Standard 1-1.A “The Big Bang Theory” Study Notes
... 4. Scientists accept the Big Bang theory because evidence supports it. 5. The big bang started when all matter in the universe burst from a tiny point. 6. A star moving away from Earth has a spectrum that is shifted toward red. 7. Hubble’s discovery that there was red shift in the spectra of galaxie ...
... 4. Scientists accept the Big Bang theory because evidence supports it. 5. The big bang started when all matter in the universe burst from a tiny point. 6. A star moving away from Earth has a spectrum that is shifted toward red. 7. Hubble’s discovery that there was red shift in the spectra of galaxie ...
![Star Cycle [Recovered]](http://s1.studyres.com/store/data/008086481_1-2d8d14aa9163345f6c20c4baab23c80a-300x300.png)
Star Cycle [Recovered]
... SUPERNOVA explosion A ___________________ is an _________________ that marks the end of a very massive star’s life. When it occurs, the exploding star can outshine all of the other stars in the galaxy in total for several days and may leave behind only a crushed core. ...
... SUPERNOVA explosion A ___________________ is an _________________ that marks the end of a very massive star’s life. When it occurs, the exploding star can outshine all of the other stars in the galaxy in total for several days and may leave behind only a crushed core. ...
21_LectureOutline
... • A nova is a star that suddenly brightens and gradually fades; it is a white dwarf whose larger partner continually transfers material to it. ...
... • A nova is a star that suddenly brightens and gradually fades; it is a white dwarf whose larger partner continually transfers material to it. ...
Stellar Evolution - FSU High Energy Physics
... • Thermal motion of the ions will become less important and eventually degenerate electron pressure opposes gravitational collapse. ...
... • Thermal motion of the ions will become less important and eventually degenerate electron pressure opposes gravitational collapse. ...
оценка и стандартизация радионуклидных данных
... Half-lives of long-lived radionuclides more than 108 years such as of 176Lu, 187Re, 232Th, 235U, and 238U are used in nuclear astrophysics for dating different cosmic events and also half-lives of 40K and 87Rb are used in nuclear geochronology for determination of the ages of minerals. Moreover, rec ...
... Half-lives of long-lived radionuclides more than 108 years such as of 176Lu, 187Re, 232Th, 235U, and 238U are used in nuclear astrophysics for dating different cosmic events and also half-lives of 40K and 87Rb are used in nuclear geochronology for determination of the ages of minerals. Moreover, rec ...
a Supernova!
... subjected to a bombardment by large numbers of newlycreated neutrons. Since these neutrons are uncharged, they have no trouble penetrating a heavy nucleus: there is no repulsion! What happens if we bombard a heavy nucleus (say, Iron) with ...
... subjected to a bombardment by large numbers of newlycreated neutrons. Since these neutrons are uncharged, they have no trouble penetrating a heavy nucleus: there is no repulsion! What happens if we bombard a heavy nucleus (say, Iron) with ...
Abundance of Elements
... C) a-elements : C, N, O, Ne, Mg, & Si ; tightly bound, thermodynamically-favored ...
... C) a-elements : C, N, O, Ne, Mg, & Si ; tightly bound, thermodynamically-favored ...
Charterhouse2-gelletly-elements
... turning 4 protons into an alpha releases about 26 MeV of energy. It is this energy which heats the stellar interior,allows it to withstand the gravitational pressure and causes it to shine! ...
... turning 4 protons into an alpha releases about 26 MeV of energy. It is this energy which heats the stellar interior,allows it to withstand the gravitational pressure and causes it to shine! ...
gelletly-Charterhouse2-elements
... turning 4 protons into an alpha releases about 26 MeV of energy. It is this energy which heats the stellar interior,allows it to withstand the gravitational pressure and causes it to shine! ...
... turning 4 protons into an alpha releases about 26 MeV of energy. It is this energy which heats the stellar interior,allows it to withstand the gravitational pressure and causes it to shine! ...
The Birth, Life, and Death of Stars
... BBN does not generate any heavy elements! He-ashes fuse in the hot (T ≈ 108 K) and dense (n ≈ 1028 cm−3 ) core Physics demands a tiny concentration of 8 Be (n8 /n4 ≈ 10−8 ) Carbon is formed: α + α → 8 Be + α → 12 C + γ (7.367 MeV) Every atom in our body has been formed in stellar cores! ...
... BBN does not generate any heavy elements! He-ashes fuse in the hot (T ≈ 108 K) and dense (n ≈ 1028 cm−3 ) core Physics demands a tiny concentration of 8 Be (n8 /n4 ≈ 10−8 ) Carbon is formed: α + α → 8 Be + α → 12 C + γ (7.367 MeV) Every atom in our body has been formed in stellar cores! ...
Cosmological Aspects of Nucleosynthesis
... took place at about 1.2x109 K. At larger temperature, D would be destroyed by radiation background ...
... took place at about 1.2x109 K. At larger temperature, D would be destroyed by radiation background ...
Phys 214. Planets and Life
... showing the X-ray (blue), and optical (red) images superimposed. NASA/ESA. ...
... showing the X-ray (blue), and optical (red) images superimposed. NASA/ESA. ...
Elements from Stardust
... they can join together in a process called nuclear fusion. • In nuclear fusion, atomic nuclei combine to form a larger nucleus, releasing huge amounts of energy in the process. • Inside stars, nuclear fusion combines smaller nuclei into larger nuclei, thus creating heavier elements. ...
... they can join together in a process called nuclear fusion. • In nuclear fusion, atomic nuclei combine to form a larger nucleus, releasing huge amounts of energy in the process. • Inside stars, nuclear fusion combines smaller nuclei into larger nuclei, thus creating heavier elements. ...
Gold could have come from colliding stars - Horizon Magazine
... The question, according to Dr Bauswein, is whether this picture can be confirmed by observations. Fortunately, the simulations predict that every merger should generate a characteristic ‘gravitational wave’ – a ripple in the very fabric of space–time. The observation of the right kind of gravitation ...
... The question, according to Dr Bauswein, is whether this picture can be confirmed by observations. Fortunately, the simulations predict that every merger should generate a characteristic ‘gravitational wave’ – a ripple in the very fabric of space–time. The observation of the right kind of gravitation ...
minnesota
... The figures at the right show the first results of nucleosynthesis calculations in realistic (albeit 1D) models for two supernovae modelled from the main sequence through explosion carrying a network of 2000 isotopes in each of 1000 zones. A (very sparse) matrix of 2000 x 2000 was inverted approxima ...
... The figures at the right show the first results of nucleosynthesis calculations in realistic (albeit 1D) models for two supernovae modelled from the main sequence through explosion carrying a network of 2000 isotopes in each of 1000 zones. A (very sparse) matrix of 2000 x 2000 was inverted approxima ...
metallic elements
... 2) Heavier elements all very rare (∑ ~ 0.1 atom %); essentially trace elements ! 3) Progressive, exponential-like decline with atomic number Z 4) Abundance minimum at Li, Be, B 5) Abundance peaks at C, O, Fe. High for nuclides with Mass # A of multiples of 4 = a particle mass Bulk Earth > 92 wt % ...
... 2) Heavier elements all very rare (∑ ~ 0.1 atom %); essentially trace elements ! 3) Progressive, exponential-like decline with atomic number Z 4) Abundance minimum at Li, Be, B 5) Abundance peaks at C, O, Fe. High for nuclides with Mass # A of multiples of 4 = a particle mass Bulk Earth > 92 wt % ...
presentation02 - School of Physical Sciences
... The universe has been expanding ever since. Evidence for this: •Observation of galaxies flying away from us in all directions. •Remnant of the Big Bang known as the Cosmic Microwave Background Radiation. •Observed abundance of light elements made in the Big Bang matches predictions. ...
... The universe has been expanding ever since. Evidence for this: •Observation of galaxies flying away from us in all directions. •Remnant of the Big Bang known as the Cosmic Microwave Background Radiation. •Observed abundance of light elements made in the Big Bang matches predictions. ...
Nuclear Astrophysics (a Cosmic Cookbook)
... The laws of physics allow the existence of stars via the transformation of lighter elements to heavier ones All we need is hydrogen, and a little helium then gravity and the other forces of nature take care of the rest ...
... The laws of physics allow the existence of stars via the transformation of lighter elements to heavier ones All we need is hydrogen, and a little helium then gravity and the other forces of nature take care of the rest ...
Stellar Nucleosynthesis
... • See next 10 years of accelerator and reactor based neutrino experiments ...
... • See next 10 years of accelerator and reactor based neutrino experiments ...
Opportunities for low energy nuclear physics with rare isotope
... RIB : nucleosynthesis of heavy elements by r-, gammaand rp-processes ...
... RIB : nucleosynthesis of heavy elements by r-, gammaand rp-processes ...
Name: Period: ______ Date: Fission and Fusion Simulations Fission
... See how Fusion in the Sun works. http://www.universetoday.com/18707/fusion-in-the-sun/ 23. What’s the pressure and temperature like inside the Sun? ...
... See how Fusion in the Sun works. http://www.universetoday.com/18707/fusion-in-the-sun/ 23. What’s the pressure and temperature like inside the Sun? ...
Folie 1
... – Helium converted into heavier elements (carbon, oxygen, …, iron) – The star has an onion-like structure ...
... – Helium converted into heavier elements (carbon, oxygen, …, iron) – The star has an onion-like structure ...
Week one: Space Physics and Aeronomy (pdf, 1.3 MB)
... pulling in more mass and creating a denser core. Temperatures soared to 10 million degrees. At these temps, hydrogen nuclei fused to create helium. With the start of nuclear fusion, the protostar “ignited.” ...
... pulling in more mass and creating a denser core. Temperatures soared to 10 million degrees. At these temps, hydrogen nuclei fused to create helium. With the start of nuclear fusion, the protostar “ignited.” ...
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.