cosmic Perspective Star Stuff
... cool and dim after their initial formation. c) Nuclear fission would be impossible and elements heavier than iron would not exist. d) Stars would continue burning heavier and heavier elements and the universe would have far more lead and uranium. e) Stars would be much less dense, and therefore l ...
... cool and dim after their initial formation. c) Nuclear fission would be impossible and elements heavier than iron would not exist. d) Stars would continue burning heavier and heavier elements and the universe would have far more lead and uranium. e) Stars would be much less dense, and therefore l ...
The s-process in low metallicity stars - GSI
... sigma(A)Ns(A) versus atomic mass number A, but interrupted by steep decreases in correspondence of magic neutron numbers N = 50, 82 or 126, where the neutron capture cross sections are very small and the resulting s-process abundances are large. This happens at the first s-peak at Sr, Y, Zr, at the ...
... sigma(A)Ns(A) versus atomic mass number A, but interrupted by steep decreases in correspondence of magic neutron numbers N = 50, 82 or 126, where the neutron capture cross sections are very small and the resulting s-process abundances are large. This happens at the first s-peak at Sr, Y, Zr, at the ...
Matter and Atoms
... Submicroscopic is so small we cannot see it with a microscope or other tools ...
... Submicroscopic is so small we cannot see it with a microscope or other tools ...
Planck Era
... Most people are familiar with the term 'Big Bang' theory. However when astronomer Sir Fred Hoyle first coined the phrase 'Big Bang' he did so in order to mock the theory. Hoyle was a firm believer in the alternative steady state theory which gives the universe no start or end. However the name stuc ...
... Most people are familiar with the term 'Big Bang' theory. However when astronomer Sir Fred Hoyle first coined the phrase 'Big Bang' he did so in order to mock the theory. Hoyle was a firm believer in the alternative steady state theory which gives the universe no start or end. However the name stuc ...
chapter23 - Empyrean Quest Publishers
... • Ordinary matter ~ 4.4% of total • Total matter is ~ 27% of total – Dark matter is ~ 23% of total – Dark energy is ~ 73% of total • Age of 13.7 billion years In excellent agreement with observations of present-day universe and models involving inflation and WIMPs! ...
... • Ordinary matter ~ 4.4% of total • Total matter is ~ 27% of total – Dark matter is ~ 23% of total – Dark energy is ~ 73% of total • Age of 13.7 billion years In excellent agreement with observations of present-day universe and models involving inflation and WIMPs! ...
Biography of a Star - Max-Planck
... to react with the carbon, resulting in neutrons being released. The neutrons are captured by the iron particles that were present in the star in small quantities from the beginning, resulting in the formation of neutron-rich iron isotopes. If too many neutrons accumulate, radioactive beta decay occu ...
... to react with the carbon, resulting in neutrons being released. The neutrons are captured by the iron particles that were present in the star in small quantities from the beginning, resulting in the formation of neutron-rich iron isotopes. If too many neutrons accumulate, radioactive beta decay occu ...
Gamma-Ray Bursts
... gamma-ray photons, the most energetic form of light, release as much energy in their short duration as our Sun will in its entire lifetime. Two classes of GRBs have been identified, with a dividing line in the gamma-ray emission duration of about 2 seconds.The shorter events are thought to beassocia ...
... gamma-ray photons, the most energetic form of light, release as much energy in their short duration as our Sun will in its entire lifetime. Two classes of GRBs have been identified, with a dividing line in the gamma-ray emission duration of about 2 seconds.The shorter events are thought to beassocia ...
Powerpoint
... oxygen burning (Si, S, Ar, Ca, etc.) into the most tightly bound nuclei (in the iron group) for a given neutron excess, . The silicon-burning nucleosynthesis that is ejected by a supernova is produced explosively, and has a different composition dominated by 56Ni. The products of silicon-core and s ...
... oxygen burning (Si, S, Ar, Ca, etc.) into the most tightly bound nuclei (in the iron group) for a given neutron excess, . The silicon-burning nucleosynthesis that is ejected by a supernova is produced explosively, and has a different composition dominated by 56Ni. The products of silicon-core and s ...
unit notes filled out
... The most massive stars can get hot enough to fuse carbon and other elements. After they go through the giant stage they eventually fuse elements through iron. Iron cannot release energy through fusion reactions, as a result the core becomes unstable and produces a supernova explosion. The final ...
... The most massive stars can get hot enough to fuse carbon and other elements. After they go through the giant stage they eventually fuse elements through iron. Iron cannot release energy through fusion reactions, as a result the core becomes unstable and produces a supernova explosion. The final ...
universe_pp_4 - Cobb Learning
... way out on one of the spiral arms •It’s difficult to see the spiral shape of our galaxy because we’re on the inside ...
... way out on one of the spiral arms •It’s difficult to see the spiral shape of our galaxy because we’re on the inside ...
Nucleosynthesis and Stellar Evolution
... slow; and the element formed by neutron capture will have a chance to beta-decay if it is unstable, before capturing another neutron, if at all. The sequence of elements formed this way are called s-process elements (s for slow). In violent events such as supernova explosions, large flux of neutrons ...
... slow; and the element formed by neutron capture will have a chance to beta-decay if it is unstable, before capturing another neutron, if at all. The sequence of elements formed this way are called s-process elements (s for slow). In violent events such as supernova explosions, large flux of neutrons ...
type II supernova
... astronomers confirmed many of the ideas for how Type II supernovae occur. They even had pictures of the star before it exploded. It was a blue supergiant star with a mass of around 20 and a luminosity of around . They found evidence of radioactive Co in the SN's spectrum. (This isotope of cobalt is ...
... astronomers confirmed many of the ideas for how Type II supernovae occur. They even had pictures of the star before it exploded. It was a blue supergiant star with a mass of around 20 and a luminosity of around . They found evidence of radioactive Co in the SN's spectrum. (This isotope of cobalt is ...
File - Prairie Science
... Some massive stars produce leftovers too massive to become stable neutron stars. If the remaining core contains more mass than 3 times our sun, the star may contract further under gravity. The force of contraction crushes dense core of the star and leaves behind a black hole. The gravity of a black ...
... Some massive stars produce leftovers too massive to become stable neutron stars. If the remaining core contains more mass than 3 times our sun, the star may contract further under gravity. The force of contraction crushes dense core of the star and leaves behind a black hole. The gravity of a black ...
2nd Japanese-German Workshop on Nuclear Structure and
... G. Martinez-Pinedo (25+5) r-Process and nuclear structure changed to Prof. Langanke W. Aoki (25+5) Observational studies of heavy elements in metal-deficient stars H. Sakurai (25+5) RIBF ...
... G. Martinez-Pinedo (25+5) r-Process and nuclear structure changed to Prof. Langanke W. Aoki (25+5) Observational studies of heavy elements in metal-deficient stars H. Sakurai (25+5) RIBF ...
Exam #3 study guide
... Notes for Exam #3 The third exam on October 31st will cover all material through the syllabus week 9. The exam will focus primarily on material from weeks 7, 8 and 9, which include: 1. Nuclear physics (isotopes, radioactivity) 2. Stars and galaxies (H-R diagrams; big bang) 3. The Earth and other pla ...
... Notes for Exam #3 The third exam on October 31st will cover all material through the syllabus week 9. The exam will focus primarily on material from weeks 7, 8 and 9, which include: 1. Nuclear physics (isotopes, radioactivity) 2. Stars and galaxies (H-R diagrams; big bang) 3. The Earth and other pla ...
Star and Earth Chemistry Lecture Notes (PDF
... J. Silk, The Big Bang, Freeman, 2e (1989) S. Weidberg, The First Three Minutes, Fontana, (1986) There are many introductory textbook on astronomy in the Morrell Library. All cover much the same material in a similar order and there is little to choose between any of them! They are shelved in the Qua ...
... J. Silk, The Big Bang, Freeman, 2e (1989) S. Weidberg, The First Three Minutes, Fontana, (1986) There are many introductory textbook on astronomy in the Morrell Library. All cover much the same material in a similar order and there is little to choose between any of them! They are shelved in the Qua ...
ASTR 31: Descriptive Astronomy
... beryllium-8 (4 protons + 4 neutrons): 8Be carbon-12 (6 protons + 6 neutrons): 12C oxygen-16 (8 protons + 8 neutrons): 16O neon-20 (10 protons + 10 neutrons): 20Ne magnesium-24 (12 protons + 12 neutrons): 24Mg silicon-28 (14 protons + 14 neutrons): 28Si sulfer-32 (16 protons + 16 neutrons): 32S argon ...
... beryllium-8 (4 protons + 4 neutrons): 8Be carbon-12 (6 protons + 6 neutrons): 12C oxygen-16 (8 protons + 8 neutrons): 16O neon-20 (10 protons + 10 neutrons): 20Ne magnesium-24 (12 protons + 12 neutrons): 24Mg silicon-28 (14 protons + 14 neutrons): 28Si sulfer-32 (16 protons + 16 neutrons): 32S argon ...
The death of a star
... This rate of expansion continues and the star expands to produce a Red Giant the size of the Earth's orbit. This expansion is so rapid that the outer layers will cool, their temperature falling from the 6000o of its main lifetime to some 3000o in the Red Giant phase. The core is still hot and contin ...
... This rate of expansion continues and the star expands to produce a Red Giant the size of the Earth's orbit. This expansion is so rapid that the outer layers will cool, their temperature falling from the 6000o of its main lifetime to some 3000o in the Red Giant phase. The core is still hot and contin ...
Lecture 1
... Protostars: energy from gravity Main Sequence: energy from fusion converting H to He in their cores Red giants: energy from gravity Horizontal branch: fusion of He to C AGB: energy from gravity Planetary nebula: energy from gravity and spasmodic shell He fusion (and shell H fusion). ...
... Protostars: energy from gravity Main Sequence: energy from fusion converting H to He in their cores Red giants: energy from gravity Horizontal branch: fusion of He to C AGB: energy from gravity Planetary nebula: energy from gravity and spasmodic shell He fusion (and shell H fusion). ...
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.