Nuclear Exotica (online version) - ECM-UB
... production of exotic nuclei with very different N, Z numbers from the known isotopes achieved with RIB facilities experiments start unveiling the properties of short lived, weakly bound nuclei far from stability extend our knowledge of nuclear structure Major next generation facilities planned o ...
... production of exotic nuclei with very different N, Z numbers from the known isotopes achieved with RIB facilities experiments start unveiling the properties of short lived, weakly bound nuclei far from stability extend our knowledge of nuclear structure Major next generation facilities planned o ...
Lecture 16: Iron Core Collapse, Neutron Stars
... As the expanding helium core runs into the massive, but low density hydrogen envelope, the shock at its boundary decelerates. The deceleration is in opposition to the radially decreasing density gradient of the supernova. ...
... As the expanding helium core runs into the massive, but low density hydrogen envelope, the shock at its boundary decelerates. The deceleration is in opposition to the radially decreasing density gradient of the supernova. ...
26.Meikle.Supernova_2002hh
... powerful coolant and may lead to the formation of dust grains in the ejecta. Supernovae are suspected to be a major source of dust in the universe and the presence of new dust in SN 2002hh is expected to be observed at a later stage. This is only the second time for which a spectrum has been obtaine ...
... powerful coolant and may lead to the formation of dust grains in the ejecta. Supernovae are suspected to be a major source of dust in the universe and the presence of new dust in SN 2002hh is expected to be observed at a later stage. This is only the second time for which a spectrum has been obtaine ...
The Life Cycle of a Star
... Lowmass stars (red dwarfs) consume hydrogen at a very slow rate (~ 100 billion years). During this time, they lose significant mass, and eventually evaporate. The result is a very faint white dwarf. ...
... Lowmass stars (red dwarfs) consume hydrogen at a very slow rate (~ 100 billion years). During this time, they lose significant mass, and eventually evaporate. The result is a very faint white dwarf. ...
1.1 Safety in the Science Classroom
... analyze to discover the direction and amount the light has shifted. » A red shift means the wavelength is getting longer, and the star is moving away from us. » Blue shift is the opposite; the star is getting closer. ...
... analyze to discover the direction and amount the light has shifted. » A red shift means the wavelength is getting longer, and the star is moving away from us. » Blue shift is the opposite; the star is getting closer. ...
GoldCreation
... One of my favorite astronomy-themed t-shirts says “You are star dust”. It makes the point that we are all made from long dead stars. Of course, everything around us is also made of star stuff. This even includes rare elements such as gold. This paper discusses the processes of gold formation. Most m ...
... One of my favorite astronomy-themed t-shirts says “You are star dust”. It makes the point that we are all made from long dead stars. Of course, everything around us is also made of star stuff. This even includes rare elements such as gold. This paper discusses the processes of gold formation. Most m ...
Nitrogen abundances in solar
... Work focus: non-LTE line formation, quantitative analysis Solar-type stars are valuable tracers of the chemical evolution of the Milky Way over cosmic history because of their longevity. They are numerous, accessible at high spectral resolution out to distances of several kpc with large telescopes, ...
... Work focus: non-LTE line formation, quantitative analysis Solar-type stars are valuable tracers of the chemical evolution of the Milky Way over cosmic history because of their longevity. They are numerous, accessible at high spectral resolution out to distances of several kpc with large telescopes, ...
Stars
... What powers a star? A star is ‘powered’ by nuclear fusion reactions in its core. Nuclear fusion involves light atomic nuclei joining together to form heavier ones. Each fusion reaction produces a small amount of energy, but there are billions of reactions per second. Each second, the Sun produces 4 ...
... What powers a star? A star is ‘powered’ by nuclear fusion reactions in its core. Nuclear fusion involves light atomic nuclei joining together to form heavier ones. Each fusion reaction produces a small amount of energy, but there are billions of reactions per second. Each second, the Sun produces 4 ...
NAME___________ _PERIOD____DATE_____________ 29.3
... during the formation of a star. What is the correct label for the blank in the diagram? ...
... during the formation of a star. What is the correct label for the blank in the diagram? ...
Stellar Evolution Diagram Answer Key:
... Once a neutron star forms- it should have a very long life (100’s of billions of years). It is a core of a supernova after an explosion which causes it to contract into a very small but incredibly dense ball of neutrons. A spoonful of matter from a neutron star would weight 100 million tons on earth ...
... Once a neutron star forms- it should have a very long life (100’s of billions of years). It is a core of a supernova after an explosion which causes it to contract into a very small but incredibly dense ball of neutrons. A spoonful of matter from a neutron star would weight 100 million tons on earth ...
Document
... a. The latter has a diameter of almost two billion miles. b. If you counted one star a second it would take you more than thirty thousand years to count 100 billion. c. But, during your lifetime, as always, new stars are being crated. d. The solar system is located in the Milky Way Galaxy. e. Stars ...
... a. The latter has a diameter of almost two billion miles. b. If you counted one star a second it would take you more than thirty thousand years to count 100 billion. c. But, during your lifetime, as always, new stars are being crated. d. The solar system is located in the Milky Way Galaxy. e. Stars ...
Children of the stars, children of the Universe…
... The Universe was dominated by radiation over the first million years. Free electrons from ionization by gamma rays made matter opaque for photons After 1 million years, the Universe became cool enough for neutral atoms to form. The gas became transparent for radiation in this recombination phase At ...
... The Universe was dominated by radiation over the first million years. Free electrons from ionization by gamma rays made matter opaque for photons After 1 million years, the Universe became cool enough for neutral atoms to form. The gas became transparent for radiation in this recombination phase At ...
Chapter 14
... Formation of Elements beyond Iron occurs very rapidly as the star approaches supernova. ...
... Formation of Elements beyond Iron occurs very rapidly as the star approaches supernova. ...
Powerpoint of lecture 16
... in high-energy states may be captured by Ne or Mg nuclei • Pressure drops, core cannot support itself, collapses catastrophically (timescale: 10s of milliseconds!) to nuclear densities, and bounces, leading to outward-travelling shock wave • Shock also accelerated by pressure of neutrinos, produced ...
... in high-energy states may be captured by Ne or Mg nuclei • Pressure drops, core cannot support itself, collapses catastrophically (timescale: 10s of milliseconds!) to nuclear densities, and bounces, leading to outward-travelling shock wave • Shock also accelerated by pressure of neutrinos, produced ...
Star Cycle Notes
... squeezed so tightly they begin to fuse and form larger atoms like carbon and oxygen. Nuclear fusion restarts, but much more powerfully this time. The restart of nuclear fusion in the star’s core expands the star much larger than it’s original size. The star becomes a red giant (or supergiant). Fusio ...
... squeezed so tightly they begin to fuse and form larger atoms like carbon and oxygen. Nuclear fusion restarts, but much more powerfully this time. The restart of nuclear fusion in the star’s core expands the star much larger than it’s original size. The star becomes a red giant (or supergiant). Fusio ...
Supernovae - Michigan State University
... Displayed is the overproduction factor X/Xsolar This is the fraction of matter in the Galaxy that had to be processed through the scenario (massive stars here) to account for todays observed solar abundances. To explain the origin of the elements one needs to have • constant overproduction (then the ...
... Displayed is the overproduction factor X/Xsolar This is the fraction of matter in the Galaxy that had to be processed through the scenario (massive stars here) to account for todays observed solar abundances. To explain the origin of the elements one needs to have • constant overproduction (then the ...
Universe, Galaxies, and Stars – The Basics
... When light gets divided up into its wavelengths you call it a spectrum. Think about the colors of the rainbow. Maybe you have heard the acronym “ROY G BIV” to help you remember them. The colors are: Red Orange Yellow Green Blue Indigo Violet (ROY G BIV). In order to understand starlight we also need ...
... When light gets divided up into its wavelengths you call it a spectrum. Think about the colors of the rainbow. Maybe you have heard the acronym “ROY G BIV” to help you remember them. The colors are: Red Orange Yellow Green Blue Indigo Violet (ROY G BIV). In order to understand starlight we also need ...
Notes - Michigan State University
... Displayed is the overproduction factor X/Xsolar This is the fraction of matter in the Galaxy that had to be processed through the scenario (massive stars here) to account for todays observed solar abundances. To explain the origin of the elements one needs to have • constant overproduction (then the ...
... Displayed is the overproduction factor X/Xsolar This is the fraction of matter in the Galaxy that had to be processed through the scenario (massive stars here) to account for todays observed solar abundances. To explain the origin of the elements one needs to have • constant overproduction (then the ...
The Cosmic Cupboard
... Ice as well as Rock. There is a 100 times the amount of Ice compared to Rock. So the planets that form beyond the Ice Line start with much larger planetary cores of Ice and Rock. These large cores have enough gravity to accrete to cold hydrogen and helium around them. Thus they grow to be gas giant ...
... Ice as well as Rock. There is a 100 times the amount of Ice compared to Rock. So the planets that form beyond the Ice Line start with much larger planetary cores of Ice and Rock. These large cores have enough gravity to accrete to cold hydrogen and helium around them. Thus they grow to be gas giant ...
Stan Woosley (UCSC)
... Inside the shock, matter is in approximate hydrostatic equilibrium. Inside the gain radius there is net energy loss to neutrinos. Outside there is net energy gain from neutrino deposition. At any one time there is about 0.1 solar masses in the gain region absorbing a few percent of the neutrino lumi ...
... Inside the shock, matter is in approximate hydrostatic equilibrium. Inside the gain radius there is net energy loss to neutrinos. Outside there is net energy gain from neutrino deposition. At any one time there is about 0.1 solar masses in the gain region absorbing a few percent of the neutrino lumi ...
Big Bang and Synthesis of Elements
... states of matter. These leptons, which include electrons, neutrinos and photons, would soon be able to join their hadron kin in a union that would define present-day common matter. After about one to three minutes had passed since the creation of the universe, protons and neutrons began to react wit ...
... states of matter. These leptons, which include electrons, neutrinos and photons, would soon be able to join their hadron kin in a union that would define present-day common matter. After about one to three minutes had passed since the creation of the universe, protons and neutrons began to react wit ...
protostars low mass stars intermediatemass stars red giant planetary
... main sequence as it runs out of hydrogen, the shell of gases around the star begin to expand and cool, causing a reddish glow.This is where the term red giant comes from. These stars are very bright because of their larger surface area. The core becomes very compressed (not much larger than ...
... main sequence as it runs out of hydrogen, the shell of gases around the star begin to expand and cool, causing a reddish glow.This is where the term red giant comes from. These stars are very bright because of their larger surface area. The core becomes very compressed (not much larger than ...
We Are Stardust: Synthesis of the Elements Essential for Life Aparna
... • The nucleosynthesis that occurred in the first three minutes after the Big Bang made only hydrogen, helium, and trace amounts of deuterium and lithium. • Thus, all the other elements that we observe on Earth and in the universe were made subsequently. • We believe, from theoretical models and from ...
... • The nucleosynthesis that occurred in the first three minutes after the Big Bang made only hydrogen, helium, and trace amounts of deuterium and lithium. • Thus, all the other elements that we observe on Earth and in the universe were made subsequently. • We believe, from theoretical models and from ...
History of the universe timeline
... Nuclei of hydrogen, helium, lithium and other light elements form. ...
... Nuclei of hydrogen, helium, lithium and other light elements form. ...
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.